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Author name code: noyes
ADS astronomy entries on 2022-09-14
author:"Noyes, Robert W."
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Title: VizieR Online Data Catalog: Light curve and radial velocities
for 7 host stars (Bakos+, 2021)
Authors: Bakos, G. A.; Hartman, J. D.; Bhatti, W.; Csubry, Z.;
Penev, K.; Bieryla, A.; Latham, D. W.; Quinn, S.; Buchhave, L. A.;
Kovacs, G.; Torres, G.; Noyes, R. W.; Falco, E.; Beky, B.; Szklenar,
T.; Esquerdo, G. A.; Howard, A. W.; Isaacson, H.; Marcy, G.; Sato,
B.; Boisse, I.; Santerne, A.; Hebrard, G.; Rabus, M.; Harbeck, D.;
McCully, C.; Everett, M. E.; Horch, E. P.; Hirsch, L.; Howell, S. B.;
Huang, C. X.; Lazar, J.; Papp, I.; Sari, P.
2021yCat..51620007B Altcode:
We presented the discovery of seven hot Jupiters transiting bright
stars. These planets were first identified as transiting planet
candidates by the HATNet survey from among some six million stars that
have been observed to date since 2004. They were subsequently confirmed
and accurately characterized using high-precision time-series photometry
from Fred Lawrence Whipple Observatory (FLWO) 1.2 m/KeplerCam, and
the NASA Transiting Exoplents Survey Satellite (TESS) mission, and
high-resolution spectroscopy, enabling high-precision RVel measurements,
carried out with the FLWO 1.5m/TRES (Tillinghast Reflector Echelle
Spectrograph), Keck-I/HIRES (High Resolution Echelle Spectrometer),
Observatoire de Haute Provence (OHP) 1.93m/SOPHIE, Subaru 8m/HDS, Apache
Point Observatory (APO) 3.5m/ARCES, Nordic Optical Telescope (NOT)
2.5m/FIES (fiber-fed echelle Spectrograph), and Las Cumbres Observatory
Grand Telescope (LCOGT) 1m/NRES telescopes/instruments. Filters, dates
and resolutions can be found in table 1, 2 and 3. <P />(2 data files).
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Title: HAT-P-58b-HAT-P-64b: Seven Planets Transiting Bright Stars
Authors: Bakos, G. Á.; Hartman, J. D.; Bhatti, W.; Csubry, Z.;
Penev, K.; Bieryla, A.; Latham, D. W.; Quinn, S.; Buchhave, L. A.;
Kovács, G.; Torres, Guillermo; Noyes, R. W.; Falco, E.; Béky,
Bence; Szklenár, T.; Esquerdo, G. A.; Howard, A. W.; Isaacson, H.;
Marcy, G.; Sato, B.; Boisse, I.; Santerne, A.; Hébrard, G.; Rabus,
M.; Harbeck, D.; McCully, C.; Everett, M. E.; Horch, E. P.; Hirsch,
L.; Howell, S. B.; Huang, C. X.; Lázár, J.; Papp, I.; Sári, P.
2021AJ....162....7B Altcode: 2020arXiv200705528B
We report the discovery and characterization of seven transiting
exoplanets from the HATNet survey. The planets, which are hot
Jupiters and Saturns transiting bright Sun-like stars, include:
HAT-P-58b (with mass M<SUB>p</SUB> = 0.37 M<SUB>J</SUB>, radius
R<SUB>p</SUB> = 1.33 R<SUB>J</SUB>, and orbital period P = 4.0138
days), HAT-P-59b (M<SUB>p</SUB> = 1.54 M<SUB>J</SUB>, R<SUB>p</SUB>
= 1.12 R<SUB>J</SUB>, P = 4.1420 days), HAT-P-60b (M<SUB>p</SUB> =
0.57 M<SUB>J</SUB>, R<SUB>p</SUB> = 1.63 R<SUB>J</SUB>, P = 4.7948
days), HAT-P-61b (M<SUB>p</SUB> = 1.06 M<SUB>J</SUB>, R<SUB>p</SUB>
= 0.90 R<SUB>J</SUB>, P = 1.9023 days), HAT-P-62b (M<SUB>p</SUB> =
0.76 M<SUB>J</SUB>, R<SUB>p</SUB> = 1.07 R<SUB>J</SUB>, P = 2.6453
days), HAT-P-63b (M<SUB>p</SUB> = 0.61 M<SUB>J</SUB>, R<SUB>p</SUB>
= 1.12 R<SUB>J</SUB>, P = 3.3777 days), and HAT-P-64b (M<SUB>p</SUB>
= 0.58 M<SUB>J</SUB>, R<SUB>p</SUB> = 1.70 R<SUB>J</SUB>, P = 4.0072
days). The typical errors on these quantities are 0.06 M<SUB>J</SUB>,
0.03 R<SUB>J</SUB>, and 0.2 s, respectively. We also provide accurate
stellar parameters for each of the host stars. With V = 9.710 ±
0.050 mag, HAT-P-60 is an especially bright transiting planet host,
and an excellent target for additional follow-up observations. With
R<SUB>p</SUB> = 1.703 ± 0.070 R<SUB>J</SUB>, HAT-P-64b is a highly
inflated hot Jupiter around a star nearing the end of its main-sequence
lifetime, and is among the largest known planets. Five of the seven
systems have long-cadence observations by TESS which are included
in the analysis. Of particular note is HAT-P-59 (TOI-1826.01) which
is within the northern continuous viewing zone of the TESS mission,
and HAT-P-60, which is the TESS candidate TOI-1580.01. <SUP>*</SUP>
Based on observations of the Hungarian-made Automated Telescope Network
and observations obtained at the following observatories: W. M. Keck
Observatory, the 1.5 m and the 1.2 m telescopes at the Fred Lawrence
Whipple Observatory of the Smithsonian Astrophysical Observatory, the
Kitt Peak National Observatory, the 1.93 m telescope at Observatoire
de Haute-Provence, the Subaru Telescope of the National Astronomical
Observatory of Japan, the Nordic Optical Telescope in the Spanish
Observatorio del Roque de los Muchachos of the Intituto de Astrofísica
de Canarias, and the Apache Point Observatory 3.5 m telescope.
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Title: Two New HATNet Hot Jupiters around A Stars and the First
Glimpse at the Occurrence Rate of Hot Jupiters from TESS
Authors: Zhou, G.; Huang, C. X.; Bakos, G. Á.; Hartman, J. D.;
Latham, David W.; Quinn, S. N.; Collins, K. A.; Winn, J. N.; Wong, I.;
Kovács, G.; Csubry, Z.; Bhatti, W.; Penev, K.; Bieryla, A.; Esquerdo,
G. A.; Berlind, P.; Calkins, M. L.; de Val-Borro, M.; Noyes, R. W.;
Lázár, J.; Papp, I.; Sári, P.; Kovács, T.; Buchhave, Lars A.;
Szklenar, T.; Béky, B.; Johnson, M. C.; Cochran, W. D.; Kniazev,
A. Y.; Stassun, K. G.; Fulton, B. J.; Shporer, A.; Espinoza, N.;
Bayliss, D.; Everett, M.; Howell, S. B.; Hellier, C.; Anderson,
D. R.; Collier Cameron, A.; West, R. G.; Brown, D. J. A.; Schanche,
N.; Barkaoui, K.; Pozuelos, F.; Gillon, M.; Jehin, E.; Benkhaldoun,
Z.; Daassou, A.; Ricker, G.; Vanderspek, R.; Seager, S.; Jenkins,
J. M.; Lissauer, Jack J.; Armstrong, J. D.; Collins, K. I.; Gan, T.;
Hart, R.; Horne, K.; Kielkopf, J. F.; Nielsen, L. D.; Nishiumi, T.;
Narita, N.; Palle, E.; Relles, H. M.; Sefako, R.; Tan, T. G.; Davies,
M.; Goeke, Robert F.; Guerrero, N.; Haworth, K.; Villanueva, S.
2019AJ....158..141Z Altcode: 2019arXiv190600462Z
Wide-field surveys for transiting planets are well suited to searching
diverse stellar populations, enabling a better understanding of the link
between the properties of planets and their parent stars. We report
the discovery of HAT-P-69 b (TOI 625.01) and HAT-P-70 b (TOI 624.01),
two new hot Jupiters around A stars from the Hungarian-made Automated
Telescope Network (HATNet) survey that have also been observed by
the Transiting Exoplanet Survey Satellite. HAT-P-69 b has a mass
of {3.58}<SUB>-0.58</SUB><SUP>+0.58</SUP> M <SUB>Jup</SUB> and a
radius of {1.676}<SUB>-0.033</SUB><SUP>+0.051</SUP> R <SUB>Jup</SUB>
and resides in a prograde 4.79 day orbit. HAT-P-70 b has a radius of
{1.87}<SUB>-0.10</SUB><SUP>+0.15</SUP> R <SUB>Jup</SUB> and a mass
constraint of < 6.78 (3σ ) M <SUB>Jup</SUB> and resides in a
retrograde 2.74 day orbit. We use the confirmation of these planets
around relatively massive stars as an opportunity to explore the
occurrence rate of hot Jupiters as a function of stellar mass. We define
a sample of 47,126 main-sequence stars brighter than T <SUB>mag</SUB>
= 10 that yields 31 giant planet candidates, including 18 confirmed
planets, 3 candidates, and 10 false positives. We find a net hot Jupiter
occurrence rate of 0.41 ± 0.10% within this sample, consistent with
the rate measured by Kepler for FGK stars. When divided into stellar
mass bins, we find the occurrence rate to be 0.71 ± 0.31% for G stars,
0.43 ± 0.15% for F stars, and 0.26 ± 0.11% for A stars. Thus, at this
point, we cannot discern any statistically significant trend in the
occurrence of hot Jupiters with stellar mass. <P />Based on observations
obtained with the Hungarian-made Automated Telescope Network. Based
in part on observations obtained with the Tillinghast Reflector 1.5 m
telescope and the 1.2 m telescope, both operated by the Smithsonian
Astrophysical Observatory at the Fred Lawrence Whipple Observatory
in Arizona. This work makes use of the Smithsonian Institution High
Performance Cluster (SI/HPC). Based in part on observations made with
the Southern African Large Telescope (SALT).
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Title: VizieR Online Data Catalog: Differential photometry &
RVs of HAT-P-69 & HAT-P-70 (Zhou+, 2019)
Authors: Zhou, G.; Huang, C. X.; Bakos, G. A.; Hartman, J. D.; Latham,
D. W.; Quinn, S. N.; Collins, K. A.; Winn, J. N.; Wong, I.; Kovacs,
G.; Csubry, Z.; Bhatti, W.; Penev, K.; Bieryla, A.; Esquerdo, G. A.;
Berlind, P.; Calkins, M. L.; de Val-Borro, M.; Noyes, R. W.; Lazar,
J.; Papp, I.; Sari, P.; Kovacs, T.; Buchhave, L. A.; Szklenar, T.;
Beky, B.; Johnson, M. C.; Cochran, W. D.; Kniazev, A. Y.; Stassun,
K. G.; Fulton, B. J.; Shporer, A.; Espinoza, N.; Bayliss, D.;
Everett, M.; Howell, S. B.; Hellier, C.; Anderson, D. R.; Cameron,
A. C.; West, R. G.; Brown, D. J. A.; Schanche, N.; Barkaoui, K.;
Pozuelos, F.; Gillon, M.; Jehin, E.; Benkhaldoun, Z.; Daassou, A.;
Ricker, G.; Vanderspek, R.; Seager, S.; Jenkins, J. M.; Lissauer,
J. J.; Armstrong, J. D.; Collins, K. I.; Gan, T.; Hart, R.; Horne,
K.; Kielkopf, J. F.; Nielsen, L. D.; Nishiumi, T.; Narita, N.; Palle,
E.; Relles, H. M.; Sefako, R.; Tan, T. G.; Davies, M.; Goeke, R. F.;
Guerrero, N.; Haworth, K.; Villanueva, S.
2019yCat..51580141Z Altcode:
The HATNet survey (Bakos et al. 2004PASP..116..266B) is one of
the longest-running wide-field photometric surveys for transiting
planets. It employs a network of small robotic telescopes at
the Fred Lawrence Whipple Observatory (FLWO) in Arizona and at
Maunakea Observatory in Hawaii. Each survey field is 8°x8°, and
observations are obtained with the Sloan r' filter. HAT-P-69 and
HAT-P-70 were both independently identified as planet candidates by
the WASP survey (Schanche et al. 2019MNRAS.483.5534S). The northern
facility (SuperWASP-North) and the southern facility (WASP-South)
both consist of arrays of eight 200 mm f/1.8 Canon telephoto lenses
on a common mount. Each camera is coupled with 2Kx2K detectors,
yielding a field of view of 7.8°x7.8° per camera (Pollacco et
al. 2006PASP..118.1407P). HAT-P-69 was observed by both WASP-South and
SuperWASP-North, producing 25200 photometric points spanning from 2009
January 14 to 2012 April 23. HAT-P-70 was observed by SuperWASP-North,
producing 19200 observations spanning 2008 October 13 to 2011 February
4. A number of transit observations were obtained with the FLWO 1.2 m
telescope and KeplerCam, a 4Kx4K CCD camera operated with 2x2 binning,
giving a plate scale of 0.672"/pixel. Photometry was extracted
as per Bakos et al. (2010, J/ApJ/710/1724). Follow-up photometry
was also obtained using the Las Cumbres Observatory (LCO; Brown et
al. 2013PASP..125.1031B) network. These observations included transits
obtained via the 0.8 m LCO telescope located at the Byrne Observatory
at Sedgwick, California, using the SBIG STX-16803 4Kx4K camera with
a field of view of 16'x16'. Additional photometric follow-up was
obtained using the TRAPPIST (TRAnsiting Planets and PlanetesImals
Small Telescope) North facility (Jehin et al. 2011Msngr.145....2J;
Gillon et al. 2013, J/A+A/552/A82; Barkaoui et al. 2019, J/AJ/157/43)
at Oukaimeden Observatory in Morocco. TRAPPIST-North is a 0.6 m robotic
photometer employing a 2Kx2K CCD with a field of view of 19.8'x19.8'
at a plate scale of 0.6" per pixel. The Tillinghast Reflector
Echelle Spectrograph (TRES; Furesz 2008, PhD thesis Univ. Szeged)
on the 1.5 m telescope at FLWO, Arizona, was used to obtain dozens
of spectra for each system. TRES is a fiber-fed echelle spectrograph
with a spectral resolution of R=44000 over the wavelength region of
3850-9100 Å. The observing strategy and data reduction process are
described by Buchhave et al. (2012, J/other/Nat/486.375). For HAT-P-69,
relative radial velocities were obtained using a multiorder analysis
(Quinn et al. 2012, J/ApJ/745/80) of the TRES spectra. For HAT-P-70,
we modeled the stellar line profiles derived from a least-squares
deconvolution (LSD; Donati et al. 1997MNRAS.291..658D) to derive the
absolute radial velocities of each spectrum. <P />(8 data files).
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Title: VizieR Online Data Catalog: HAT-TR-318-007: a double-lined
M dwarf binary (Hartman+, 2018)
Authors: Hartman, J. D.; Quinn, S. N.; Bakos, G. A.; Torres, G.;
Kovacs, G.; Latham, D. W.; Noyes, R. W.; Shporer, A.; Fulton, B. J.;
Esquerdo, G. A.; Everett, M. E.; Penev, K.; Bhatti, W.; Csubry, Z.
2018yCat..51550114H Altcode:
HAT-TR-318-007 was initially detected as a candidate transiting planet
system by the HATNet survey (Bakos et al. 2004PASP..116..266B). The
available HATNet observations data of this system are provided in Table
2. In order to determine the atmospheric parameters for the individual
components of HAT-TR-318-007, we obtained medium-resolution NIR spectra
using the Folded-port InfraRed Echellette (FIRE) spectrograph (Simcoe
et al. 2013PASP..125..270S) on the 6.5 m Magellan Baade telescope at
Las Campanas Observatory in Chile. Observations were conducted during
the last ~4 hr before twilight on the UT nights of 2011 December 09,
10, and 11, with a total secondary eclipse occurring during the night
of 2011 December 10. We observed HAT-TR-318-007 continuously over an
83-minute period encompassing the secondary eclipse and on each of the
nights before and after the eclipse. For calibration we also observed
a number of M dwarf standard stars. The data are provided in Table
6. <P />(7 data files).
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Title: VizieR Online Data Catalog: Differential photometry of the
F-subgiant HAT-P-67 (Zhou+, 2017)
Authors: Zhou, G.; Bakos, G. A.; Hartman, J. D.; Latham, D. W.; Torres,
G.; Bhatti, W.; Penev, K.; Buchhave, L.; Kovacs, G.; Bieryla, A.;
Quinn, S.; Isaacson, H.; Fulton, B. J.; Falco, E.; Csubry, Z.; Everett,
M.; Szklenar, T.; Esquerdo, G.; Berlind, P.; Calkins, M. L.; Beky, B.;
Knox, R. P.; Hinz, P.; Horch, E. P.; Hirsch, L.; Howell, S. B.; Noyes,
R. W.; Marcy, G.; de Val-Borro, M.; Lazar, J.; Papp, I.; Sari, P.
2018yCat..51530211Z Altcode:
The transits of HAT-P-67b were first detected with the HATNet survey
(Bakos et al. 2004PASP..116..266B). HATNet employs a network of small,
wide field telescopes, located at the Fred Lawrence Whipple Observatory
(FLWO) in Arizona and at the Mauna Kea Observatory (MKO) in Hawaii,
to photometrically monitor selected 8x8° fields of the sky. A total
of 4050 I band observations were taken by HAT-5 and HAT-8 from 2005
January to July, and an additional 4518 observations were obtained in
the Cousins R band using HAT-5, HAT-7, and HAT-8 telescopes between 2008
February and August. To better characterize the planetary properties,
follow-up photometry of the transits were obtained using the KeplerCam
on the FWLO 1.2 m telescope. KeplerCam is a 4Kx4K CCD camera with a
pixel scale of 0.672"/pixel at 2x2 pixel binning. The photometry was
reduced as per Bakos et al. (2010, J/ApJ/710/1724). A full transit
was observed in the Sloan-i band on 2012 May 28, and five partial
transits were observed on 2011 April 15, May 19, June 07, and 2013
April 25 in the Sloan-i band, and 2013 May 24 in the Sloan-z band. <P
/>(1 data file).
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Title: HAT-TR-318-007: A Double-lined M Dwarf Binary with Total
Secondary Eclipses Discovered by HATNet and Observed by K2
Authors: Hartman, J. D.; Quinn, S. N.; Bakos, G. Á.; Torres, G.;
Kovács, G.; Latham, D. W.; Noyes, R. W.; Shporer, A.; Fulton, B. J.;
Esquerdo, G. A.; Everett, M. E.; Penev, K.; Bhatti, W.; Csubry, Z.
2018AJ....155..114H Altcode: 2018arXiv180103570H
We report the discovery by the HATNet survey of HAT-TR-318-007,
a P=3.34395390+/- 0.00000020 day period detached double-lined
M dwarf binary with total secondary eclipses. We combine radial
velocity (RV) measurements from TRES/FLWO 1.5 m and time-series
photometry from HATNet, FLWO 1.2 m, BOS 0.8 m, and NASA K2
Campaign 5, to determine the masses and radii of the component
stars: M<SUB>A</SUB>=0.448+/-0.011 M<SUB>⊙</SUB><SUP>N</SUP>,
M<SUB>B</SUB>=0.2721<SUB>-0.0042</SUB><SUP>+0.0041</SUP>
M<SUB>⊙</SUB><SUP>N</SUP>,
R<SUB>A</SUB>=0.4548<SUB>-0.0036</SUB><SUP>+0.0035</SUP>
R<SUB>⊙</SUB><SUP>N</SUP>, and
R<SUB>B</SUB>=0.2913<SUB>-0.0024</SUB><SUP>+0.0023</SUP>
R<SUB>⊙</SUB><SUP>N</SUP>. We obtained a FIRE/Magellan near-infrared
spectrum of the primary star during a total secondary eclipse, and we
use this to obtain disentangled spectra of both components. We determine
spectral types of ST<SUB>A</SUB>=M 3.71+/- 0.69 and ST<SUB>B</SUB>=M
5.01+/- 0.73 and effective temperatures of T<SUB>eff</SUB>, A=
3190+/-110 K and T<SUB>eff</SUB>, B=3100+/- 110 K for the primary
and secondary star, respectively. We also measure a metallicity of
[Fe/H] = +0.298+/- 0.080 for the system. We find that the system
has a small, but significant, nonzero eccentricity of 0.0136+/-
0.0026. The K2 light curve shows a coherent variation at a period
of 3.41315<SUB>-0.00032</SUB><SUP>+0.00030</SUP> days, which is
slightly longer than the orbital period, and which we demonstrate
comes from the primary star. We interpret this as the rotation
period of the primary. We perform a quantitative comparison
between the Dartmouth stellar evolution models and the seven
systems, including HAT-TR-318-007, that contain M dwarfs with 0.2
M<SUB>⊙</SUB><SUP>N</SUP>< M< 0.5 M<SUB>⊙</SUB><SUP>N</SUP>,
have metallicity measurements, and have masses and radii determined
to better than 5% precision. Discrepancies between the predicted and
observed masses and radii are found for three of the systems.
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Title: VizieR Online Data Catalog: Differential photometry of the EB*
HATS551-027 (Zhou+, 2015)
Authors: Zhou, G.; Bayliss, D.; Hartman, J. D.; Rabus, M.; Bakos,
G. A.; Jordan, A.; Brahm, R.; Penev, K.; Csubry, Z.; Mancini, L.;
Espinoza, N.; de Val-Borro, M.; Bhatti, W.; Ciceri, S.; Henning, T.;
Schmidt, B.; Murphy, S. J.; Butler, R. P.; Arriagada, P.; Shectman,
S.; Crane, J.; Thompson, I.; Suc, V.; Noyes, R. W.
2017yCat..74512263Z Altcode:
The eclipses of HATS551-027 were first identified by observations from
the HATSouth survey (Bakos et al. 2013PASP..125..154B). HATSouth is
a global network of identical, fully robotic telescopes, providing
continuous monitoring of selected 128 deg<SUP>2</SUP> fields of
the southern sky. A total of 16622 observations of HATS551-027 were
obtained from HATSouth units HS-1, HS-2 in Chile, HS-3, HS-4 in Namibia,
and HS-6 in Australia from 2009 September to 2010 September. Two
secondary eclipses of HATS551-027 were observed by the Merope camera
on 2-m Faulkes Telescope South (FTS), at Siding Spring Observatory,
on 2012 December 12 and 2013 March 20. A near-complete primary eclipse
of HATS551-027 was observed by the SITe#3 camera on the Swope 1 m
telescope at Las Campanas Observatory, Chile, on 2013 February 26. <P
/>(1 data file).
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Title: HATS-22b, HATS-23b and HATS-24b: three new transiting
super-Jupiters from the HATSouth project
Authors: Bento, J.; Schmidt, B.; Hartman, J. D.; Bakos, G. Á.; Ciceri,
S.; Brahm, R.; Bayliss, D.; Espinoza, N.; Zhou, G.; Rabus, M.; Bhatti,
W.; Penev, K.; Csubry, Z.; Jordán, A.; Mancini, L.; Henning, T.;
de Val-Borro, M.; Tinney, C. G.; Wright, D. J.; Durkan, S.; Suc, V.;
Noyes, R.; Lázár, J.; Papp, I.; Sári, P.
2017MNRAS.468..835B Altcode: 2016arXiv160700688B
We report the discovery of three moderately high-mass transiting
hot Jupiters from the HATSouth survey: HATS-22b, HATS-23b and
HATS-24b. These planets add to the number of known planets in the
∼2M<SUB>J</SUB> regime. HATS-22b is a 2.74 ± 0.11 M<SUB>J</SUB>
mass and 0.953_{-0.029}^{+0.048} R_J radius planet orbiting a V =
13.455 ± 0.040 sub-solar mass (M<SUB>*</SUB> = 0.759 ± 0.019
M<SUB>⊙</SUB>; R<SUB>*</SUB> = 0.759 ± 0.019 R<SUB>⊙</SUB>)
K-dwarf host star on an eccentric (e = 0.079 ± 0.026) orbit. This
planet's high planet-to-stellar mass ratio is further evidence that
migration mechanisms for hot Jupiters may rely on exciting orbital
eccentricities that bring the planets closer to their parent stars
followed by tidal circularization. HATS-23b is a 1.478 ± 0.080
M<SUB>J</SUB> mass and 1.69 ± 0.24 R<SUB>J</SUB> radius planet on a
grazing orbit around a V = 13.901 ± 0.010 G-dwarf with properties
very similar to those of the Sun (M<SUB>*</SUB> = 1.115 ± 0.054;
R<SUB>*</SUB> = 1.145 ± 0.070). HATS-24b orbits a moderately bright
V = 12.830 ± 0.010 F-dwarf star (M<SUB>*</SUB> = 1.218 ± 0.036
M<SUB>⊙</SUB>; R_\star = 1.194_{-0.041}^{+0.066} R_{⊙}). This
planet has a mass of 2.39_{-0.12}^{+0.21} M_J and an inflated radius
of 1.516_{-0.065}^{+0.085} R_J.
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Title: VizieR Online Data Catalog: i filter photometry for HATS-25
through HATS-30 (Espinoza+, 2016)
Authors: Espinoza, N.; Bayliss, D.; Hartman, J. D.; Bakos, G. A.;
Jordan, A.; Zhou, G.; Mancini, L.; Brahm, R.; Ciceri, S.; Bhatti,
W.; Csubry, Z.; Rabus, M.; Penev, K.; Bento, J.; de Val-Borro, M.;
Henning, T.; Schmidt, B.; Suc, V.; Wright, D. J.; Tinney, C. G.; Tan,
T. G.; Noyes, R.
2017yCat..51520108E Altcode:
The photometric detection data of the six exoplanets come from the
three HATSouth sites, namely, the site at Las Campanas Observatory in
Chile (LCO, whose stations are designated HS-1 and HS-2), the site
at of the High Energy Spectroscopic Survey (HESS) in Namibia (whose
stations are designated HS-3 and HS-4) and the site at the Siding
Spring Observatory (SSO) in Australia whose stations are designated
HS-5 and HS-6). <P />HATS-25 was observed with an r SDSS filter on
2011 Mar-2011 Aug using HS-2.1, on 2011 Jul-2011 Aug using HS-4.1, and
on 2011 May with HS-6.1. HATS-26 was observed with an r SDSS filter
on 2012 Feb-2012 Jun using HS-2.3, HS-4.3, and HS-6.3. HATS-27 was
observed with an r SDSS filter on 2011 Apr-2012 Jul using HS-2.1,
on 2011 Jul-2012 Jul using HS-4.1, and on 2011 May-2012 Jul using
HS-6.1. HATS-28 was observed with an r SDSS filter on 2013 Mar-2013 Oct
using HS-1.2, on 2013 Sep-2013 Oct using HS-2.2, on 2013 Apr-2013 Nov
using HS-3.2, on 2013 Sep-2013 Nov using HS-4.2 and HS-6.2, and 2013
Mar-2013 Nov using HS-5.2. HATS-29 was observed with an r SDSS filter
on 2013 Apr-2013 May using HS-1.1, on 2013 Sep-2013 Oct using HS-2.1,
on 2013 Apr-2013 Nov using HS-3.1, on 2013 Sep-2013 Nov using HS-4.1
and HS-6.1, and on 2013 Mar-2013 Nov using HS-5.1. HATS-30 was observed
using an r SDSS filter on 2012 Sep-2012 Dec using HS-2.3, HS-6.3 and
HS-2.4, on 2012 Sep-2013 Jan using HS-4.4, on 2012 Sep-2012 Dec using
HS-6.4, and on 2011 Jul-2012 Oct using HS-1.1, HS-3.1 and HS-5.1. <P
/>Photometric follow-up for the six systems was obtained mainly from
1m-class telescopes at different sites of the Las Cumbres Observatory
Global Telescope (LCOGT) network, using the i filter. In particular,
one partial transit and a full transit was observed for HATS-25b on 2015
February 23 at Cerro Tololo Inter-American Observatory (CTIO) and 2015
March 16 at SSO, respectively; three partial transits were observed for
HATS-26b on 2015 April 19 and 2015 May 21 at CTIO, and 2015 June 04 at
SSO; one full transit was observed for HATS-27b on 2015 April 09 at SSO;
two partial transits were observed for HATS-28b on 2015 August 31 and
2015 September 03 at CTIO; one full transit and a partial transit were
observed for HATS-29b on 2015 and 2014 June, respectively, at CTIO;
and two partial transits were observed for HATS-30b on 2014 October
19 at South African Astronomical Observatory (SAAO) and on 2014 Oct
23 at CTIO. In addition, one full transit of HATS-27b was observed
using the 0.3m Perth Exoplanet Survey Telescope (PEST) on 2015 March
12 using a R<SUB>C</SUB> filter. <P />The reconnaissance spectroscopy
of our candidates was made using the Wide Field Spectrograph (WiFeS),
located on the Australian National University (ANU) 2.3m telescope. The
observing strategy usually consists of taking data with two resolutions:
R=λ/Δλ=7000 (medium) and R=3000 (low). For HATS-25, four medium
resolution spectra (2014 Jun-Aug) and one low resolution spectrum (2014
Aug 5) were obtained. For HATS-26, two medium resolution spectra (2014
Jun 3-5) and one low resolution spectrum (2014 Jun 4) were obtained. For
HATS-27, three medium resolution (2014 Jun 3-5) and one low resolution
(2014 Jun 2) spectra were obtained. For HATS-28, only one low resolution
spectrum (2015 Jun 1) was obtained. For HATS-29, four medium resolution
spectra (2014 Dec-2015 Mar) and one low resolution spectrum (2015
Mar 2) were obtained. For HATS-30, three medium resolution spectra
(2014 Oct 4-10) and one low resolution spectrum (2014 Oct 4) were
obtained. <P />High-precision spectroscopy was obtained for our targets
with different instruments. Several R=115000 spectra were taken with
the High Accuracy Radial Velocity Planet Searcher (HARPS) on the ESO
3.6m telescope at La Silla Observatory (LSO) between 2015 February
and 2016 March in order to obtain high-precision radial velocities for
HATS-25, HATS-26, HATS-27, and HATS-29. Spectra with R=48000 were also
taken with the Fiber-fed Extended Range Optical Spectrograph (FEROS)
mounted on the Max Planck Gesellschaft (MPG) 2.2m telescope at La
Silla Observatory (LSO) between 2014 July and 2015 July in order to
both extract precise spectroscopic parameters of the host stars and
obtain precise radial velocities for all of our targets. In addition,
R=60000 spectra were also taken with the CORALIE spectrograph mounted
on the 1.2m Euler telescope at LSO between 2014 June and November for
HATS-26, HATS-27, HATS-29, and HATS-30. Finally, eight R=70000 spectra
were obtained for HATS-29 on 2015 May to measure radial velocities,
using the CYCLOPS2 fiber feed with the University College London
Echelle Spectrograph (UCLES) on the 3.9m Anglo-Australian Telescope
(AAT). <P />(3 data files).
---------------------------------------------------------
Title: HAT-P-67b: An Extremely Low Density Saturn Transiting an
F-subgiant Confirmed via Doppler Tomography
Authors: Zhou, G.; Bakos, G. Á.; Hartman, J. D.; Latham, D. W.;
Torres, G.; Bhatti, W.; Penev, K.; Buchhave, L.; Kovács, G.; Bieryla,
A.; Quinn, S.; Isaacson, H.; Fulton, B. J.; Falco, E.; Csubry, Z.;
Everett, M.; Szklenar, T.; Esquerdo, G.; Berlind, P.; Calkins, M. L.;
Béky, B.; Knox, R. P.; Hinz, P.; Horch, E. P.; Hirsch, L.; Howell,
S. B.; Noyes, R. W.; Marcy, G.; de Val-Borro, M.; Lázár, J.; Papp,
I.; Sári, P.
2017AJ....153..211Z Altcode: 2017arXiv170200106Z
We report the discovery of HAT-P-67b, which is a hot-Saturn
transiting a rapidly rotating F-subgiant. HAT-P-67b has a radius of
{R}<SUB>{{p</SUB>}}={2.085}<SUB>-0.071</SUB><SUP>+0.096</SUP>
{R}<SUB>{{J</SUB>}}, and orbites a {M}<SUB>*
</SUB>={1.642}<SUB>-0.072</SUB><SUP>+0.155</SUP> {M}<SUB>⊙ </SUB>,
{R}<SUB>* </SUB>={2.546}<SUB>-0.084</SUB><SUP>+0.099</SUP> {R}<SUB>⊙
</SUB> host star in a ∼4.81 day period orbit. We place an upper
limit on the mass of the planet via radial velocity measurements
to be {M}<SUB>{{p</SUB>}}< 0.59 {M}<SUB>{{J</SUB>}}, and a lower
limit of > 0.056 {M}<SUB>{{J</SUB>}} by limitations on Roche lobe
overflow. Despite being a subgiant, the host star still exhibits
relatively rapid rotation, with a projected rotational velocity of
v\sin {I}<SUB>\star </SUB>=35.8+/- 1.1 {km} {{{s}}}<SUP>-1</SUP>,
which makes it difficult to precisely determine the mass of the planet
using radial velocities. We validated HAT-P-67b via two Doppler
tomographic detections of the planetary transit, which eliminate
potential eclipsing binary blend scenarios. The Doppler tomographic
observations also confirm that HAT-P-67b has an orbit that is aligned to
within 12°, in projection, with the spin of its host star. HAT-P-67b
receives strong UV irradiation and is among one of the lowest density
planets known, which makes it a good candidate for future UV transit
observations in the search for an extended hydrogen exosphere. <P
/>Based on observations obtained with the Hungarian-made Automated
Telescope Network. Based in part on observations made with the Keck-I
telescope at Mauna Kea Observatory, HI (Keck time awarded through
NASA programs N029Hr, N108Hr, N154Hr, and N130Hr; and NOAO programs
A289Hr and A284Hr). Based in part on observations obtained with the
Tillinghast Reflector 1.5 m telescope and the 1.2 m telescope, both of
which are operated by the Smithsonian Astrophysical Observatory at the
Fred Lawrence Whipple Observatory in Arizona. This work makes use of
the Smithsonian Institution High Performance Cluster (SI/HPC). Based in
part on observations made with the Nordic Optical Telescope, operated
on the island of La Palma jointly by Denmark, Finland, Iceland, Norway,
and Sweden, in the Spanish Observatorio del Roque de los Muchachos of
the Instituto de Astrofísica de Canarias.
---------------------------------------------------------
Title: VizieR Online Data Catalog: Sloan i follow-up light curves
of HATS-18 (Penev+, 2016)
Authors: Penev, K.; Hartman, J. D.; Bakos, G. A.; Ciceri, S.; Brahm,
R.; Bayliss, D.; Bento, J.; Jordan, A.; Csubry, Z.; Bhatti, W.; de
Val-Borro, M.; Espinoza, N.; Zhou, G.; Mancini, L.; Rabus, M.; Suc, V.;
Henning, T.; Schmidt, B.; Noyes, R. W.; Lazar, J.; Papp, I.; Sari, P.
2017yCat..51520127P Altcode:
The star HATS-18 was observed by HATSouth instruments between UT
2011 April 18 and UT 2013 July 21 using the HS-2, HS-4, and HS-6
units at the Las Campanas Observatory in Chile, the High Energy
Spectroscopic Survey (H.E.S.S.) site in Namibia, and Siding Spring
Observatory (SSO) in Australia, respectively. A total of 5372, 3758,
and 4008 images of HATS-18 were obtained with HS-2, HS-4, and HS-6,
respectively. The observations were obtained through a Sloan r filter
with an exposure time of 240s. <P />We obtained follow-up light curves
of HATS-18 using the Las Cumbres Observatory Global Telescope (LCOGT)
1m telescope network. An ingress was observed on UT 2015 July 18 with
the SBIG camera and a Sloan i filter on the 1m at the South African
Astronomical Observatory (SAAO). A total of 33 images were collected
at a median cadence of 201s. A full transit was observed on UT 2016
January 22 with the sinistro camera and a Sloan i filter on the 1m
at Cerro Tololo Inter-American Observatory. A total of 61 images were
collected at a median cadence of 219s. For the record, we also note that
a full transit was observed on UT 2016 January 3 with the SBIG camera
on the 1m at SAAO; however, due to tracking and weather problems, we
were unable to extract high-precision photometry from these images,
and therefore do not include these data in our analysis. The data
are available in Table1. <P />Spectroscopic follow-up observations
of HATS-18 were carried out with WiFeS on the Australian National
University (ANU) 2.3m telescope and with the Fiber-fed Extended Range
Optical Spectrograph (FEROS) on the MPG 2.2m. A total of three spectra
were obtained with WiFeS between UT 2015 February 28 and UT 2015
March 2, two at a resolution of R=Δλ/λ=7000, and one at R=3000. We
obtained six R=48000 spectra with FEROS between UT 2015 June 12 and
UT 2015 June 20. The data are provided in Table2. <P />(2 data files).
---------------------------------------------------------
Title: HATS-18b: An Extreme Short-period Massive Transiting Planet
Spinning Up Its Star
Authors: Penev, K.; Hartman, J. D.; Bakos, G. Á.; Ciceri, S.; Brahm,
R.; Bayliss, D.; Bento, J.; Jordán, A.; Csubry, Z.; Bhatti, W.;
de Val-Borro, M.; Espinoza, N.; Zhou, G.; Mancini, L.; Rabus, M.;
Suc, V.; Henning, T.; Schmidt, B.; Noyes, R. W.; Lázár, J.; Papp,
I.; Sári, P.
2016AJ....152..127P Altcode: 2016arXiv160600848P
We report the discovery by the HATSouth network of HATS-18b: a 1.980+/-
0.077 {M}<SUB>{{J</SUB>}}, {1.337}<SUB>-0.049</SUB><SUP>+0.102</SUP>
{R}<SUB>{{J</SUB>}} planet in a 0.8378 day orbit, around a solar
analog star (mass 1.037+/- 0.047 {M}<SUB>⊙ </SUB> and radius
{1.020}<SUB>-0.031</SUB><SUP>+0.057</SUP> {R}<SUB>⊙ </SUB>)
with V=14.067+/- 0.040 mag. The high planet mass, combined with
its short orbital period, implies strong tidal coupling between
the planetary orbit and the star. In fact, given its inferred age,
HATS-18 shows evidence of significant tidal spin up, which together
with WASP-19 (a very similar system) allows us to constrain the
tidal quality factor for Sun-like stars to be in the range of 6.5≲
{{log}}<SUB>10</SUB>({Q}<SUP>* </SUP>/{k}<SUB>2</SUB>)≲ 7 even after
allowing for extremely pessimistic model uncertainties. In addition, the
HATS-18 system is among the best systems (and often the best system) for
testing a multitude of star-planet interactions, be they gravitational,
magnetic, or radiative, as well as planet formation and migration
theories. <P />The HATSouth network is operated by a collaboration
consisting of Princeton University (PU), the Max Planck Institute für
Astronomie (MPIA), the Australian National University (ANU), and the
Pontificia Universidad Católica de Chile (PUC). The station at Las
Campanas Observatory (LCO) of the Carnegie Institute is operated by PU
in conjunction with PUC, the station at the High Energy Spectroscopic
Survey (H.E.S.S.) site is operated in conjunction with MPIA, and the
station at Siding Spring Observatory (SSO) is operated jointly with
ANU. This paper includes data gathered with the MPG 2.2 m telescope at
the ESO Observatory in La Silla. This paper uses observations obtained
with facilities of the Las Cumbres Observatory Global Telescope.
---------------------------------------------------------
Title: VizieR Online Data Catalog: Spectroscopy and photometry of
HATS-11 and HATS-12 (Rabus+, 2016)
Authors: Rabus, M.; Jordan, A.; Hartman, J. D.; Bakos, G. A.; Espinoza,
N.; Brahm, R.; Penev, K.; Ciceri, S.; Zhou, G.; Bayliss, D.; Mancini,
L.; Bhatti, W.; de Val-Borro, M.; Csbury, Z.; Sato, B.; Tan, T. -G.;
Henning, T.; Schmidt, B.; Bento, J.; Suc, V.; Noyes, R.; Lazar, J.;
Papp, I.; Sari, P.
2016yCat..51520088R Altcode:
The initial images of HATS-11 and HATS-12 were obtained with the
HATSouth wide-field telescope network consisting of 24 Takahashi E180
astrographs with an aperture of 18cm. The photons were detected with
Apogee 4k*4k U16M ALTA CCDs. Details on the time span and number of
images are shown in Table1. The numerical data of the light curves are
available in Table3. <P />The spectroscopic observations are summarized
in Table2. The data for the phased high-precision radial velocity and
bisector span measurements are presented in Table6. <P />Photometric
follow-up observations are summarized in Table1. The data are given
in Table3. <P />(5 data files).
---------------------------------------------------------
Title: HATS-25b through HATS-30b: A Half-dozen New Inflated Transiting
Hot Jupiters from the HATSouth Survey
Authors: Espinoza, N.; Bayliss, D.; Hartman, J. D.; Bakos, G. Á.;
Jordán, A.; Zhou, G.; Mancini, L.; Brahm, R.; Ciceri, S.; Bhatti,
W.; Csubry, Z.; Rabus, M.; Penev, K.; Bento, J.; de Val-Borro, M.;
Henning, T.; Schmidt, B.; Suc, V.; Wright, D. J.; Tinney, C. G.; Tan,
T. G.; Noyes, R.
2016AJ....152..108E Altcode: 2016arXiv160600023E
We report six new inflated hot Jupiters (HATS-25b through
HATS-30b) discovered using the HATSouth global network
of automated telescopes. The planets orbit stars with V
magnitudes in the range of ∼12-14 and have masses in the
largely populated 0.5{M}<SUB>J</SUB>{--}0.7{M}<SUB>J</SUB>
region of parameter space but span a wide variety of radii,
from 1.17{R}<SUB>J</SUB> to 1.75{R}<SUB>J</SUB>. HATS-25b,
HATS-28b, HATS-29b, and HATS-30b are typical inflated hot Jupiters
({R}<SUB>p</SUB>=1.17{--}1.26{R}<SUB>J</SUB>) orbiting G-type
stars in short period (P = 3.2-4.6 days) orbits. However, HATS-26b
({R}<SUB>p</SUB>=1.75{R}<SUB>J</SUB>, P=3.3024 days) and HATS-27b
({R}<SUB>p</SUB>=1.50{R}<SUB>J</SUB>, P=4.6370 days) stand out as highly
inflated planets orbiting slightly evolved F stars just after and in
the turn-off points, respectively, which are among the least dense hot
Jupiters, with densities of 0.153 {{g}} {cm}}<SUP>-3</SUP> and 0.180
{{g}} {cm}}<SUP>-3</SUP>, respectively. All the presented exoplanets
but HATS-27b are good targets for future atmospheric characterization
studies, while HATS-27b is a prime target for Rossiter—McLaughlin
monitoring in order to determine its spin-orbit alignment given the
brightness (V = 12.8) and stellar rotational velocity (v\sin i≈ 9.3
km s<SUP>-1</SUP>) of the host star. These discoveries significantly
increase the number of inflated hot Jupiters known, contributing to
our understanding of the mechanism(s) responsible for hot Jupiter
inflation. <P />The HATSouth network is operated by a collaboration
consisting of Princeton University (PU), the Max Planck Institute für
Astronomie (MPIA), the Australian National University (ANU), and the
Pontificia Universidad Católica de Chile (PUC). The station at Las
Campanas Observatory (LCO) of the Carnegie Institute is operated by PU
in conjunction with PUC, the station at the High Energy Spectroscopic
Survey (H.E.S.S.) site is operated in conjunction with MPIA, and the
station at Siding Spring Observatory (SSO) is operated jointly with
ANU. Based in part on observations made with the MPG 2.2 m Telescope
at the ESO Observatory in La Silla.
---------------------------------------------------------
Title: HATS-11b AND HATS-12b: Two Transiting Hot Jupiters Orbiting
Subsolar Metallicity Stars Selected for the K2 Campaign 7
Authors: Rabus, M.; Jordán, A.; Hartman, J. D.; Bakos, G. Á.;
Espinoza, N.; Brahm, R.; Penev, K.; Ciceri, S.; Zhou, G.; Bayliss,
D.; Mancini, L.; Bhatti, W.; de Val-Borro, M.; Csbury, Z.; Sato, B.;
Tan, T. -G.; Henning, T.; Schmidt, B.; Bento, J.; Suc, V.; Noyes,
R.; Lázár, J.; Papp, I.; Sári, P.
2016AJ....152...88R Altcode: 2016arXiv160302894R
We report the discovery of two transiting extrasolar planets from the
HATSouth survey. HATS-11, a V = 14.1 G0-star shows a periodic 12.9 mmag
dip in its light curve every 3.6192 days and a radial velocity variation
consistent with a Keplerian orbit. HATS-11 has a mass of 1.000+/- 0.060
{M}<SUB>⊙ </SUB>, a radius of 1.444+/- 0.057 {R}<SUB>⊙ </SUB> and
an effective temperature of 6060+/- 150 K, while its companion is a
0.85+/- 0.12 {M}<SUB>{{J</SUB>}}, 1.510+/- 0.078 {R}<SUB>{{J</SUB>}}
planet in a circular orbit. HATS-12 shows a periodic 5.1 mmag flux
decrease every 3.1428 days and Keplerian RV variations around a V =
12.8 F-star. HATS-12 has a mass of 1.489+/- 0.071 {M}<SUB>⊙ </SUB>, a
radius of 2.21+/- 0.21 {R}<SUB>⊙ </SUB>, and an effective temperature
of 6408+/- 75 K. For HATS-12b, our measurements indicate that this is
a 2.38+/- 0.11 {M}<SUB>{{J</SUB>}}, 1.35+/- 0.17 {R}<SUB>{{J</SUB>}}
planet in a circular orbit. Both host stars show subsolar metallicities
of -0.390+/- 0.060 dex and -0.100+/- 0.040 dex, respectively, and are
(slightly) evolved stars. In fact, HATS-11 is among the most metal-poor
and, HATS-12, with a {log}{g}<SUB>\star </SUB> of 3.923+/- 0.065, is
among the most evolved stars hosting a hot-Jupiter planet. Importantly,
HATS-11 and HATS-12 have been observed in long cadence by Kepler as part
of K2 campaign 7 (EPIC216414930 and EPIC218131080 respectively). <P
/>The HATSouth network is operated by a collaboration consisting of
Princeton University (PU), the Max Planck Institute für Astronomie
(MPIA), the Australian National University (ANU), and the Pontificia
Universidad Católica de Chile (PUC). The station at Las Campanas
Observatory (LCO) of the Carnegie Institute is operated by PU in
conjunction with PUC, the station at the High Energy Spectroscopic
Survey (H.E.S.S.) site is operated in conjunction with MPIA, and the
station at Siding Spring Observatory (SSO) is operated jointly with
ANU. Based in part on data collected at the Subaru Telescope, which
is operated by the National Astronomical Observatory of Japan. Based
in part on observations made with the MPG 2.2 m Telescope at the ESO
Observatory in La Silla.
---------------------------------------------------------
Title: HATS-15b and HATS-16b: Two Massive Planets Transiting Old G
Dwarf Stars
Authors: Ciceri, S.; Mancini, L.; Henning, T.; Bakos, G.; Penev, K.;
Brahm, R.; Zhou, G.; Hartman, J. D.; Bayliss, D.; Jordán, A.; Csubry,
Z.; de Val-Borro, M.; Bhatti, W.; Rabus, M.; Espinoza, N.; Suc, V.;
Schmidt, B.; Noyes, R.; Howard, A. W.; Fulton, B. J.; Isaacson, H.;
Marcy, G. W.; Butler, R. P.; Arriagada, P.; Crane, J. D.; Shectman,
S.; Thompson, I.; Tan, T. G.; Lázár, J.; Papp, I.; Sari, P.
2016PASP..128g4401C Altcode: 2015arXiv151106305C
We report the discovery of HATS-15 b and HATS-16 b, two massive
transiting extrasolar planets orbiting evolved (∼10 Gyr)
main-sequence stars. The planet HATS-15 b, which is hosted by a G9
V star (V=14.8 mag), is a hot Jupiter with mass of 2.17\quad +/-
\quad 0.15 {M}<SUB>{{J</SUB>}} and radius of 1.105\quad +/- \quad
0.040 {R}<SUB>{{J</SUB>}}, and it completes its orbit in about 1.7
days. HATS-16 b is a very massive hot Jupiter with mass of 3.27\quad
+/- \quad 0.19 {M}<SUB>{{J</SUB>}} and radius of 1.30\quad +/- \quad
0.15 {R}<SUB>{{J</SUB>}}; it orbits around its G3 V parent star
(V=13.8 mag) in ∼2.7 days. HATS-16 is slightly active and shows
a periodic photometric modulation, implying a rotational period of
12 days, which is unexpectedly short given its isochronal age. This
fast rotation might be the result of the tidal interaction between
the star and its planet. <P />The HATSouth network is operated by a
collaboration consisting of Princeton University (PU), the Max Planck
Institute für Astronomie (MPIA), the Australian National University
(ANU), and the Pontificia Universidad Católica de Chile (PUC). The
station at Las Campanas Observatory (LCO) of the Carnegie Institute is
operated by PU in conjunction with PUC, the station at the High Energy
Spectroscopic Survey (H.E.S.S.) site is operated in conjunction with
MPIA, and the station at Siding Spring Observatory (SSO) is operated
jointly with ANU. Based in part on observations performed at the ESO
La Silla Observatory in Chile, with the Coralie and FEROS spectrographs
mounted on the Euler-Swiss and MPG 2.2 m telescopes, respectively. This
paper includes data gathered with the 6.5 m Magellan Telescopes located
at Las Campanas Observatory, Chile. Based in part on data collected
at Keck Telescope. Observations obtained with facilities of the Las
Cumbres Observatory Global Telescope are used in this paper.
---------------------------------------------------------
Title: HAT-P-47b AND HAT-P-48b: Two Low Density Sub-Saturn-Mass
Transiting Planets on the Edge of the Period--Mass Desert
Authors: Bakos, G. Á.; Hartman, J. D.; Torres, G.; Latham, D. W.;
Sato, B.; Bieryla, A.; Shporer, A.; Howard, A. W.; Fulton, B. J.;
Buchhave, L. A.; Penev, K.; Kovács, G.; Kovács, T.; Csubry, Z.;
Esquerdo, G. A.; Everett, M.; Szklenár, T.; Quinn, S. N.; Béky,
B.; Marcy, G. W.; Noyes, R. W.; Lázár, J.; Papp, I.; Sári, P.
2016arXiv160604556B Altcode:
We report the discovery of two new transiting extrasolar planets
orbiting moderately bright (V = 10.7 and 12.2 mag) F stars (masses of
1.39 Msun and 1.10 Msun, respectively). The planets have periods of P
= 4.7322 d and 4.4087 d, and masses of 0.21 MJ and 0.17 MJ which are
almost half-way between those of Neptune and Saturn. With radii of 1.31
RJ and 1.13 RJ, these very low density planets are the two lowest mass
planets with radii in excess that of Jupiter. Comparing with other
recent planet discoveries, we find that sub-Saturns (0.18MJ < Mp
< 0.3MJ) and super-Neptunes (0.05MJ < Mp < 0.18MJ) exhibit a
wide range of radii, and their radii exhibit a weaker correlation with
irradiation than higher mass planets. The two planets are both suitable
for measuring the Rossiter-McLaughlin effect and for atmospheric
characterization. Measuring the former effect would allow an interesting
test of the theory that star-planet tidal interactions are responsible
for the tendency of close-in giant planets around convective envelope
stars to be on low obliquity orbits. Both planets fall on the edge of
the short period Neptunian desert in the semi-major axis-mass plane.
---------------------------------------------------------
Title: VizieR Online Data Catalog: Photometry and spectroscopy of
HAT-P-57 (Hartman+, 2015)
Authors: Hartman, J. D.; Bakos, G. A.; Buchhave, L. A.; Torres, G.;
Latham, D. W.; Kovacs, G.; Bhatti, W.; Csubry, Z.; de Val-Borro,
M.; Penev, K.; Huang, C. X.; Beky, B.; Bieryla, A.; Quinn, S. N.;
Howard, A. W.; Marcy, G. W.; Johnson, J. A.; Isaacson, H.; Fischer,
D. A.; Noyes, R. W.; Falco, E.; Esquerdo, G. A.; Knox, R. P.; Hinz,
P.; Lazar, J.; Papp, I.; Sari, P.
2016yCat..51500197H Altcode:
The star HAT-P-57 was observed by the HATNet wide-field photometric
instruments between the nights of UT 2009 May 12 and UT 2009 September
14. A total of 622 observations of a 10.6°*10.6° field centered at
RA=06<SUP>h</SUP>24<SUP>m</SUP>, decl.=+30° were made with the HAT-5
telescope in Arizona, and 3202 observations of this same field were
made with the HAT-9 telescope in Hawaii. We used a Sloan r filter. <P
/>Photometric follow-up observations of HAT-P-57 were carried out
with KeplerCam on the Fred Lawrence Whipple Observatory (FLWO) 1.2m
telescope. We observed ingress events on the nights of 2010 April 3
and 2012 April 24, in i and g-bands respectively, and a full transit on
the night of 2010 June 26 in z-band. Additional photometric follow-up
observations were carried out with the FLWO 1.2m on the night of 2015
May 12. <P />All time-series photometric data that we collected for
HAT-P-57 are provided in Table1. <P />Spectroscopic observations were
obtained using the HIgh-Resolution Echelle Spectrometer (HIRES) on the
Keck-I 10m telescope between UT 2010 June 27 and UT 2012 March 10. A
total of 24 HIRES observations were collected during this time period,
including 14 observations made through the I<SUB>2</SUB> cell (e.g.,
Marcy & Butler, 1992PASP..104..270M), and 10 observations without
the I<SUB>2</SUB> cell. These latter observations were obtained on
the night of UT 2010 June 27, primarily during a planetary transit
(Section 3.3 discusses the analysis of these observations in more
detail). <P />Table2 gives the relative radial velocity measurements
obtained with the I<SUB>2</SUB> Doppler pipeline, the radial velocity
measurements obtained from the CCFs, and the Bisector Spans for the
HIRES observations. <P />(2 data files).
---------------------------------------------------------
Title: VizieR Online Data Catalog: Spectroscopy and photometry for
HAT-P-50--HAT-P-53 (Hartman+, 2015)
Authors: Hartman, J. D.; Bhatti, W.; Bakos, G. A.; Bieryla, A.;
Kovacs, G.; Latham, D. W.; Csubry, Z.; de Val-Borro, M.; Penev, K.;
Buchhave, L. A.; Torres, G.; Howard, A. W.; Marcy, G. W.; Johnson,
J. A.; Isaacson, H.; Sato, B.; Boisse, I.; Falco, E.; Everett, M. E.;
Szklenar, T.; Fulton, B. J.; Shporer, A.; Kovacs, T.; Hansen, T.;
Beky, B.; Noyes, R. W.; Lazar, J.; Papp, I.; Sari, P.
2016yCat..51500168H Altcode:
The HATNet network consists of six identical fully automated
instruments, with four at Fred Lawrence Whipple Observatory (FLWO) in
AZ, and two on the roof of the Submillimeter Array Hangar Building at
Mauna Kea Observatory (MKO) in HI. The light-gathering elements of each
instrument include an 11cm diameter telephoto lens, a Sloan r filter,
and a 4K*4K front-side-illuminated CCD camera. Observations made in
2007 and early 2008 were carried out using a Cousins R filter. The
instruments have a field of view of 10.6°*10.6° and a pixel scale
of 9"/pixel at the center of an image. <P />Additional time-series
photometric measurements were obtained for all four of the systems using
Keplercam on the FLWO 1.2m telescope. For HAT-P-50 we also obtained
follow-up photometry with the CCD imager on the Byrne Observatory at
Sedgwick (BOS) 0.8m telescope, located at Sedgwick Reserve in Santa
Ynez Valley, CA, and operated by the Las Cumbres Observatory Global
Telescope institute (LCOGT). <P />HAT-P-50 was observed with HAT-10/G316
on 2008 Nov-2009 May, with HAT-5/G364 on 2009 May, with HAT-9/G364
on 2008 Dec-2009 May, with BOS on 2012 Feb 15, on 2012 Feb 21 and on
2012 Apr 08, and with Keplercam on 2012 Feb 18, on 2012 Nov 28, on 2012
Dec 23, on 2013 Jan 14, and on 2013 Jan 17. HAT-P-51 was observed with
HAT-6/G164 on 2007 Sep-2008 Feb, with HAT-9/G164 on 2007 Sep-2008 Feb,
with HAT-10/G165 on 2010 Sep-2011 Jan, with HAT-5/G165 on 2010 Nov-2011
Feb, with HAT-8/G165 on 2010 Nov-2011 Feb, with HAT-6/G209 on 2010
Nov-2011 Feb, with HAT-9/G209 on 2010 Nov-2011 Feb, with HAT-7/G210
on 2010 Nov-2011 Jan, and with Keplercam on 2011 Oct 21, on 2012 Jan
05, on 2012 Oct 05, on 2012 Oct 26, and on 2012 Nov 12. HAT-P-52 was
observed with HAT-5/G212 on 2010 Sep-Nov, with HAT-8/G212 on 2010
Aug-Nov, and with Keplercam on 2010 Dec 23, on 2011 Sep 05, on 2011
Sep 27, on 2011 Nov 21, and on 2012 Jan 07. HAT-P-53 was observed with
HAT-6/G164 on 2007 Sep-2008 Feb, with HAT-9/G164 on 2007 Sep-2008
Feb, with HAT-10/G165 on 2010 Sep-2011 Jan, with HAT-5/G165 on 2010
Nov-2011 Feb, with HAT-8/G165 on 2010 Nov-2011 Feb, and with Keplercam
on 2011 Oct 19 and on 2011 Oct 27. <P />The facilities used for each
system include the Tillinghast Reflector Echelle Spectrograph (TRES;
Resolution Δλ/λ/1000=44) on the 1.5m Tillinghast Reflector at FLWO
(used on 2010 Dec-2012 Feb for HAT-P-50, on 2011 Sep 21 for HAT-P-51,
on 2010 Dec-2011 Jan for HAT-P-52, and on 2011 Sep 18-19 for HAT-P-53);
the Astrophysical Research Consortium Echelle Spectrometer (ARCES;
Resolution Δλ/λ/1000=31.5) on the ARC 3.5m telescope at Apache Point
Observatory (APO) in New Mexico (used on 2011 Sep 19 for HAT-P-51, and
on 2011 Sep 19-20 for HAT-P-53); the FIbre-fed Echelle Spectrograph
(FIES) at the 2.5m Nordic Optical Telescope (NOT) at La Palma, Spain
(used on 2012 Mar 13-17 with Δλ/λ/1000=67 for HAT-P-50, and on
2011 Aug 4 with Δλ/λ/1000=46 for HAT-P-51); the SOPHIE Spectrograph
(Resolution Δλ/λ/1000=39) on the 1.93m telescope at OHP in France
(used for HAT-P-51 on 2011 Dec 4-12; the HIgh Resolution Echelle
Spectrometer (HIRES; Resolution Δλ/λ/1000=55) on the Keck-I telescope
in Hawaii together with the I<SUB>2</SUB> absorption cell (used on
2011 Oct-2012 Feb for HAT-P-51, on 2011 Oct 19 and 2011 Feb-2012 Jul
for HAT-P-52, and on 2011 Nov 14 and 2011 Nov-2012 Feb for HAT-P-53);
and the High-Dispersion Spectrograph (HDS; Resolution Δλ/λ/1000=60)
with the I<SUB>2</SUB> absorption cell on the Subaru telescope in Hawaii
(used on 2012 Feb 7 and 2012 Feb-Sep for HAT-P-50, and on 2012 Feb 9
and 2012 Feb 7-10 for HAT-P-51). <P />The high-precision radial velocity
measurements for all objects are seen to vary in phase with the transit
ephemerides. The data are listed in Table4. All photometric measurements
made for the four objects are available in Table5. <P />(3 data files).
---------------------------------------------------------
Title: VizieR Online Data Catalog: Differential photometry of the
K dwarf HATS-7 (Bakos+, 2015)
Authors: Bakos, G. A.; Penev, K.; Bayliss, D.; Hartman, J. D.; Zhou,
G.; Brahm, R.; Mancini, L.; de Val-Borro, M.; Bhatti, W.; Jordan, A.;
Rabus, M.; Espinoza, N.; Csubry, Z.; Howard, A. W.; Fulton, B. J.;
Buchhave, L. A.; Ciceri, S.; Henning, T.; Schmidt, B.; Isaacson, H.;
Noyes, R. W.; Marcy, G. W.; Suc, V.; Howe, A. R.; Burrows, A. S.;
Lazar, J.; Papp, I.; Sari, P.
2016yCat..18130111B Altcode:
The star HATS-7 (2MASS J13552567-2112276) was observed by the
Hungarian-made Automated Telescope Network-South (HATSouth)
wide-field telescope network between UT 2011 March 24 and UT 2011
August 19. Observations were made from Las Campanas Observatory (LCO)
in Chile, the High Energy Stereoscopic System (HESS) site in Namibia,
and Siding Spring Observatory (SSO) in Australia. <P />Photometric
follow-up observations of HATS-7 were performed using the 1-m telescopes
in the Las Cumbres Observatory Global Telescope network (LCOGT) and
the GROND instrument on the MPG 2.2m telescope at La Silla Observatory
(LSO) in Chile; in 2014 Jun 12,16 and 2014 Jul 20. <P />(1 data file).
---------------------------------------------------------
Title: HAT-P-57b: A Short-period Giant Planet Transiting a Bright
Rapidly Rotating A8V Star Confirmed Via Doppler Tomography
Authors: Hartman, J. D.; Bakos, G. Á.; Buchhave, L. A.; Torres, G.;
Latham, D. W.; Kovács, G.; Bhatti, W.; Csubry, Z.; de Val-Borro,
M.; Penev, K.; Huang, C. X.; Béky, B.; Bieryla, A.; Quinn, S. N.;
Howard, A. W.; Marcy, G. W.; Johnson, J. A.; Isaacson, H.; Fischer,
D. A.; Noyes, R. W.; Falco, E.; Esquerdo, G. A.; Knox, R. P.; Hinz,
P.; Lázár, J.; Papp, I.; Sári, P.
2015AJ....150..197H Altcode: 2015arXiv151008839H
We present the discovery of HAT-P-57b, a P = 2.4653 day transiting
planet around a V=10.465+/- 0.029 mag, {T}<SUB>{{eff</SUB>}}=7500+/-
250 K main sequence A8V star with a projected rotation velocity
of v{sin}i=102.1+/- 1.3 {km} {{{s}}}<SUP>-1</SUP>. We measure the
radius of the planet to be R=1.413+/- 0.054 {R}<SUB>{{J</SUB>}} and,
based on RV observations, place a 95% confidence upper limit on its
mass of M\lt 1.85 {M}<SUB>{{J</SUB>}}. Based on theoretical stellar
evolution models, the host star has a mass and radius of 1.47+/-
0.12 {M}<SUB>⊙ </SUB> and 1.500+/- 0.050 {R}<SUB>⊙ </SUB>,
respectively. Spectroscopic observations made with Keck-I/HIRES during
a partial transit event show the Doppler shadow of HAT-P-57b moving
across the average spectral line profile of HAT-P-57, confirming the
object as a planetary system. We use these observations, together with
analytic formulae that we derive for the line profile distortions,
to determine the projected angle between the spin axis of HAT-P-57 and
the orbital axis of HAT-P-57b. The data permit two possible solutions,
with -16\buildrel{\circ}\over{.} 7\lt λ \lt 3\buildrel{\circ}\over{.}
3 or 27\buildrel{\circ}\over{.} 6\lt λ \lt 57\buildrel{\circ}\over{.}
4 at 95% confidence, and with relative probabilities for the two
modes of 26% and 74%, respectively. Adaptive optics imaging with
MMT/Clio2 reveals an object located 2\buildrel{\prime\prime}\over{.}
7 from HAT-P-57 consisting of two point sources separated in turn
from each other by 0\buildrel{\prime\prime}\over{.} 22. The H-
and {L}<SUP>\prime </SUP>-band magnitudes of the companion stars
are consistent with their being physically associated with HAT-P-57,
in which case they are stars of mass 0.61+/- 0.10 {M}<SUB>⊙ </SUB>
and 0.53+/- 0.08 {M}<SUB>⊙ </SUB>. HAT-P-57 is the most rapidly
rotating star, and only the fourth main sequence A star, known to
host a transiting planet. <P />Based on observations obtained with
the Hungarian-made Automated Telescope Network. Based in part on
observations made with the Keck-I telescope at Mauna Kea Observatory,
HI (Keck time awarded through NASA programs N029Hr, N108Hr, N154Hr
and N130Hr and NOAO programs A289Hr, and A284Hr). Based in part on
observations made with the Nordic Optical Telescope, operated on the
island of La Palma jointly by Denmark, Finland, Iceland, Norway, and
Sweden, in the Spanish Observatorio del Roque de los Muchachos of the
Instituto de Astrofísica de Canarias. Based in part on observations
obtained with the Tillinghast Reflector 1.5 m telescope and the 1.2 m
telescope, both operated by the Smithsonian Astrophysical Observatory
at the Fred Lawrence Whipple Observatory in Arizona.
---------------------------------------------------------
Title: HAT-P-50b, HAT-P-51b, HAT-P-52b, and HAT-P-53b: Three
Transiting Hot Jupiters and a Transiting Hot Saturn From the HATNet
Survey
Authors: Hartman, J. D.; Bhatti, W.; Bakos, G. Á.; Bieryla, A.;
Kovács, G.; Latham, D. W.; Csubry, Z.; de Val-Borro, M.; Penev, K.;
Buchhave, L. A.; Torres, G.; Howard, A. W.; Marcy, G. W.; Johnson,
J. A.; Isaacson, H.; Sato, B.; Boisse, I.; Falco, E.; Everett, M. E.;
Szklenar, T.; Fulton, B. J.; Shporer, A.; Kovács, T.; Hansen, T.;
Béky, B.; Noyes, R. W.; Lázár, J.; Papp, I.; Sári, P.
2015AJ....150..168H Altcode: 2015arXiv150304149H
We report the discovery and characterization of four transiting
exoplanets by the HATNet survey. The planet HAT-P-50b has a mass
of 1.35 {M}<SUB>{{J</SUB>}} and radius of 1.29 {R}<SUB>{{J</SUB>}},
and orbits a bright (V=11.8 mag) M=1.27 {M}<SUB>⊙ </SUB>, R=1.70
{R}<SUB>⊙ </SUB> star every P=3.1220 days. The planet HAT-P-51b has a
mass of 0.31 {M}<SUB>{{J</SUB>}} and radius of 1.29 {R}<SUB>{{J</SUB>}},
and orbits a V=13.4 mag, M=0.98 {M}<SUB>⊙ </SUB>, R=1.04 {R}<SUB>⊙
</SUB> star with a period of P=4.2180 days. The planet HAT-P-52b has a
mass of 0.82 {M}<SUB>{{J</SUB>}} and radius of 1.01 {R}<SUB>{{J</SUB>}},
and orbits a V=14.1 mag, M=0.89 {M}<SUB>⊙ </SUB>, R=0.89 {R}<SUB>⊙
</SUB> star with a period of P=2.7536 days. The planet HAT-P-53b has a
mass of 1.48 {M}<SUB>{{J</SUB>}} and radius of 1.32 {R}<SUB>{{J</SUB>}},
and orbits a V=13.7 mag, M=1.09 {M}<SUB>⊙ </SUB>, R=1.21 {R}<SUB>⊙
</SUB> star with a period of P=1.9616 days. All four planets are
consistent with having circular orbits and have masses and radii
measured to better than 10% precision. The low stellar jitter and
favorable {R}<SUB>p</SUB>/{R}<SUB>\star </SUB> ratio for HAT-P-51
make it a promising target for measuring the Rossiter-McLaughlin
effect for a Saturn-mass planet. <P />Based on observations
obtained with the Hungarian-made Automated Telescope Network. Based
on observations obtained at the W. M. Keck Observatory, which is
operated by the University of California and the California Institute
of Technology. Keck time has been granted by NOAO (A245Hr) and NASA
(N154Hr, N130Hr). Based on data collected at Subaru Telescope, which
is operated by the National Astronomical Observatory of Japan. Based
on observations made with the Nordic Optical Telescope, operated on
the island of La Palma jointly by Denmark, Finland, Iceland, Norway,
Sweden, in the Spanish Observatorio del Roque de los Muchachos of the
Instituto de Astrofísica de Canarias. Based on observations obtained
with the Tillinghast Reflector 1.5 m telescope and the 1.2 m telescope,
both operated by the Smithsonian Astrophysical Observatory at the
Fred Lawrence Whipple Observatory in AZ. Based on radial velocities
obtained with the Sophie spectrograph mounted on the 1.93 m telescope
at Observatoire de Haute-Provence. Based on observations obtained with
facilities of the Las Cumbres Observatory Global Telescope.
---------------------------------------------------------
Title: HATS-7b: A Hot Super Neptune Transiting a Quiet K Dwarf Star
Authors: Bakos, G. Á.; Penev, K.; Bayliss, D.; Hartman, J. D.; Zhou,
G.; Brahm, R.; Mancini, L.; de Val-Borro, M.; Bhatti, W.; Jordán,
A.; Rabus, M.; Espinoza, N.; Csubry, Z.; Howard, A. W.; Fulton, B. J.;
Buchhave, L. A.; Ciceri, S.; Henning, T.; Schmidt, B.; Isaacson, H.;
Noyes, R. W.; Marcy, G. W.; Suc, V.; Howe, A. R.; Burrows, A. S.;
Lázár, J.; Papp, I.; Sári, P.
2015ApJ...813..111B Altcode: 2015arXiv150701024B
We report the discovery by the HATSouth network of HATS-7b, a transiting
Super-Neptune with a mass of 0.120 ± 0.012 {M}<SUB>{{J</SUB>}}, a
radius of {0.563}<SUB>-0.034</SUB><SUP>+0.046</SUP> {R}<SUB>{{J</SUB>}},
and an orbital period of 3.1853 days. The host star is a moderately
bright (V=13.340\+/- 0.010 mag, {K}<SUB>S</SUB>=10.976\+/- 0.026
mag) K dwarf star with a mass of 0.849 ± 0.027 {M}<SUB>⊙ </SUB>,
a radius of {0.815}<SUB>-0.035</SUB><SUP>+0.049</SUP> {R}<SUB>⊙
</SUB>, and a metallicity of [{Fe}/{{H}}] =+0.250\+/- 0.080. The
star is photometrically quiet to within the precision of the HATSouth
measurements, has low RV jitter, and shows no evidence for chromospheric
activity in its spectrum. HATS-7b is the second smallest radius planet
discovered by a wide-field ground-based transit survey, and one of only
a handful of Neptune-size planets with mass and radius determined to 10%
precision. Theoretical modeling of HATS-7b yields a hydrogen-helium
fraction of 18 ± 4% (rock-iron core and H<SUB>2</SUB>-He envelope),
or 9 ± 4% (ice core and H<SUB>2</SUB>-He envelope), i.e., it has
a composition broadly similar to that of Uranus and Neptune, and
very different from that of Saturn, which has 75% of its mass in
H<SUB>2</SUB>-He. Based on a sample of transiting exoplanets with
accurately (<20%) determined parameters, we establish approximate
power-law relations for the envelopes of the mass-density distribution
of exoplanets. HATS-7b, which, together with the recently discovered
HATS-8b, is one of the first two transiting super-Neptunes discovered
in the Southern sky, is a prime target for additional follow-up
observations with Southern hemisphere facilities to characterize
the atmospheres of Super-Neptunes (which we define as objects with
mass greater than that of Neptune, and smaller than halfway between
that of Neptune and Saturn, i.e., 0.054 {M}<SUB>{{J</SUB>}}\lt
{M}<SUB>{{p</SUB>}}\lt 0.18 {M}<SUB>{{J</SUB>}}). <P />The HATSouth
network is operated by a collaboration consisting of Princeton
University (PU), the Max Planck Institute für Astronomie (MPIA), the
Australian National University (ANU), and the Pontificia Universidad
Católica de Chile (PUC). The station at Las Campanas Observatory (LCO)
of the Carnegie Institute is operated by PU in conjunction with PUC,
the station at the High Energy Spectroscopic Survey (H.E.S.S.) site is
operated in conjunction with MPIA, and the station at Siding Spring
Observatory (SSO) is operated jointly with ANU. This paper includes
data gathered with the 10 m Keck-I telescope at Mauna Kea, the MPG 2.2
m and ESO 3.6 m telescopes at the ESO Observatory in La Silla. This
paper uses observations obtained with facilities of the Las Cumbres
Observatory Global Telescope.
---------------------------------------------------------
Title: HAT-P-55b: A Hot Jupiter Transiting a Sun-Like Star
Authors: Juncher, D.; Buchhave, L. A.; Hartman, J. D.; Bakos, G. Á.;
Bieryla, A.; Kovács, T.; Boisse, I.; Latham, D. W.; Kovács, G.;
Bhatti, W.; Csubry, Z.; Penev, K.; de Val-Borro, M.; Falco, E.;
Torres, G.; Noyes, R. W.; Lázár, J.; Papp, I.; Sári, P.
2015PASP..127..851J Altcode: 2015arXiv150603734J
Not Available <P />Based on observations obtained with the
Hungarian-made Automated Telescope Network. Based in part on radial
velocities obtained with the SOPHIE spectrograph mounted on the 1.93-m
telescope at Observatoire de Haute-Provence, France. Based in part on
observations made with the Nordic Optical Telescope, operated on the
island of La Palma jointly by Denmark, Finland, Iceland, Norway, and
Sweden, in the Spanish Observatorio del Roque de los Muchachos of the
Instituto de Astrofísica de Canarias. Based in part on observations
obtained with the Tillinghast Reflector 1.5-m telescope and the 1.2-m
telescope, both operated by the Smithsonian Astrophysical Observatory
at the Fred Lawrence Whipple Observatory in Arizona.
---------------------------------------------------------
Title: HATS-13b and HATS-14b: two transiting hot Jupiters from the
HATSouth survey
Authors: Mancini, L.; Hartman, J. D.; Penev, K.; Bakos, G. Á.;
Brahm, R.; Ciceri, S.; Henning, Th.; Csubry, Z.; Bayliss, D.; Zhou,
G.; Rabus, M.; de Val-Borro, M.; Espinoza, N.; Jordán, A.; Suc, V.;
Bhatti, W.; Schmidt, B.; Sato, B.; Tan, T. G.; Wright, D. J.; Tinney,
C. G.; Addison, B. C.; Noyes, R. W.; Lázár, J.; Papp, I.; Sári, P.
2015A&A...580A..63M Altcode: 2015arXiv150303469M
We report the discovery of HATS-13b and HATS-14b, which are two
hot-Jupiter transiting planets discovered by the HATSouth survey. The
host stars are quite similar to each other (HATS-13: V = 13.9 mag,
M<SUB>⋆</SUB> = 0.96 M<SUB>⊙</SUB>, R<SUB>⋆</SUB> = 0.89
R<SUB>⊙</SUB>, T<SUB>eff</SUB> ≈ 5500 K, [Fe/H] = 0.05; HATS-14:
V = 13.8 mag, M<SUB>⋆</SUB> = 0.97 M<SUB>⊙</SUB>, R<SUB>⋆</SUB>
= 0.93 R<SUB>⊙</SUB>, T<SUB>eff</SUB> ≈ 5350 K, [Fe/H] = 0.33)
and both the planets orbit around them with a period of ~3 days and
a separation of ~0.04 au. However, even though they are irradiated
in a similar way, the physical characteristics of the two planets
are very different. HATS-13b, with a mass of M<SUB>p</SUB> = 0.543
± 0.072 M<SUB>J</SUB> and a radius of R<SUB>p</SUB> = 1.212 ±
0.035 R<SUB>J</SUB>, appears as an inflated planet, while HATS-14b,
having a mass of M<SUB>p</SUB> = 1.071 ± 0.070 M<SUB>J</SUB> and
a radius of R<SUB>p</SUB> = 1.039 ± 0.032 R<SUB>J</SUB>, is only
slightly larger in radius than Jupiter. <P />The HATSouth network
is operated by a collaboration consisting of Princeton University
(PU), the Max Planck Institute für Astronomie (MPIA), the Australian
National University (ANU), and the Pontificia Universidad Católica
de Chile (PUC). The station at Las Campanas Observatory (LCO) of
the Carnegie Institute is operated by PU in conjunction with PUC,
the station at the High Energy Spectroscopic Survey (HESS) site is
operated in conjunction with MPIA, and the station at Siding Spring
Observatory (SSO) is operated jointly with ANU. Based in part on
observations made with (i) the Subaru Telescope, which is operated
by the National Astronomical Observatory of Japan; (ii) the MPG
2.2 m and the (iii) Euler 1.2 m Telescopes at the ESO Observatory
in La Silla; (iv) the CTIO 0.9 m Telescope at the Observatory
of Cerro Tololo.Appendix A is available in electronic form at <A
href="http://www.aanda.org/10.1051/0004-6361/201526069/olm">http://www.aanda.org</A>Full
Table A.1 and RV Tables are only available at the CDS via anonymous ftp
to <A href="http://cdsarc.u-strasbg.fr">http://cdsarc.u-strasbg.fr</A>
(ftp://130.79.128.5) or via <A
href="http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/580/A63">http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/580/A63</A>
---------------------------------------------------------
Title: HATS-8b: A Low-density Transiting Super-Neptune
Authors: Bayliss, D.; Hartman, J. D.; Bakos, G. Á.; Penev, K.; Zhou,
G.; Brahm, R.; Rabus, M.; Jordán, A.; Mancini, L.; de Val-Borro, M.;
Bhatti, W.; Espinoza, N.; Csubry, Z.; Howard, A. W.; Fulton, B. J.;
Buchhave, L. A.; Henning, T.; Schmidt, B.; Ciceri, S.; Noyes, R. W.;
Isaacson, H.; Marcy, G. W.; Suc, V.; Lázár, J.; Papp, I.; Sári, P.
2015AJ....150...49B Altcode: 2015arXiv150601334B
HATS-8b is a low density transiting super-Neptune discovered as part
of the HATSouth project. The planet orbits its solar-like G-dwarf host
(V = 14.03+/- 0.10, {T}<SUB>{eff</SUB>} = 5679+/- 50 K) with a period
of 3.5839 days. HATS-8b is the third lowest-mass transiting exoplanet to
be discovered from a wide-field ground-based search, and with a mass of
0.138+/- 0.019 {M}<SUB>{{J</SUB>}} it is approximately halfway between
the masses of Neptune and Saturn. However, HATS-8b has a radius of
{0.873}<SUB>-0.075</SUB><SUP>+0.123</SUP> {R}<SUB>{{J</SUB>}}, resulting
in a bulk density of just 0.259+/- 0.091 {{g}} {{cm}}<SUP>-3</SUP>. The
metallicity of the host star is super-solar ([{Fe}/{{H}}] = 0.210+/-
0.080), providing evidence against the idea that low-density exoplanets
form from metal-poor environments. The low density and large radius
of HATS-8b results in an atmospheric scale height of almost 1000 km,
and in addition to this there is an excellent reference star of nearly
equal magnitude at just 19″ separation in the sky. These factors
make HATS-8b an exciting target for future atmospheric characterization
studies, particularly for long-slit transmission spectroscopy. <P />The
HATSouth network is operated by a collaboration consisting of Princeton
University (PU), the Max Planck Institute für Astronomie (MPIA), the
Australian National University (ANU), and the Pontificia Universidad
Católica de Chile (PUC). The station at Las Campanas Observatory (LCO)
of the Carnegie Institute is operated by PU in conjunction with PUC,
the station at the High Energy Spectroscopic Survey site is operated in
conjunction with MPIA, and the station at Siding Spring Observatory is
operated jointly with ANU. This paper includes data gathered with the
6.5 m Magellan Telescopes located in LCO, Chile. The work is based
in part on observations made with the MPG 2.2 m Telescope and the
ESO 3.6 m Telescope at the ESO Observatory in La Silla. This paper
uses observations obtained using the facilities of the Las Cumbres
Observatory Global Telescope.
---------------------------------------------------------
Title: A 0.24+0.18 M<SUB>⊙</SUB> double-lined eclipsing binary
from the HATSouth survey
Authors: Zhou, G.; Bayliss, D.; Hartman, J. D.; Rabus, M.; Bakos,
G. Á.; Jordán, A.; Brahm, R.; Penev, K.; Csubry, Z.; Mancini, L.;
Espinoza, N.; de Val-Borro, M.; Bhatti, W.; Ciceri, S.; Henning, T.;
Schmidt, B.; Murphy, S. J.; Butler, R. P.; Arriagada, P.; Shectman,
S.; Crane, J.; Thompson, I.; Suc, V.; Noyes, R. W.
2015MNRAS.451.2263Z Altcode: 2015arXiv150502860Z
We report the discovery and characterization of a new M-dwarf binary,
with component masses and radii of M_1 = 0.244_{-0.003}^{+0.003}
M_{⊙}, R_1 = 0.261_{-0.009}^{+0.006} R_{⊙}, M_2 =
0.179_{-0.001}^{+0.002} M_{⊙}, R_2 = 0.218 _{-0.011}^{+0.007}
R_{⊙}, and orbital period of ∼4.1 d. The M-dwarf binary HATS551-027
(LP 837-20) was identified as an eclipsing binary by the HATSouth
survey, and characterized by a series of high-precision photometric
observations of the eclipse events, and spectroscopic determinations
of the atmospheric parameters and radial velocity orbits. HATS551-027
is one of few systems with both stellar components lying in the fully
convective regime of very low mass stars, and can serve as a test for
stellar interior models. The radius of HATS551-027A is consistent with
models to 1σ, whilst HATS551-027B is inflated by 9 per cent at 2σ
significance. We measure the effective temperatures for the two stellar
components to be T<SUB>eff, 1</SUB> = 3190 ± 100 K and T<SUB>eff,
2</SUB> = 2990 ± 110 K; both are slightly cooler than theoretical
models predict, but consistent with other M-dwarfs of similar masses
that have previously been studied. We also measure significant H α
emission from both components of the binary system, and discuss this
in the context of the correlation between stellar activity and the
discrepancies between the observed and model temperatures.
---------------------------------------------------------
Title: HATS9-b and HATS10-b: Two Compact Hot Jupiters in Field 7 of
the K2 Mission
Authors: Brahm, R.; Jordán, A.; Hartman, J. D.; Bakos, G. Á.;
Bayliss, D.; Penev, K.; Zhou, G.; Ciceri, S.; Rabus, M.; Espinoza,
N.; Mancini, L.; de Val-Borro, M.; Bhatti, W.; Sato, B.; Tan, T. G.;
Csubry, Z.; Buchhave, L.; Henning, T.; Schmidt, B.; Suc, V.; Noyes,
R. W.; Papp, I.; Lázár, J.; Sári, P.
2015AJ....150...33B Altcode: 2015arXiv150300062B
We report the discovery of two transiting extrasolar planets by the
HATSouth survey. HATS-9b orbits an old (10.8 ± 1.5 Gyr) V = 13.3 G
dwarf star with a period P≈ 1.9153 days. The host star has a mass
of 1.03 {M}<SUB>⊙ </SUB>, radius of 1.503 {R}<SUB>⊙ </SUB> , and
effective temperature 5366 ± 70 K. The planetary companion has a mass
of 0.837 {M}<SUB>{{J</SUB>}} and radius of 1.065 {R}<SUB>{{J</SUB>}},
yielding a mean density of 0.85 {{g}} {{cm}}<SUP>-3</SUP>. HATS-10b
orbits a V = 13.1 G dwarf star with a period P≈ 3.3128 days. The
host star has a mass of 1.1 {M}<SUB>⊙ </SUB>, radius of 1.11
{R}<SUB>⊙ </SUB> , and effective temperature 5880 ± 120 K. The
planetary companion has a mass of 0.53 {M}<SUB>{{J</SUB>}} and radius
of 0.97 {R}<SUB>{{J</SUB>}}, yielding a mean density of 0.7 {{g}}
{{cm}}<SUP>-3</SUP>. Both planets are compact in comparison with
planets receiving similar irradiation from their host stars and lie
in the nominal coordinates of Field 7 of K2, but only HATS-9b falls
on working silicon. Future characterization of HATS-9b with the
exquisite photometric precision of the Kepler telescope may provide
measurements of its reflected light signature. <P />The HATSouth network
is operated by a collaboration consisting of Princeton University (PU),
the Max Planck Institute for Astronomy (MPIA), the Australian National
University (ANU), and the Pontificia Universidad Católica de Chile
(PUC). The station at Las Campanas Observatory (LCO) of the Carnegie
Institute is operated by PU in conjunction with PUC, the station at
the High Energy Spectroscopic Survey (H.E.S.S.) site is operated in
conjunction with MPIA, and the station at Siding Spring Observatory
(SSO) is operated jointly with ANU. Based in part on data collected
at Subaru Telescope, which is operated by the National Astronomical
Observatory of Japan. Based in part on observations made with the MPG
2.2 m Telescope at the ESO Observatory in La Silla. This paper uses
observations obtained with facilities of the Las Cumbres Observatory
Global Telescope. Based on observations obtained with the Apache
Point Observatory 3.5 m telescope, which is owned and operated by the
Astrophysical Research Consortium.
---------------------------------------------------------
Title: VizieR Online Data Catalog: HATS-13b and HATS-14b light and
RV curves (Mancini+, 2015)
Authors: Mancini, L.; Hartman, J. D.; Penev, K.; Bakos, G. A.;
Brahm, R.; Ciceri, S.; Henning, T.; Csubry, Z.; Bayliss, D.; Zhou,
G.; Rabus, M.; de Val-Borro, M.; Espinoza, N.; Jordan, A.; Suc, V.;
Bhatti, W.; Schmidt, B.; Sato, B.; Tan, T. G.; Wright, D. J.; Tinney,
C. G.; Addison, B. C.; Noyes, R. W.; Lazar, J.; Papp, I.; Sari, P.
2015yCat..35800063M Altcode:
Radial velocity measurements of HATS-13 and HATS-14 obtained with
various instruments. <P />Light curves of HATS-13 and HATS-14 from
the HATSouth survey; light curves of four transit events of the
extrasolar planet HATS-13b and two transit events of the extrasolar
planet HATS-14b. Three of the datasets were obtained using the PEST
30-cm telescope (filter: R), one with the CTIO 0.9-m telescope (filter:
Sloan z) at the Observatory of Cerro Tololo (Chile), and eight with
the MPG 2.2-m telescope (filter: Sloan g,r,i,z) at the ESO Observatory
in La Silla (Chile). <P />(16 data files).
---------------------------------------------------------
Title: HATS-6b: A Warm Saturn Transiting an Early M Dwarf Star,
and a Set of Empirical Relations for Characterizing K and M Dwarf
Planet Hosts
Authors: Hartman, J. D.; Bayliss, D.; Brahm, R.; Bakos, G. Á.;
Mancini, L.; Jordán, A.; Penev, K.; Rabus, M.; Zhou, G.; Butler,
R. P.; Espinoza, N.; de Val-Borro, M.; Bhatti, W.; Csubry, Z.; Ciceri,
S.; Henning, T.; Schmidt, B.; Arriagada, P.; Shectman, S.; Crane, J.;
Thompson, I.; Suc, V.; Csák, B.; Tan, T. G.; Noyes, R. W.; Lázár,
J.; Papp, I.; Sári, P.
2015AJ....149..166H Altcode: 2014arXiv1408.1758H
We report the discovery by the HATSouth survey of HATS-6b, an
extrasolar planet transiting a V = 15.2 mag, i = 13.7 mag M1V
star with a mass of 0.57 {{M}<SUB>⊙ </SUB>} and a radius of 0.57
{{R}<SUB>⊙ </SUB>}. HATS-6b has a period of P = 3.3253 d, mass of
{{M}<SUB>p</SUB>} = 0.32 {{M}<SUB>J</SUB>}, radius of {{R}<SUB>p</SUB>}
= 1.00 {{R}<SUB>J</SUB>}, and zero-albedo equilibrium temperature of
{{T}<SUB>eq</SUB>} = 712.8 ± 5.1 K. HATS-6 is one of the lowest mass
stars known to host a close-in gas giant planet, and its transits
are among the deepest of any known transiting planet system. We
discuss the follow-up opportunities afforded by this system, noting
that despite the faintness of the host star, it is expected to have
the highest K-band S/N transmission spectrum among known gas giant
planets with {{T}<SUB>eq</SUB>}\lt 750 K. In order to characterize
the star we present a new set of empirical relations between the
density, radius, mass, bolometric magnitude, and V-, J-, H- and
K-band bolometric corrections for main sequence stars with M\lt
0.80 {{M}<SUB>⊙ </SUB>}, or spectral types later than K5. These
relations are calibrated using eclipsing binary components as well as
members of resolved binary systems. We account for intrinsic scatter
in the relations in a self-consistent manner. We show that from the
transit-based stellar density alone it is possible to measure the mass
and radius of a ∼0.6 {{M}<SUB>⊙ </SUB>} star to ∼7 and ∼2%
precision, respectively. Incorporating additional information, such
as the V-K color, or an absolute magnitude, allows the precision to
be improved by up to a factor of two. <P />The HATSouth network is
operated by a collaboration consisting of Princeton University (PU),
the Max Planck Institute für Astronomie (MPIA), the Australian National
University (ANU), and the Pontificia Universidad Católica de Chile
(PUC). The station at Las Campanas Observatory (LCO) of the Carnegie
Institute is operated by PU in conjunction with PUC, the station at
the High Energy Spectroscopic Survey (H.E.S.S.) site is operated in
conjunction with MPIA, and the station at Siding Spring Observatory
(SSO) is operated jointly with ANU. This paper includes data gathered
with the 6.5 m Magellan Telescopes located as Las Campanas Observatory,
Chile. Based in part on observations made with the MPG 2.2 m Telescope
and the ESO 3.6 m Telescope at the ESO Observatory in La Silla. This
paper uses observations obtained with facilities of the Las Cumbres
Observatory Global Telescope.
---------------------------------------------------------
Title: HAT-P-54b: A Hot Jupiter Transiting a 0.6 M<SUB>⊙</SUB>
Star in Field 0 of the K2 Mission
Authors: Bakos, G. Á.; Hartman, J. D.; Bhatti, W.; Bieryla, A.; de
Val-Borro, M.; Latham, D. W.; Buchhave, L. A.; Csubry, Z.; Penev, K.;
Kovács, G.; Béky, B.; Falco, E.; Kovács, T.; Howard, A. W.; Johnson,
J. A.; Isaacson, H.; Marcy, G. W.; Torres, G.; Noyes, R. W.; Berlind,
P.; Calkins, M. L.; Esquerdo, G. A.; Lázár, J.; Papp, I.; Sári, P.
2015AJ....149..149B Altcode: 2014arXiv1404.4417B
We report the discovery of HAT-P-54b, a planet transiting a late K
dwarf star in field 0 of the NASA K2 mission. We combine ground-based
photometric light curves with radial velocity measurements to determine
the physical parameters of the system. HAT-P-54b has a mass of 0.760\+/-
0.032 {{M}<SUB>J</SUB>}, a radius of 0.944 ± 0.028 {{R}<SUB>J</SUB>},
and an orbital period of 3.7998 days. The star has V=13.505\+/- 0.060,
a mass of 0.645\+/- 0.020 {{M}<SUB></SUB>}, a radius of 0.617\+/-
0.013 {{R}<SUB></SUB>}, an effective temperature of {{T}<SUB>eff\star
</SUB>}=4390\+/- 50, and a subsolar metallicity of [Fe/H]=-0.127\+/-
0.080. We also detect a periodic signal with P = 15.6 days and 5.6
mmag amplitude in the light curve, which we interpret as due to the
rotation of the star. HAT-P-54b has a radius that is smaller than
92% of the known transiting planets with masses greater than that of
Saturn, while HAT-P-54 is one of the lowest-mass stars known to host a
hot Jupiter. Follow-up high-precision photometric observations by the
K2 mission promise to make this a well-studied planetary system. <P
/>Based on observations obtained with the Hungarian-made Automated
Telescope Network (HATNet). Based in part on observations obtained at
the W. M. Keck Observatory, using time granted by NASA (N133Hr). Based
in part on observations obtained with the Tillinghast Reflector 1.5 m
telescope and the 1.2 m telescope, both operated by the Smithsonian
Astrophysical Observatory at the Fred Lawrence Whipple Observatory
in Arizona.
---------------------------------------------------------
Title: HATS-4b: A Dense Hot Jupiter Transiting a Super Metal-rich
G star
Authors: Jordán, Andrés; Brahm, Rafael; Bakos, G. Á.; Bayliss,
D.; Penev, K.; Hartman, J. D.; Zhou, G.; Mancini, L.; Mohler-Fischer,
M.; Ciceri, S.; Sato, B.; Csubry, Z.; Rabus, M.; Suc, V.; Espinoza,
N.; Bhatti, W.; de Val-Borro, M.; Buchhave, L.; Csák, B.; Henning,
T.; Schmidt, B.; Tan, T. G.; Noyes, R. W.; Béky, B.; Butler, R. P.;
Shectman, S.; Crane, J.; Thompson, I.; Williams, A.; Martin, R.;
Contreras, C.; Lázár, J.; Papp, I.; Sári, P.
2014AJ....148...29J Altcode: 2014arXiv1402.6546J
We report the discovery by the HATSouth survey of HATS-4b, an extrasolar
planet transiting a V = 13.46 mag G star. HATS-4b has a period of P ≈
2.5167 days, mass of M<SUB>p</SUB> ≈ 1.32 M <SUB>Jup</SUB>, radius of
R<SUB>p</SUB> ≈ 1.02 R <SUB>Jup</SUB>, and density of ρ<SUB> p </SUB>
= 1.55 ± 0.16 g cm<SUP>-3</SUP> ≈1.24 ρ<SUB>Jup</SUB>. The host star
has a mass of 1.00 M <SUB>⊙</SUB>, a radius of 0.92 R <SUB>⊙</SUB>,
and a very high metallicity [Fe/H]=0.43 ± 0.08. HATS-4b is among the
densest known planets with masses between 1 and 2 M <SUB>J</SUB> and is
thus likely to have a significant content of heavy elements of the order
of 75 M <SUB>⊕</SUB>. In this paper we present the data reduction,
radial velocity measurements, and stellar classification techniques
adopted by the HATSouth survey for the CORALIE spectrograph. We
also detail a technique for simultaneously estimating vsin i and
macroturbulence using high resolution spectra. <P />The HATSouth network
is operated by a collaboration consisting of Princeton University (PU),
the Max Planck Institut für Astronomie (MPIA), and the Australian
National University (ANU). The station at Las Campanas Observatory
(LCO) of the Carnegie Institution is operated by PU in conjunction
with collaborators at the Pontificia Universidad Católica de Chile,
the station at the High Energy Spectroscopic Survey site is operated
in conjunction with MPIA, and the station at Siding Spring Observatory
(SSO) is operated jointly with ANU. This paper includes data gathered
with the 6.5 m Magellan Telescopes located at LCO, Chile. Based in
part on data collected at Subaru Telescope, which is operated by
the National Astronomical Observatory of Japan, and on observations
made with the MPG/ESO 2.2 m Telescope at the ESO Observatory in La
Silla. This paper uses observations obtained with facilities of the
Las Cumbres Observatory Global Telescope.
---------------------------------------------------------
Title: HATS-5b: A Transiting Hot Saturn from the HATSouth Survey
Authors: Zhou, G.; Bayliss, D.; Penev, K.; Bakos, G. Á.; Hartman,
J. D.; Jordán, A.; Mancini, L.; Mohler, M.; Csubry, Z.; Ciceri, S.;
Brahm, R.; Rabus, M.; Buchhave, L.; Henning, T.; Suc, V.; Espinoza,
N.; Béky, B.; Noyes, R. W.; Schmidt, B.; Butler, R. P.; Shectman,
S.; Thompson, I.; Crane, J.; Sato, B.; Csák, B.; Lázár, J.; Papp,
I.; Sári, P.; Nikolov, N.
2014AJ....147..144Z Altcode: 2014arXiv1401.1582Z
We report the discovery of HATS-5b, a transiting hot Saturn
orbiting a G-type star, by the HATSouth survey. HATS-5b has a mass
of M<SUB>p</SUB> ≈ 0.24 M <SUB>J</SUB>, radius of R<SUB>p</SUB>
≈ 0.91 R <SUB>J</SUB>, and transits its host star with a period
of P ≈ 4.7634 days. The radius of HATS-5b is consistent with
both theoretical and empirical models. The host star has a V-band
magnitude of 12.6, mass of 0.94 M <SUB>⊙</SUB>, and radius of
0.87 R <SUB>⊙</SUB>. The relatively high scale height of HATS-5b
and the bright, photometrically quiet host star make this planet
a favorable target for future transmission spectroscopy follow-up
observations. We reexamine the correlations in radius, equilibrium
temperature, and metallicity of the close-in gas giants and find
hot Jupiter-mass planets to exhibit the strongest dependence between
radius and equilibrium temperature. We find no significant dependence
in radius and metallicity for the close-in gas giant population. <P
/>The HATSouth network is operated by a collaboration consisting of
Princeton University (PU), the Max Planck Institute für Astronomie
(MPIA), and the Australian National University (ANU). The station at
Las Campanas Observatory (LCO) of the Carnegie Institute is operated
by PU in conjunction with collaborators at the Pontificia Universidad
Católica de Chile (PUC), the station at the High Energy Spectroscopic
Survey (HESS) site is operated in conjunction with MPIA, and the station
at Siding Spring Observatory (SSO) is operated jointly with ANU. This
paper includes data gathered with the 6.5 m Magellan Telescopes located
at Las Campanas Observatory, Chile.
---------------------------------------------------------
Title: HAT-P-44b, HAT-P-45b, and HAT-P-46b: Three Transiting Hot
Jupiters in Possible Multi-planet Systems
Authors: Hartman, J. D.; Bakos, G. Á.; Torres, G.; Kovács, G.;
Johnson, J. A.; Howard, A. W.; Marcy, G. W.; Latham, D. W.; Bieryla,
A.; Buchhave, L. A.; Bhatti, W.; Béky, B.; Csubry, Z.; Penev, K.; de
Val-Borro, M.; Noyes, R. W.; Fischer, D. A.; Esquerdo, G. A.; Everett,
M.; Szklenár, T.; Zhou, G.; Bayliss, D.; Shporer, A.; Fulton, B. J.;
Sanchis-Ojeda, R.; Falco, E.; Lázár, J.; Papp, I.; Sári, P.
2014AJ....147..128H Altcode: 2013arXiv1308.2937H
We report the discovery by the HATNet survey of three new transiting
extrasolar planets orbiting moderately bright (V = 13.2, 12.8, and
11.9) stars. The planets have orbital periods of 4.3012, 3.1290,
and 4.4631 days, masses of 0.35, 0.89, and 0.49 M <SUB>J</SUB>, and
radii of 1.24, 1.43, and 1.28 R <SUB>J</SUB>. The stellar hosts have
masses of 0.94, 1.26, and 1.28 M <SUB>⊙</SUB>. Each system shows
significant systematic variations in its residual radial velocities,
indicating the possible presence of additional components. Based on
its Bayesian evidence, the preferred model for HAT-P-44 consists of
two planets, including the transiting component, with the outer planet
having a period of 872 days, eccentricity of 0.494 ± 0.081, and a
minimum mass of 4.0 M <SUB>J</SUB>. Due to aliasing we cannot rule
out alternative solutions for the outer planet having a period of 220
days or 438 days. For HAT-P-45, at present there is not enough data to
justify the additional free parameters included in a multi-planet model;
in this case a single-planet solution is preferred, but the required
jitter of 22.5 ± 6.3 m s<SUP>-1</SUP> is relatively high for a star of
this type. For HAT-P-46 the preferred solution includes a second planet
having a period of 78 days and a minimum mass of 2.0 M <SUB>J</SUB>,
however the preference for this model over a single-planet model is not
very strong. While substantial uncertainties remain as to the presence
and/or properties of the outer planetary companions in these systems,
the inner transiting planets are well characterized with measured
properties that are fairly robust against changes in the assumed models
for the outer planets. Continued radial velocity monitoring is necessary
to fully characterize these three planetary systems, the properties of
which may have important implications for understanding the formation
of hot Jupiters. <P />Based in part on observations obtained at
the W. M. Keck Observatory, which is operated by the University of
California and the California Institute of Technology. Keck time has
been granted by NOAO (A284Hr) and NASA (N154Hr, N108Hr).
---------------------------------------------------------
Title: The Discovery of the Solar 5-minute Oscillations and the
Supergranulation
Authors: Noyes, Robert W.
2014AAS...22420301N Altcode:
The summer of 1960 marked the discovery, from the Mt. Wilson 60-foot
solar tower telescope, of both the solar 5-minute oscillation and the
supergranulation. We review the history of how, starting in 1955, Robert
Leighton at Caltech carried out studies of the sun at high resolution
from the Mt. Wilson 60-foot solar tower telescope. In 1958 he developed
a method to map the spatial distribution of solar magnetic fields by
photographically subtracting pairs of spectroheliograph images differing
only in the sign of their Zeeman-effect sensitivity to longitudinal
magnetic fields, and showed for the first time that photospheric
magnetic fields trace out the heating of the overlying chromosphere
as revealed by the pattern of the Ca II emission network. Leighton
then developed a variation of the technique to measure velocity fields
and their spatial and temporal variation, and in the summer of 1960 he
and his students made a series of discoveries that changed the face of
solar physics. One of these was the discovery that the velocity field
of the sun exhibits a very strong quasi-periodic vertical oscillation
with a period of about 5 minutes; this discovery represents the dawn
of helioseismology, which over the past 50 years has grown to embrace
research lines in solar and stellar astrophysics that were unimaginable
at the time. A parallel discovery made by Leighton and his students
during that same summer was the "large cells", later to be termed
the supergranulation, which show a complex pattern of flow fields,
evidently produced bylarge-scale convective motions that are still
not well-understood, but which create the magnetic network and hence
the pattern of heating in the overlying chromosphere.
---------------------------------------------------------
Title: Stellar Rotation-Planetary Orbit Period Commensurability in
the HAT-P-11 System
Authors: Béky, Bence; Holman, Matthew J.; Kipping, David M.; Noyes,
Robert W.
2014ApJ...788....1B Altcode: 2014arXiv1403.7526B
A number of planet host stars have been observed to rotate with a
period equal to an integer multiple of the orbital period of their
close planet. We expand this list by analyzing Kepler data of HAT-P-11
and finding a period ratio of 6:1. In particular, we present evidence
for a long-lived spot on the stellar surface that is eclipsed by the
planet in the same position four times, every sixth transit. We also
identify minima in the out-of-transit light curve and confirm that their
phase with respect to the stellar rotation is mostly stationary for
the 48 month time frame of the observations, confirming the proposed
rotation period. For comparison, we apply our methods to Kepler-17 and
confirm the findings of Bonomo & Lanza that the period ratio is
not exactly 8:1 in that system. Finally, we provide a hypothesis on how
interactions between a star and its planet could possibly result in an
observed commensurability for systems where the stellar differential
rotation profile happens to include a period at some latitude that is
commensurable to the planetary orbit.
---------------------------------------------------------
Title: HAT-P-49b: A 1.7 M <SUB>J</SUB> Planet Transiting a Bright
1.5 M <SUB>⊙</SUB> F-star
Authors: Bieryla, A.; Hartman, J. D.; Bakos, G. Á.; Bhatti, W.;
Kovács, G.; Boisse, I.; Latham, D. W.; Buchhave, L. A.; Csubry,
Z.; Penev, K.; de Val-Borro, M.; Béky, B.; Falco, E.; Torres, G.;
Noyes, R. W.; Berlind, P.; Calkins, M. C.; Esquerdo, G. A.; Lázár,
J.; Papp, I.; Sári, P.
2014AJ....147...84B Altcode: 2014arXiv1401.5460B
We report the discovery of the transiting extrasolar planet
HAT-P-49b. The planet transits the bright (V = 10.3) slightly evolved
F-star HD 340099 with a mass of 1.54 M <SUB>⊙</SUB> and a radius of
1.83 R <SUB>⊙</SUB>. HAT-P-49b is orbiting one of the 25 brightest
stars to host a transiting planet which makes this a favorable candidate
for detailed follow-up. This system is an especially strong target for
Rossiter-McLaughlin follow-up due to the host star's fast rotation, 16
km s<SUP>-1</SUP>. The planetary companion has a period of 2.6915 days,
mass of 1.73 M <SUB>J</SUB>, and radius of 1.41 R <SUB>J</SUB>. The
planetary characteristics are consistent with that of a classical hot
Jupiter but we note that this is the fourth most massive star to host
a transiting planet with both M<SUB>p</SUB> and R<SUB>p</SUB> well
determined. <P />Based on observations obtained with the Hungarian-made
Automated Telescope Network. Based in part on observations obtained
with the Tillinghast Reflector 1.5 m telescope and the 1.2 m telescope,
both operated by the Smithsonian Astrophysical Observatory at the
Fred Lawrence Whipple Observatory in Arizona. Based in part on radial
velocities obtained with the SOPHIE spectrograph mounted on the 1.93
m telescope at Observatoire de Haute Provence, France.
---------------------------------------------------------
Title: Robert Leighton and the Dawn of Helioseismology
Authors: Noyes, R. W.
2013ASPC..478....5N Altcode:
We review the events leading up to and including the discovery in
1960 by Robert Leighton of the solar 5-minute oscillation, which may
be characterized as the dawn of helioseismology.
---------------------------------------------------------
Title: HATS-3b: An Inflated Hot Jupiter Transiting an F-type Star
Authors: Bayliss, D.; Zhou, G.; Penev, K.; Bakos, G. Á.; Hartman,
J. D.; Jordán, A.; Mancini, L.; Mohler-Fischer, M.; Suc, V.; Rabus,
M.; Béky, B.; Csubry, Z.; Buchhave, L.; Henning, T.; Nikolov, N.;
Csák, B.; Brahm, R.; Espinoza, N.; Noyes, R. W.; Schmidt, B.; Conroy,
P.; Wright, D. J.; Tinney, C. G.; Addison, B. C.; Sackett, P. D.;
Sasselov, D. D.; Lázár, J.; Papp, I.; Sári, P.
2013AJ....146..113B Altcode: 2013arXiv1306.0624B
We report the discovery by the HATSouth survey of HATS-3b, a transiting
extrasolar planet orbiting a V = 12.4 F dwarf star. HATS-3b has a
period of P = 3.5479 days, mass of M<SUB>p</SUB> = 1.07 M <SUB>J</SUB>,
and radius of R<SUB>p</SUB> = 1.38 R <SUB>J</SUB>. Given the radius
of the planet, the brightness of the host star, and the stellar
rotational velocity (vsin i = 9.0 km s<SUP>-1</SUP>), this system
will make an interesting target for future observations to measure the
Rossiter-McLaughlin effect and determine its spin-orbit alignment. We
detail the low-/medium-resolution reconnaissance spectroscopy that we
are now using to deal with large numbers of transiting planet candidates
produced by the HATSouth survey. We show that this important step in
discovering planets produces log g and T <SUB>eff</SUB> parameters
at a precision suitable for efficient candidate vetting, as well
as efficiently identifying stellar mass eclipsing binaries with
radial velocity semi-amplitudes as low as 1 km s<SUP>-1</SUP>. <P
/>The HATSouth network is operated by a collaboration consisting of
Princeton University (PU), the Max Planck Institute für Astronomie
(MPIA), and the Australian National University (ANU). The station at
Las Campanas Observatory (LCO) of the Carnegie Institute is operated
by PU in conjunction with collaborators at the Pontificia Universidad
Católica de Chile (PUC), the station at the High Energy Spectroscopic
Survey (HESS) site is operated in conjunction with MPIA, and the
station at Siding Spring Observatory (SSO) is operated jointly with ANU.
---------------------------------------------------------
Title: HAT-P-42b and HAT-P-43b. Two inflated transiting hot Jupiters
from the HATNet Survey
Authors: Boisse, I.; Hartman, J. D.; Bakos, G. Á.; Penev, K.; Csubry,
Z.; Béky, B.; Latham, D. W.; Bieryla, A.; Torres, G.; Kovács, G.;
Buchhave, L. A.; Hansen, T.; Everett, M.; Esquerdo, G. A.; Szklenár,
T.; Falco, E.; Shporer, A.; Fulton, B. J.; Noyes, R. W.; Stefanik,
R. P.; Lázár, J.; Papp, I.; Sári, P.
2013A&A...558A..86B Altcode: 2012arXiv1212.6448B
<BR /> Aims: We announce the discovery of two new transiting planets,
and provide their accurate initial characterization. <BR /> Methods:
First identified from the HATNet wide-field photometric survey, these
candidate transiting planets were then followed-up with a variety
of photometric observations. Determining the planetary nature of
the objects and characterizing the parameters of the systems were
mainly done with the SOPHIE spectrograph at the 1.93 m telescope at
OHP and the TRES spectrograph at the 1.5 m telescope at FLWO. <BR />
Results: HAT-P-42b and HAT-P-43b are typical hot Jupiters on circular
orbits around early-G/late-F main sequence host stars, with periods of
4.641878 ± 0.000032 and 3.332687 ± 0.000015 days, masses of 1.044 ±
0.083 and 0.662 ± 0.060 M<SUB>J</SUB>, and radii of 1.280 ± 0.153 and
1.28<SUP>+0.062</SUP><SUB>-0.033</SUB>R<SUB>J</SUB>, respectively. These
discoveries increase the sample of planets with measured mean densities,
which are needed to constrain theories of planetary interiors and
atmospheres. Moreover, their hosts are relatively bright (V < 13.5),
which facilitates further follow-up studies. <P />Full Table 2 is
only available in electronic form at the CDS via anonymous ftp to <A
href="http://cdsarc.u-strasbg.fr">http://cdsarc.u-strasbg.fr</A>
(ftp://130.79.128.5) or via <A
href="http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/558/A86">http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/558/A86</A>The
photometric/spectroscopic data presented in this paper are based in
part on observations carried out by the Hungarian-made Automated
Telescope Network, using telescopes operated at the Fred Lawrence
Whipple Observatory (FLWO) of the Smithsonian Astrophysical Observatory
(SAO), and at the Submillimeter Array (SMA) of SAO, by the Tillinghast
Reflector 1.5 m telescope and the 1.2 m telescope, both operated by SAO
at FLWO, by the SOPHIE spectrograph mounted on the 1.93 m telescope
at Observatoire de Haute Provence, France (runs DDT-Dec. 2011), by
the Nordic Optical Telescope, operated on the island of La Palma
jointly by Denmark, Finland, Iceland, Norway, and Sweden, in the
Spanish Observatorio del Roque de los Muchachos of the Instituto de
Astrofisica de Canarias, and by the facilities of the Las Cumbres
Observatory Global Telescope.
---------------------------------------------------------
Title: HATS-2b: A transiting extrasolar planet orbiting a K-type
star showing starspot activity
Authors: Mohler-Fischer, M.; Mancini, L.; Hartman, J. D.; Bakos,
G. Á.; Penev, K.; Bayliss, D.; Jordán, A.; Csubry, Z.; Zhou, G.;
Rabus, M.; Nikolov, N.; Brahm, R.; Espinoza, N.; Buchhave, L. A.;
Béky, B.; Suc, V.; Csák, B.; Henning, T.; Wright, D. J.; Tinney,
C. G.; Addison, B. C.; Schmidt, B.; Noyes, R. W.; Papp, I.; Lázár,
J.; Sári, P.; Conroy, P.
2013A&A...558A..55M Altcode: 2013arXiv1304.2140M
We report the discovery of HATS-2b, the second transiting extrasolar
planet detected by the HATSouth survey. HATS-2b is moving on a circular
orbit around a V = 13.6 mag, K-type dwarf star (GSC 6665-00236),
at a separation of 0.0230 ± 0.0003 AU and with a period of 1.3541
days. The planetary parameters have been robustly determined using a
simultaneous fit of the HATSouth, MPG/ESO 2.2 m/GROND, Faulkes Telescope
South/Spectral transit photometry, and MPG/ESO 2.2 m/FEROS, Euler 1.2
m/CORALIE, AAT 3.9 m/CYCLOPS radial-velocity measurements. HATS-2b
has a mass of 1.37 ± 0.16 M<SUB>J</SUB>, a radius of 1.14 ± 0.03
R<SUB>J</SUB>, and an equilibrium temperature of 1567 ± 30 K. The
host star has a mass of 0.88 ± 0.04 M<SUB>⊙</SUB> and a radius
of 0.89 ± 0.02 R<SUB>⊙</SUB>, and it shows starspot activity. We
characterized the stellar activity by analyzing two photometric
follow-up transit light curves taken with the GROND instrument, both
obtained simultaneously in four optical bands (covering the wavelength
range of 3860-9520 Å). The two light curves contain anomalies
compatible with starspots on the photosphere of the host star along
the same transit chord. <P />Tables of the individual photometric
measurements are only available at the CDS via anonymous ftp to <A
href="http://cdsarc.u-strasbg.fr">http://cdsarc.u-strasbg.fr</A>
(ftp://130.79.128.5) or via <A
href="http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/558/A55">http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/558/A55</A>
---------------------------------------------------------
Title: VizieR Online Data Catalog: HATS-2b griz light curves
(Mohler-Fischer+, 2013)
Authors: Mohler-Fischer, M.; Mancini, L.; Hartman, J. D.; Bakos,
G. A.; Penev, K.; Bayliss, D.; Jordan, A.; Csubry, Z.; Zhou, G.;
Rabus, M.; Nikolov, N.; Brahm, R.; Espinoza, N.; Buchhave, L. A.;
Beky, B.; Suc, V.; Csak, B.; Henning, T.; Wright, D. J.; Tinney,
C. G.; Addison, B. C.; Schmidt, B.; Noyes, R. W.; Papp, I.; Lazar,
J.; Sari, P.; Conroy, P.
2013yCat..35580055M Altcode: 2013yCat..35589055M
Files contain the data used to plot the lightcurves in Fig. 2, 6 and 7
in the paper. The data were obtained using two different instruments:
GROND mounted on the MPG/ESO 2.2 telescope in La Silla Observatory,
and the Spectral imaging camera, mounted at 2.0m FTS at Siding Spring
Observatory. <P />(9 data files).
---------------------------------------------------------
Title: Relative Photometry of HAT-P-1b Occultations
Authors: Béky, Bence; Holman, Matthew J.; Gilliland, Ronald L.; Bakos,
Gáspár Á.; Winn, Joshua N.; Noyes, Robert W.; Sasselov, Dimitar D.
2013AJ....145..166B Altcode: 2013arXiv1305.3281B
We present Hubble Space Telescope (HST) Space Telescope Imaging
Spectrograph observations of two occultations of the transiting
exoplanet HAT-P-1b. By measuring the planet to star flux ratio near
opposition, we constrain the geometric albedo of the planet, which is
strongly linked to its atmospheric temperature gradient. An advantage of
HAT-P-1 as a target is its binary companion ADS 16402 A, which provides
an excellent photometric reference, simplifying the usual steps in
removing instrumental artifacts from HST time-series photometry. We
find that without this reference star, we would need to detrend the
lightcurve with the time of the exposures as well as the first three
powers of HST orbital phase, and this would introduce a strong bias
in the results for the albedo. However, with this reference star,
we only need to detrend the data with the time of the exposures to
achieve the same per-point scatter, therefore we can avoid most of the
bias associated with detrending. Our final result is a 2σ upper limit
of 0.64 for the geometric albedo of HAT-P-1b between 577 and 947 nm.
---------------------------------------------------------
Title: Comprehensive time series analysis of the transiting extrasolar
planet WASP-33b
Authors: Kovács, G.; Kovács, T.; Hartman, J. D.; Bakos, G. Á.;
Bieryla, A.; Latham, D.; Noyes, R. W.; Regály, Zs.; Esquerdo, G. A.
2013A&A...553A..44K Altcode: 2012arXiv1205.5060K
Context. HD 15082 (WASP-33) is the hottest and fastest rotating star
known to harbor a transiting extrasolar planet (WASP-33b). The lack of
high precision radial velocity (RV) data stresses the need for precise
light curve analysis and gathering further RV data. <BR /> Aims: By
using available photometric and RV data, we perform a blend analysis,
compute more accurate system parameters, confine the planetary mass,
and, attempt to cast light on the observed transit anomalies. <BR />
Methods: We combined the original HATNet observations and various
followup data to jointly analyze the signal content and extract the
transit component and used our RV data to aid the global parameter
determination. <BR /> Results: The blend analysis of the combination of
multicolor light curves yields the first independent confirmation of
the planetary nature of WASP-33b. We clearly identify three frequency
components in the 15-21 d<SUP>-1</SUP> regime with amplitudes 7-5
mmag. These frequencies correspond to the δ Scuti-type pulsation
of the host star. None of these pulsation frequencies or their
low-order linear combinations are in close resonance with the orbital
frequency. We show that these pulsation components explain some but
not all of the observed transit anomalies. The grand-averaged transit
light curve shows that there is a ~1.5 mmag brightening shortly after
the planet passes the mid-transit phase. Although the duration and
amplitude of this brightening varies, it is visible even through the
direct inspections of the individual transit events (some 40-60% of the
followup light curves show this phenomenon). We suggest that the most
likely explanation of this feature is the presence of a well-populated
spot belt which is highly inclined to the orbital plane. This
geometry is consistent with the inference from the spectroscopic
anomalies. Finally, we constrain the planetary mass to M<SUB>p</SUB> =
3.27 ± 0.73 M<SUB>J</SUB> by using our RV data collected by the TRES
spectrograph. <P />Appendix A is available in electronic form at <A
href="http://www.aanda.org">http://www.aanda.org</A>Photometric time
series and lightcurves are only available at the CDS via anonymous ftp
to <A href="http://cdsarc.u-strasbg.fr">cdsarc.u-strasbg.fr</A>
(ftp://130.79.128.5) or via <A
href="http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/553/A44">http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/553/A44</A>
---------------------------------------------------------
Title: VizieR Online Data Catalog: HAT-P-42b and HAT-P-43b ri light
curves (Boisse+, 2013)
Authors: Boisse, I.; Hartman, J.; Bakos, G.; Penev, K.; Csubry, Z.;
Beky, B.; Latham, D.; Bieryla, A.; Torres, G.; Kovacs, G.; Buchhave,
L.; Hansen, T.; Everett, M.; Esquerdo, G.; Szklenar, T.; Falco, E.;
Shporer, A.; Fulton, B.; Noyes, R.; Stefanik, R.; Lazar, J.; Papp,
I.; Sari, P.
2013yCat..35580086B Altcode: 2013yCat..35589086B
High precision differential photometry of HAT-P-42 and of HAT-P-43. <P
/>(1 data file).
---------------------------------------------------------
Title: VizieR Online Data Catalog: Transiting extrasolar planet
WASP-33b (Kovacs+, 2013)
Authors: Kovacs, G.; Kovacs, T.; Hartman, J. D.; Bakos, G. A.; Bieryla,
A.; Latham, D.; Noyes, R. W.; Regaly, Zs.; Esquerdo, G. A.
2013yCat..35530044K Altcode: 2013yCat..35539044K
Light curves (LCs) used in the time series analysis of WASP-33 are
presented. <P />All LCs are on magnitude scale. The material constitutes
of: (1) the TFA-filtered/reconstructed (see Kovacs, Bakos & Noyes,
2005MNRAS.356..557K) HATNet LC in approximate Ic (Cousins) color;
(2) LCs given in Table 1: except for the FLWO data (lc02) all LCs
are corrected for linear trends, shifted to zero magnitude at the
out-of-transit level. Time is in Heliocentric Julian Date, colors are
given in Table 1. (3) Grand-averaged LC, as shown in Fig. 10 of the
paper. <P />(4 data files).
---------------------------------------------------------
Title: HATSouth: A Global Network of Fully Automated Identical
Wide-Field Telescopes
Authors: Bakos, G. Á.; Csubry, Z.; Penev, K.; Bayliss, D.; Jordán,
A.; Afonso, C.; Hartman, J. D.; Henning, T.; Kovács, G.; Noyes,
R. W.; Béky, B.; Suc, V.; Csák, B.; Rabus, M.; Lázár, J.; Papp,
I.; Sári, P.; Conroy, P.; Zhou, G.; Sackett, P. D.; Schmidt, B.;
Mancini, L.; Sasselov, D. D.; Ueltzhoeffer, K.
2013PASP..125..154B Altcode: 2012arXiv1206.1391B
HATSouth is the world’s first network of automated and homogeneous
telescopes that is capable of year-round 24 hr monitoring of positions
over an entire hemisphere of the sky. The primary scientific goal
of the network is to discover and characterize a large number of
transiting extrasolar planets, reaching out to long periods and down to
small planetary radii. HATSouth achieves this by monitoring extended
areas on the sky, deriving high precision light curves for a large
number of stars, searching for the signature of planetary transits,
and confirming planetary candidates with larger telescopes. HATSouth
employs six telescope units spread over three prime locations with
large longitude separation in the southern hemisphere (Las Campanas
Observatory, Chile; HESS site, Namibia; Siding Spring Observatory,
Australia). Each of the HATSouth units holds four 0.18 m diameter
f/2.8 focal ratio telescope tubes on a common mount producing an
8.2° × 8.2° field of view on the sky, imaged using four 4 K × 4
K CCD cameras and Sloan r filters, to give a pixel scale of 3.7″
pixel<SUP>-1</SUP>. The HATSouth network is capable of continuously
monitoring 128 square arc degrees at celestial positions moderately
close to the anti-solar direction. We present the technical details
of the network, summarize operations, and present detailed weather
statistics for the three sites. Robust operations have meant that on
average each of the six HATSouth units has conducted observations on
∼500 nights over a 2 years time period, yielding a total of more than
1 million science frames at a 4 minute integration time and observing
∼10.65 hr day<SUP>-1</SUP> on average. We describe the scheme of our
data transfer and reduction from raw pixel images to trend-filtered
light curves and transiting planet candidates. Photometric precision
reaches ∼6 mmag at 4 minute cadence for the brightest non-saturated
stars at r ≈ 10.5. We present detailed transit recovery simulations
to determine the expected yield of transiting planets from HATSouth. We
highlight the advantages of networked operations, namely, a threefold
increase in the expected number of detected planets, as compared to all
telescopes operating from the same site. <P />The HATSouth hardware
was acquired by NSF MRI NSF/AST-0723074 and is owned by Princeton
University. The HATSouth network is operated by a collaboration
consisting of Princeton University (PU), the Max Planck Institute for
Astronomy (MPIA), and the Australian National University (ANU). The
station at Las Campanas Observatory (LCO), of the Carnegie Institution
for Science, is operated by PU in conjunction with collaborators
at the Pontificia Universidad Católica de Chile (PUC); the station
at the High Energy Spectroscopic Survey (HESS) site is operated in
conjunction with MPIA; and the station at Siding Springs Observatory
(SSO) is operated jointly with ANU.
---------------------------------------------------------
Title: HATS-1b: The First Transiting Planet Discovered by the
HATSouth Survey
Authors: Penev, K.; Bakos, G. Á.; Bayliss, D.; Jordán, A.; Mohler,
M.; Zhou, G.; Suc, V.; Rabus, M.; Hartman, J. D.; Mancini, L.; Béky,
B.; Csubry, Z.; Buchhave, L.; Henning, T.; Nikolov, N.; Csák, B.;
Brahm, R.; Espinoza, N.; Conroy, P.; Noyes, R. W.; Sasselov, D. D.;
Schmidt, B.; Wright, D. J.; Tinney, C. G.; Addison, B. C.; Lázár,
J.; Papp, I.; Sári, P.
2013AJ....145....5P Altcode: 2012arXiv1206.1524P
We report the discovery of HATS-1b, a transiting extrasolar planet
orbiting the moderately bright V = 12.05 G dwarf star GSC 6652-00186,
and the first planet discovered by HATSouth, a global network of
autonomous wide-field telescopes. HATS-1b has a period of P ≈ 3.4465
days, mass of M<SUB>p</SUB> ≈ 1.86 M <SUB>J</SUB>, and radius of
R<SUB>p</SUB> ≈ 1.30 R <SUB>J</SUB>. The host star has a mass of 0.99
M <SUB>⊙</SUB> and radius of 1.04 R <SUB>⊙</SUB>. The discovery
light curve of HATS-1b has near-continuous coverage over several
multi-day timespans, demonstrating the power of using a global network
of telescopes to discover transiting planets. <P />The HATSouth network
is operated by a collaboration consisting of Princeton University (PU),
the Max Planck Institute für Astronomie (MPIA), and the Australian
National University (ANU). The station at Las Campanas Observatory
(LCO) of the Carnegie Institute, is operated by PU in conjunction
with collaborators at the Pontificia Universidad Católica de Chile
(PUC), the station at the High Energy Spectroscopic Survey (HESS)
site is operated in conjunction with MPIA, and the station at Siding
Spring Observatory (SSO) is operated jointly with ANU. Based in part
on observations made with the Nordic Optical Telescope, operated
on the island of La Palma in the Spanish Observatorio del Roque de
los Muchachos of the Instituto de Astrofisica de Canarias. Based
on observations made with the MPG/ESO 2.2 m Telescope at the
ESO Observatory in La Silla. FEROS ID programmes: P087.A-9014(A),
P088.A-9008(A), P089.A-9008(A), P087.C-0508(A). GROND ID programme:
089.A-9006(A). This paper uses observations obtained with facilities
of the Las Cumbres Observatory Global Telescope.
---------------------------------------------------------
Title: HAT-P-39b-HAT-P-41b: Three Highly Inflated Transiting Hot
Jupiters
Authors: Hartman, J. D.; Bakos, G. Á.; Béky, B.; Torres, G.; Latham,
D. W.; Csubry, Z.; Penev, K.; Shporer, A.; Fulton, B. J.; Buchhave,
L. A.; Johnson, J. A.; Howard, A. W.; Marcy, G. W.; Fischer, D. A.;
Kovács, G.; Noyes, R. W.; Esquerdo, G. A.; Everett, M.; Szklenár,
T.; Quinn, S. N.; Bieryla, A.; Knox, R. P.; Hinz, P.; Sasselov, D. D.;
Fűrész, G.; Stefanik, R. P.; Lázár, J.; Papp, I.; Sári, P.
2012AJ....144..139H Altcode: 2012arXiv1207.3344H
We report the discovery of three new transiting extrasolar planets
orbiting moderately bright (V = 11.1, 11.7, and 12.4) F stars. The
planets HAT-P-39b through HAT-P-41b have periods of P = 3.5439 days,
4.4572 days, and 2.6940 days, masses of 0.60 M <SUB>J</SUB>, 0.62 M
<SUB>J</SUB>, and 0.80 M <SUB>J</SUB>, and radii of 1.57 R <SUB>J</SUB>,
1.73 R <SUB>J</SUB>, and 1.68 R <SUB>J</SUB>, respectively. They orbit
stars with masses of 1.40 M <SUB>⊙</SUB>, 1.51 M <SUB>⊙</SUB>, and
1.51 M <SUB>⊙</SUB>, respectively. The three planets are members of an
emerging population of highly inflated Jupiters with 0.4 M <SUB>J</SUB>
< M < 1.5 M <SUB>J</SUB> and R > 1.5 R <SUB>J</SUB>. <P
/>Based in part on observations obtained at the W. M. Keck Observatory,
which is operated by the University of California and the California
Institute of Technology. Keck time has been granted by NOAO (A201Hr,
A289Hr, and A284Hr), NASA (N049Hr, N018Hr, N167Hr, N029Hr, N108Hr, and
N154Hr), and the NOAO Gemini/Keck time-exchange program (G329Hr). Based
in part on observations made with the Nordic Optical Telescope,
operated on the island of La Palma jointly by Denmark, Finland,
Iceland, Norway, and Sweden, in the Spanish Observatorio del Roque
de los Muchachos of the Instituto de Astrofisica de Canarias. Based
in part on observations obtained with facilities of the Las Cumbres
Observatory Global Telescope. Observations reported here were obtained
at the MMT Observatory, a joint facility of the Smithsonian Institution
and the University of Arizona.
---------------------------------------------------------
Title: HAT-P-38b: A Saturn-Mass Planet Transiting a Late G Star
Authors: Sato, Bun'ei; Hartman, Joel D.; Bakos, Gáspár Á.; Béky,
Bence; Torres, Guillermo; Latham, David W.; Kovács, Géza; Csubry,
Zoltán; Penev, Kaloyan; Noyes, Robert W.; Buchhave, Lars A.; Quinn,
Samuel N.; Everett, Mark; Esquerdo, Gilbert A.; Fischer, Debra A.;
Howard, Andrew W.; Johnson, John A.; Marcy, Geoff W.; Sasselov, Dimitar
D.; Szklenár, Tamás; Lázár, József; Papp, István; Sári, Pál
2012PASJ...64...97S Altcode: 2012arXiv1201.5075S
We report on the discovery of HAT-P-38b, a Saturn-mass exoplanet,
transiting the V = 12.56 dwarf star GSC 2314-00559 on a P = 4.6404 d
circular orbit. The host star is a 0.89 M<SUB>⊙</SUB> late G dwarf,
with solar metallicity and a radius of 0.92 R<SUB>⊙</SUB>. The
planetary companion has a mass of 0.27 M<SUB>J</SUB> and a radius of
0.82 R<SUB>J</SUB>. HAT-P-38b is one of the planets the mass and radius
of which have ever been discovered to be the closest to those of Saturn.
---------------------------------------------------------
Title: First Results of the Konkoly Blazhko Survey II
Authors: Sódor, Á.; Jurcsik, J.; Molnár, L.; Szeidl, B.; Hurta,
Zs.; Bakos, G. Á.; Hartman, J.; Béky, B.; Noyes, R. W.; Sasselov,
D.; Mazeh, T.; Bartus, J.; Belucz, B.; Hajdu, G.; Kovári, Zs.; Kun,
E.; Nagy, I.; Posztobányi, K.; Smitola, P.; Vida, K.
2012ASPC..462..228S Altcode: 2012arXiv1201.5474S
The two parts of the Konkoly Blazhko Survey (KBS I and II) are
introduced. The most important preliminary findings of the second part
are presented in comparison to the results of the first part. Two
interesting cases of very strong modulation from the KBS II are
also shown.
---------------------------------------------------------
Title: HAT-P-34b-HAT-P-37b: Four Transiting Planets More Massive
than Jupiter Orbiting Moderately Bright Stars
Authors: Bakos, G. Á.; Hartman, J. D.; Torres, G.; Béky, B.;
Latham, D. W.; Buchhave, L. A.; Csubry, Z.; Kovács, G.; Bieryla, A.;
Quinn, S.; Szklenár, T.; Esquerdo, G. A.; Shporer, A.; Noyes, R. W.;
Fischer, D. A.; Johnson, J. A.; Howard, A. W.; Marcy, G. W.; Sato,
B.; Penev, K.; Everett, M.; Sasselov, D. D.; Fűrész, G.; Stefanik,
R. P.; Lázár, J.; Papp, I.; Sári, P.
2012AJ....144...19B Altcode: 2012arXiv1201.0659B
We report the discovery of four transiting extrasolar planets
(HAT-P-34b-HAT-P-37b) with masses ranging from 1.05 to 3.33 M
<SUB>J</SUB> and periods from 1.33 to 5.45 days. These planets
orbit relatively bright F and G dwarf stars (from V = 10.16 to V =
13.2). Of particular interest is HAT-P-34b which is moderately massive
(3.33 M <SUB>J</SUB>), has a high eccentricity of e = 0.441 ± 0.032
at a period of P = 5.452654 ± 0.000016 days, and shows hints of an
outer component. The other three planets have properties that are
typical of hot Jupiters. <P />Based in part on observations obtained
at the W. M. Keck Observatory, which is operated by the University
of California and the California Institute of Technology. Keck time
has been granted by NOAO (A289Hr) and NASA (N167Hr and N029Hr). Based
in part on data collected at the Subaru Telescope, which is operated
by the National Astronomical Observatory of Japan. Based in part on
observations made with the Nordic Optical Telescope, operated on the
island of La Palma jointly by Denmark, Finland, Iceland, Norway, and
Sweden, in the Spanish Observatorio del Roque de los Muchachos of the
Instituto de Astrofisica de Canarias.
---------------------------------------------------------
Title: HAT-P-17b,c: A Transiting, Eccentric, Hot Saturn and a
Long-period, Cold Jupiter
Authors: Howard, A. W.; Bakos, G. Á.; Hartman, J.; Torres, G.;
Shporer, A.; Mazeh, T.; Kovács, Géza; Latham, D. W.; Noyes, R. W.;
Fischer, D. A.; Johnson, J. A.; Marcy, G. W.; Esquerdo, G. A.; Béky,
B.; Butler, R. P.; Sasselov, D. D.; Stefanik, R. P.; Perumpilly, G.;
Lázár, J.; Papp, I.; Sári, P.
2012ApJ...749..134H Altcode: 2010arXiv1008.3898H
We report the discovery of HAT-P-17b,c, a multi-planet system with an
inner transiting planet in a short-period, eccentric orbit and an outer
planet in a 4.4 yr, nearly circular orbit. The inner planet, HAT-P-17b,
transits the bright V = 10.54 early K dwarf star GSC 2717-00417, with an
orbital period P = 10.338523 ± 0.000009 days, orbital eccentricity e =
0.342 ± 0.006, transit epoch T<SUB>c</SUB> = 2454801.16943 ± 0.00020
(BJD: barycentric Julian dates throughout the paper are calculated
from Coordinated Universal Time (UTC)), and transit duration 0.1690 ±
0.0009 days. HAT-P-17b has a mass of 0.534 ± 0.018 M <SUB>J</SUB> and
radius of 1.010 ± 0.029 R <SUB>J</SUB> yielding a mean density of 0.64
± 0.05 g cm<SUP>-3</SUP>. This planet has a relatively low equilibrium
temperature in the range 780-927 K, making it an attractive target for
follow-up spectroscopic studies. The outer planet, HAT-P-17c, has a
significantly longer orbital period P <SUB>2</SUB> = 1610 ± 20 days and
a minimum mass m <SUB>2</SUB>sin i <SUB>2</SUB> = 1.31<SUP>+0.18</SUP>
<SUB>-0.15</SUB> M <SUB>J</SUB>. The orbital inclination of HAT-P-17c is
unknown as transits have not been observed and may not be present. The
host star has a mass of 0.86 ± 0.04 M <SUB>⊙</SUB>, radius of 0.84
± 0.02 R <SUB>⊙</SUB>, effective temperature 5246 ± 80 K, and
metallicity [Fe/H] = 0.00 ± 0.08. HAT-P-17 is the second multi-planet
system detected from ground-based transit surveys. <P />Based in
part on observations obtained at the W. M. Keck Observatory, which is
operated by the University of California and the California Institute
of Technology. Keck time has been granted by NOAO and NASA.
---------------------------------------------------------
Title: HAT-P-25b: A Hot-Jupiter Transiting a Moderately Faint G Star
Authors: Quinn, S. N.; Bakos, G. Á.; Hartman, J.; Torres, G.; Kovács,
G.; Latham, D. W.; Noyes, R. W.; Fischer, D. A.; Johnson, J. A.; Marcy,
G. W.; Howard, A. W.; Szentgyorgyi, A.; Fűrész, G.; Buchhave, L. A.;
Béky, B.; Sasselov, D. D.; Stefanik, R. P.; Perumpilly, G.; Everett,
M.; Lázár, J.; Papp, I.; Sári, P.
2012ApJ...745...80Q Altcode: 2010arXiv1008.3565Q
We report the discovery of HAT-P-25b, a transiting extrasolar planet
orbiting the V = 13.19 G5 dwarf star GSC 1788-01237, with a period P =
3.652836 ± 0.000019 days, transit epoch T<SUB>c</SUB> = 2455176.85173
± 0.00047 (BJD—barycentric Julian dates throughout the paper are
calculated from Coordinated Universal Time, UTC), and transit duration
0.1174 ± 0.0017 days. The host star has a mass of 1.01 ± 0.03 M
<SUB>⊙</SUB>, radius of 0.96<SUP>+0.05</SUP> <SUB>- 0.04</SUB> R
<SUB>⊙</SUB>, effective temperature 5500 ± 80 K, and metallicity
[Fe/H] = +0.31 ± 0.08. The planetary companion has a mass of 0.567
± 0.022 M <SUB>J</SUB> and radius of 1.190<SUP>+0.081</SUP> <SUB>-
0.056</SUB> R <SUB>J</SUB> yielding a mean density of 0.42 ± 0.07
g cm<SUP>-3</SUP>. <P />Based in part on observations obtained at
the W. M. Keck Observatory, which is operated by the University of
California and the California Institute of Technology. Keck time
has been granted by NOAO (A201Hr), NASA (N018Hr and N167Hr), and
the NASA Gemini-Keck time-exchange program (G329Hr). Based in part
on observations made with the Nordic Optical Telescope, operated on
the island of La Palma jointly by Denmark, Finland, Iceland, Norway,
and Sweden, in the Spanish Observatorio del Roque de los Muchachos of
the Instituto de Astrofisica de Canarias.
---------------------------------------------------------
Title: HAT-P-20b-HAT-P-23b: Four Massive Transiting Extrasolar Planets
Authors: Bakos, G. Á.; Hartman, J.; Torres, G.; Latham, D. W.;
Kovács, Géza; Noyes, R. W.; Fischer, D. A.; Johnson, J. A.; Marcy,
G. W.; Howard, A. W.; Kipping, D.; Esquerdo, G. A.; Shporer, A.;
Béky, B.; Buchhave, L. A.; Perumpilly, G.; Everett, M.; Sasselov,
D. D.; Stefanik, R. P.; Lázár, J.; Papp, I.; Sári, P.
2011ApJ...742..116B Altcode: 2010arXiv1008.3388B
We report the discovery of four relatively massive (2-7 M <SUB>J</SUB>)
transiting extrasolar planets. HAT-P-20b orbits the moderately bright
V = 11.339 K3 dwarf star GSC 1910-00239 on a circular orbit, with a
period P = 2.875317 ± 0.000004 days, transit epoch T<SUB>c</SUB> =
2455080.92661 ± 0.00021 (BJD<SUB>UTC</SUB>), and transit duration
0.0770 ± 0.0008 days. The host star has a mass of 0.76 ± 0.03 M
<SUB>⊙</SUB>, radius of 0.69 ± 0.02 R <SUB>⊙</SUB>, effective
temperature 4595 ± 80 K, and metallicity [Fe/H] = +0.35 ± 0.08. The
planetary companion has a mass of 7.246 ± 0.187 M <SUB>J</SUB> and
a radius of 0.867 ± 0.033 R <SUB>J</SUB> yielding a mean density
of 13.78 ± 1.50 g cm<SUP>-3</SUP>. HAT-P-21b orbits the V = 11.685
G3 dwarf star GSC 3013-01229 on an eccentric (e = 0.228 ± 0.016)
orbit, with a period P = 4.124481 ± 0.000007 days, transit epoch
T<SUB>c</SUB> = 2454996.41312 ± 0.00069, and transit duration
0.1530 ± 0.0027 days. The host star has a mass of 0.95 ± 0.04 M
<SUB>⊙</SUB>, radius of 1.10 ± 0.08 R <SUB>⊙</SUB>, effective
temperature 5588 ± 80 K, and metallicity [Fe/H] = +0.01 ± 0.08. The
planetary companion has a mass of 4.063 ± 0.161 M <SUB>J</SUB> and
a radius of 1.024 ± 0.092 R <SUB>J</SUB> yielding a mean density of
4.68<SUP>+1.59</SUP> <SUB>- 0.99</SUB> g cm<SUP>-3</SUP>. HAT-P-21b
is a borderline object between the pM and pL class planets, and
the transits occur near apastron. HAT-P-22b orbits the bright V =
9.732 G5 dwarf star HD 233731 on a circular orbit, with a period P =
3.212220 ± 0.000009 days, transit epoch T<SUB>c</SUB> = 2454930.22001
± 0.00025, and transit duration 0.1196 ± 0.0014 days. The host star
has a mass of 0.92 ± 0.03 M <SUB>⊙</SUB>, radius of 1.04 ± 0.04 R
<SUB>⊙</SUB>, effective temperature 5302 ± 80 K, and metallicity
[Fe/H] = +0.24 ± 0.08. The planet has a mass of 2.147 ± 0.061 M
<SUB>J</SUB> and a compact radius of 1.080 ± 0.058 R <SUB>J</SUB>
yielding a mean density of 2.11<SUP>+0.40</SUP> <SUB>- 0.29</SUB>
g cm<SUP>-3</SUP>. The host star also harbors an M-dwarf companion at
a wide separation. Finally, HAT-P-23b orbits the V = 12.432 G0 dwarf
star GSC 1632-01396 on a close to circular orbit, with a period P =
1.212884 ± 0.000002 days, transit epoch T<SUB>c</SUB> = 2454852.26464
± 0.00018, and transit duration 0.0908 ± 0.0007 days. The host star
has a mass of 1.13 ± 0.04 M <SUB>⊙</SUB>, radius of 1.20 ± 0.07 R
<SUB>⊙</SUB>, effective temperature 5905 ± 80 K, and metallicity
[Fe/H] = +0.15 ± 0.04. The planetary companion has a mass of 2.090
± 0.111 M <SUB>J</SUB> and a radius of 1.368 ± 0.090 R <SUB>J</SUB>
yielding a mean density of 1.01 ± 0.18 g cm<SUP>-3</SUP>. HAT-P-23b is
an inflated and massive hot Jupiter on a very short period orbit, and
has one of the shortest characteristic infall times (7.5<SUP>+2.9</SUP>
<SUB>- 1.8</SUB> Myr) before it gets engulfed by the star. <P />Based in
part on observations obtained at the W. M. Keck Observatory, which is
operated by the University of California and the California Institute
of Technology. Keck time has been granted by NOAO and NASA.
---------------------------------------------------------
Title: HAT-P-32b and HAT-P-33b: Two Highly Inflated Hot Jupiters
Transiting High-jitter Stars
Authors: Hartman, J. D.; Bakos, G. Á.; Torres, G.; Latham, D. W.;
Kovács, Géza; Béky, B.; Quinn, S. N.; Mazeh, T.; Shporer, A.;
Marcy, G. W.; Howard, A. W.; Fischer, D. A.; Johnson, J. A.; Esquerdo,
G. A.; Noyes, R. W.; Sasselov, D. D.; Stefanik, R. P.; Fernandez,
J. M.; Szklenár, T.; Lázár, J.; Papp, I.; Sári, P.
2011ApJ...742...59H Altcode: 2011arXiv1106.1212H
We report the discovery of two exoplanets transiting high-jitter
stars. HAT-P-32b orbits the bright V = 11.289 late-F-early-G dwarf
star GSC 3281-00800, with a period P = 2.150008 ± 0.000001 d. The
stellar and planetary masses and radii depend on the eccentricity
of the system, which is poorly constrained due to the high-velocity
jitter (~80 m s<SUP>-1</SUP>). Assuming a circular orbit, the star
has a mass of 1.16 ± 0.04 M <SUB>⊙</SUB> and radius of 1.22 ±
0.02 R <SUB>⊙</SUB>, while the planet has a mass of 0.860 ± 0.164 M
<SUB>J</SUB> and a radius of 1.789 ± 0.025 R <SUB>J</SUB>. The second
planet, HAT-P-33b, orbits the bright V = 11.188 late-F dwarf star GSC
2461-00988, with a period P = 3.474474 ± 0.000001 d. As for HAT-P-32,
the stellar and planetary masses and radii of HAT-P-33 depend on the
eccentricity, which is poorly constrained due to the high jitter (~50
m s<SUP>-1</SUP>). In this case, spectral line bisector spans (BSs)
are significantly anti-correlated with the radial velocity residuals,
and we are able to use this correlation to reduce the residual rms to
~35 m s<SUP>-1</SUP>. We find that the star has a mass of 1.38 ± 0.04
M <SUB>⊙</SUB> and a radius of 1.64 ± 0.03 R <SUB>⊙</SUB> while the
planet has a mass of 0.762 ± 0.101 M <SUB>J</SUB> and a radius of 1.686
± 0.045 R <SUB>J</SUB> for an assumed circular orbit. Due to the large
BS variations exhibited by both stars we rely on detailed modeling of
the photometric light curves to rule out blend scenarios. Both planets
are among the largest radii transiting planets discovered to date. <P
/>Based in part on observations obtained at the W. M. Keck Observatory,
which is operated by the University of California and the California
Institute of Technology. Keck time has been granted by NOAO (A285Hr,
A146Hr, A201Hr, A289Hr), NASA (N128Hr, N145Hr, N049Hr, N018Hr, N167Hr,
N029Hr), and the NOAO Gemini/Keck time-exchange program (G329Hr).
---------------------------------------------------------
Title: HAT-P-31b,c: A Transiting, Eccentric, Hot Jupiter and a
Long-period, Massive Third Body
Authors: Kipping, D. M.; Hartman, J.; Bakos, G. Á.; Torres, G.;
Latham, D. W.; Bayliss, D.; Kiss, L. L.; Sato, B.; Béky, B.; Kovács,
Géza; Quinn, S. N.; Buchhave, L. A.; Andersen, J.; Marcy, G. W.;
Howard, A. W.; Fischer, D. A.; Johnson, J. A.; Noyes, R. W.; Sasselov,
D. D.; Stefanik, R. P.; Lázár, J.; Papp, I.; Sári, P.; Fűrész, G.
2011AJ....142...95K Altcode: 2011arXiv1106.1169K
We report the discovery of HAT-P-31b, a transiting exoplanet orbiting
the V = 11.660 dwarf star GSC 2099-00908. HAT-P-31b is the first
planet discovered with the Hungarian-made Automated Telescope (HAT)
without any follow-up photometry, demonstrating the feasibility of a
new mode of operation for the HATNet project. The 2.17 M<SUB>J</SUB>
, 1.1 R<SUB>J</SUB> planet has a period of P<SUB>b</SUB> = 5.0054 days
and maintains an unusually high eccentricity of e<SUB>b</SUB> = 0.2450
± 0.0045, determined through Keck, FIbr-fed Échelle Spectrograph,
and Subaru high-precision radial velocities (RVs). Detailed
modeling of the RVs indicates an additional quadratic residual
trend in the data detected to very high confidence. We interpret
this trend as a long-period outer companion, HAT-P-31c, of minimum
mass 3.4 M<SUB>J</SUB> and period >=2.8 years. Since current RVs
span less than half an orbital period, we are unable to determine
the properties of HAT-P-31c to high confidence. However, dynamical
simulations of two possible configurations show that orbital stability
is to be expected. Further, if HAT-P-31c has non-zero eccentricity,
our simulations show that the eccentricity of HAT-P-31b is actively
driven by the presence of c, making HAT-P-31 a potentially intriguing
dynamical laboratory. <P />Based in part on observations obtained at
the W. M. Keck Observatory, which is operated by the University of
California and the California Institute of Technology. Keck time has
been granted by NASA (N167Hr). Based in part on data collected at Subaru
Telescope, which is operated by the National Astronomical Observatory
of Japan. Based in part on observations made with the Nordic Optical
Telescope, operated on the island of La Palma jointly by Denmark,
Finland, Iceland, Norway, and Sweden, in the Spanish Observatorio del
Roque de los Muchachos of the Instituto de Astrofisica de Canarias.
---------------------------------------------------------
Title: Confirmation spectroscopy of HATNet transiting exoplanet
candidates using Keck-I/HIRES
Authors: Bakos, Gaspar; Torres, Guillermo; Latham, David W.; Noyes,
Robert W.; Hartman, Joel D.
2011noao.prop..600B Altcode:
The HATNet project has produced dozens of high quality transiting
exoplanet (TEP) candidates around bright (V<13.0) stars. In order
to confirm their planetary nature, and perform accurate initial
characterization, they require high-precision radial velocity (RV)
observations and spectral line bisector analysis. Thirty HATNet
TEPs have been published or submitted so far based almost entirely
on Keck/HIRES observations; several more have been verified and
are in the process of being analyzed, some of these may require
additional observations if detailed analysis suggests the presence
of additional planets in the system or a non-zero eccentricity, ~26
more need further Keck/HIRES spectra for better characterization
leading to final confirmation, and ~17 more are ready for initial
HIRES observations. There is a continuous flow of dozens of high
quality candidates per semester. To date, 75% of the HIRES time is
spent on candidates that are eventually identified as hosting TEPs -
representing a very efficient use of Keck. We propose for 4 nights
on Keck-I/HIRES for 2011B to finish pending candidates and also to
perform a similar analysis on new targets. We are confident that this
effort will lead to the announcement of several new bright TEPs.
---------------------------------------------------------
Title: HAT-P-30b: A Transiting Hot Jupiter on a Highly Oblique Orbit
Authors: Johnson, John Asher; Winn, J. N.; Bakos, G. Á.; Hartman,
J. D.; Morton, T. D.; Torres, G.; Kovács, Géza; Latham, D. W.;
Noyes, R. W.; Sato, B.; Esquerdo, G. A.; Fischer, D. A.; Marcy, G. W.;
Howard, A. W.; Buchhave, L. A.; Fűrész, G.; Quinn, S. N.; Béky,
B.; Sasselov, D. D.; Stefanik, R. P.; Lázár, J.; Papp, I.; Sári, P.
2011ApJ...735...24J Altcode: 2011arXiv1103.3825J
We report the discovery of HAT-P-30b, a transiting exoplanet orbiting
the V = 10.419 dwarf star GSC 0208-00722. The planet has a period P =
2.810595 ± 0.000005 days, transit epoch T<SUB>c</SUB> = 2455456.46561
± 0.00037 (BJD), and transit duration 0.0887 ± 0.0015 days. The host
star has a mass of 1.24 ± 0.04 M <SUB>sun</SUB>, radius of 1.21 ± 0.05
R <SUB>sun</SUB>, effective temperature of 6304 ± 88 K, and metallicity
[Fe/H] = +0.13 ± 0.08. The planetary companion has a mass of 0.711
± 0.028 M <SUB>J</SUB> and radius of 1.340 ± 0.065 R <SUB>J</SUB>
yielding a mean density of 0.37 ± 0.05 g cm<SUP>-3</SUP>. We also
present radial velocity measurements that were obtained throughout
a transit that exhibit the Rossiter-McLaughlin effect. By modeling
this effect, we measure an angle of λ = 73fdg5 ± 9fdg0 between
the sky projections of the planet's orbit normal and the star's spin
axis. HAT-P-30b represents another example of a close-in planet on a
highly tilted orbit, and conforms to the previously noted pattern that
tilted orbits are more common around stars with T <SUB>effsstarf</SUB>
>~ 6250 K. <P />Based in part on observations obtained at the
W. M. Keck Observatory, which is operated by the University of
California and the California Institute of Technology. Keck time
has been granted by NASA (N167Hr). Based in part on data collected
at Subaru Telescope, which is operated by the National Astronomical
Observatory of Japan.
---------------------------------------------------------
Title: Hat-P-28b and Hat-P-29b: Two Sub-Jupiter Mass Transiting
Planets
Authors: Buchhave, L. A.; Bakos, G. Á.; Hartman, J. D.; Torres,
G.; Latham, D. W.; Andersen, J.; Kovács, G.; Noyes, R. W.; Shporer,
A.; Esquerdo, G. A.; Fischer, D. A.; Johnson, J. A.; Marcy, G. W.;
Howard, A. W.; Béky, B.; Sasselov, D. D.; Fűrész, G.; Quinn, S. N.;
Stefanik, R. P.; Szklenár, T.; Berlind, P.; Calkins, M. L.; Lázár,
J.; Papp, I.; Sári, P.
2011ApJ...733..116B Altcode: 2011arXiv1103.1813B
We present the discovery of two transiting exoplanets. HAT-P-28b orbits
a V = 13.03 G3 dwarf star with a period P = 3.2572 days and has a mass
of 0.63 ± 0.04 M <SUB>J</SUB> and a radius of 1.21<SUP>+0.11</SUP>
<SUB>- 0.08</SUB> R <SUB>J</SUB> yielding a mean density of 0.44 ±
0.09 g cm<SUP>-3</SUP>. HAT-P-29b orbits a V = 11.90 F8 dwarf star
with a period P = 5.7232 days and has a mass of 0.78<SUP>+0.08</SUP>
<SUB>- 0.04</SUB> M <SUB>J</SUB> and a radius of 1.11<SUP>+0.14</SUP>
<SUB>- 0.08</SUB> R <SUB>J</SUB> yielding a mean density of 0.71 ±
0.18 g cm<SUP>-3</SUP>. We discuss the properties of these planets in
the context of other known transiting planets.
---------------------------------------------------------
Title: HAT-P-27b: A Hot Jupiter Transiting a G Star on a 3 Day Orbit
Authors: Béky, B.; Bakos, G. Á.; Hartman, J.; Torres, G.; Latham,
D. W.; Jordán, A.; Arriagada, P.; Bayliss, D.; Kiss, L. L.; Kovács,
Géza; Quinn, S. N.; Marcy, G. W.; Howard, A. W.; Fischer, D. A.;
Johnson, J. A.; Esquerdo, G. A.; Noyes, R. W.; Buchhave, L. A.;
Sasselov, D. D.; Stefanik, R. P.; Perumpilly, G.; Lázár, J.; Papp,
I.; Sári, P.
2011ApJ...734..109B Altcode: 2011arXiv1101.3511B
We report the discovery of HAT-P-27b, an exoplanet transiting the
moderately bright G8 dwarf star GSC 0333-00351 (V = 12.214). The
orbital period is 3.039586 ± 0.000012 days, the reference epoch of
transit is 2455186.01879 ± 0.00054 (BJD), and the transit duration is
0.0705 ± 0.0019 days. The host star with its effective temperature
5300 ± 90 K is somewhat cooler than the Sun and is more metal-rich
with a metallicity of +0.29 ± 0.10. Its mass is 0.94 ± 0.04 M
<SUB>sun</SUB> and radius is 0.90<SUP>+0.05</SUP> <SUB>- 0.04</SUB>
R <SUB>sun</SUB>. For the planetary companion we determine a mass of
0.660 ± 0.033 M <SUB>J</SUB> and radius of 1.038<SUP>+0.077</SUP>
<SUB>- 0.058</SUB> R <SUB>J</SUB>. For the 30 known transiting
exoplanets between 0.3 M <SUB>J</SUB> and 0.8 M <SUB>J</SUB>, a negative
correlation between host star metallicity and planetary radius and an
additional dependence of planetary radius on equilibrium temperature are
confirmed at a high level of statistical significance. <P />Based in
part on observations obtained at the W. M. Keck Observatory, which is
operated by the University of California and the California Institute
of Technology. Keck time has been granted by NOAO (A201Hr) and NASA
(N018Hr, N167Hr).
---------------------------------------------------------
Title: A Photometric Variability Survey of Field K and M Dwarf Stars
with HATNet
Authors: Hartman, J. D.; Bakos, G. Á.; Noyes, R. W.; Sipőcz, B.;
Kovács, G.; Mazeh, T.; Shporer, A.; Pál, A.
2011AJ....141..166H Altcode:
Using light curves from the HATNet survey for transiting extrasolar
planets we investigate the optical broadband photometric variability
of a sample of 27, 560 field K and M dwarfs selected by color and
proper motion (V - K >~ 3.0, μ > 30 mas yr<SUP>-1</SUP>,
plus additional cuts in J - H versus H - K<SUB>S</SUB> and on the
reduced proper motion). We search the light curves for periodic
variations and for large-amplitude, long-duration flare events. A
total of 2120 stars exhibit potential variability, including 95 stars
with eclipses and 60 stars with flares. Based on a visual inspection
of these light curves and an automated blending classification, we
select 1568 stars, including 78 eclipsing binaries (EBs), as secure
variable star detections that are not obvious blends. We estimate that
a further ~26% of these stars may be blends with fainter variables,
though most of these blends are likely to be among the hotter stars
in our sample. We find that only 38 of the 1568 stars, including
five of the EBs, have previously been identified as variables or
are blended with previously identified variables. One of the newly
identified EBs is 1RXS J154727.5+450803, a known P = 3.55 day, late
M-dwarf SB2 system, for which we derive preliminary estimates for
the component masses and radii of M <SUB>1</SUB> = M <SUB>2</SUB> =
0.258 ± 0.008 M <SUB>sun</SUB> and R <SUB>1</SUB> = R <SUB>2</SUB> =
0.289 ± 0.007 R <SUB>sun</SUB>. The radii of the component stars are
larger than theoretical expectations if the system is older than ~200
Myr. The majority of the variables are heavily spotted BY Dra-type
stars for which we determine rotation periods. Using this sample, we
investigate the relations between period, color, age, and activity
measures, including optical flaring, for K and M dwarfs, finding
that many of the well-established relations for F, G, and K dwarfs
continue into the M dwarf regime. We find that the fraction of stars
that is variable with peak-to-peak amplitudes greater than 0.01 mag
increases exponentially with the V - K<SUB>S</SUB> color such that
approximately half of field dwarfs in the solar neighborhood with M
<~ 0.2 M <SUB>sun</SUB> are variable at this level. Our data hint
at a change in the rotation-activity-age connection for stars with M
<~ 0.25 M <SUB>sun</SUB>.
---------------------------------------------------------
Title: VizieR Online Data Catalog: HATNet Pleiades Rotation Period
Catalogue (Hartman+, 2010)
Authors: Hartman, J. D.; Bakos, G. A.; Kovacs, G.; Noyes, R. W.
2011yCat..74080475H Altcode:
Photometric time-series observations of the Pleiades cluster were
obtained between 2008 September 15 and 2009 March 16 using the
identical HAT-9 and HAT-10 11-cm aperture robotic telescopes located
at Mauna Kea Observatory (MKO) in Hawaii and at Fred L. Whipple
Observatory (FLWO) in Arizona, respectively. <P />This catalogue
contains photometric rotation periods for stars in the Pleiades open
cluster. Most of the periods were measured from light curves obtained
with the Hungarian-made Automated Telescope Network (HATNet) of small
aperture robotic telescopes located in Arizona and Hawaii. A handful
of stars with periods from the literature that were not recovered with
the HATNet data are also included in the catalogue. <P />(5 data files).
---------------------------------------------------------
Title: Planets from the HATNet project
Authors: Bakos, G. Á.; Hartman, J. D.; Torres, G.; Kovács, G.;
Noyes, R. W.; Latham, D. W.; Sasselov, D. D.; Béky, B.
2011EPJWC..1101002B Altcode: 2011arXiv1101.0322B
We summarize the contribution of the HATNet project to extrasolar
planet science, highlighting published planets (HAT-P-1b through
HAT-P-26b). We also briefly discuss the operations, data analysis,
candidate selection and confirmation procedures, and we summarize what
HATNet provides to the exoplanet community with each discovery.
---------------------------------------------------------
Title: HAT-P-26b: A Low-density Neptune-mass Planet Transiting a
K Star
Authors: Hartman, J. D.; Bakos, G. Á.; Kipping, D. M.; Torres, G.;
Kovács, G.; Noyes, R. W.; Latham, D. W.; Howard, A. W.; Fischer,
D. A.; Johnson, J. A.; Marcy, G. W.; Isaacson, H.; Quinn, S. N.;
Buchhave, L. A.; Béky, B.; Sasselov, D. D.; Stefanik, R. P.; Esquerdo,
G. A.; Everett, M.; Perumpilly, G.; Lázár, J.; Papp, I.; Sári, P.
2011ApJ...728..138H Altcode: 2010arXiv1010.1008H
We report the discovery of HAT-P-26b, a transiting extrasolar planet
orbiting the moderately bright V = 11.744 K1 dwarf star GSC 0320-01027,
with a period P = 4.234516 ± 0.000015 days, transit epoch T<SUB>c</SUB>
= 2455304.65122 ± 0.00035 (BJD; Barycentric Julian dates throughout the
paper are calculated from Coordinated Universal Time (UTC)), and transit
duration 0.1023 ± 0.0010 days. The host star has a mass of 0.82 ±
0.03 M <SUB>sun</SUB>, radius of 0.79<SUP>+0.10</SUP> <SUB>-0.04</SUB>
R <SUB>sun</SUB>, effective temperature 5079 ± 88 K, and metallicity
[Fe/H] = -0.04 ± 0.08. The planetary companion has a mass of
0.059 ± 0.007 M <SUB>J</SUB>, and radius of 0.565<SUP>+0.072</SUP>
<SUB>-0.032</SUB> R <SUB>J</SUB> yielding a mean density of 0.40 ±
0.10 g cm<SUP>-3</SUP>. HAT-P-26b is the fourth Neptune-mass transiting
planet discovered to date. It has a mass that is comparable to those
of Neptune and Uranus, and slightly smaller than those of the other
transiting Super-Neptunes, but a radius that is ~65% larger than
those of Neptune and Uranus, and also larger than those of the other
transiting Super-Neptunes. HAT-P-26b is consistent with theoretical
models of an irradiated Neptune-mass planet with a 10 M <SUB>⊕</SUB>
heavy element core that comprises gsim50% of its mass with the remainder
contained in a significant hydrogen-helium envelope, though the exact
composition is uncertain as there are significant differences between
various theoretical models at the Neptune-mass regime. The equatorial
declination of the star makes it easily accessible to both Northern and
Southern ground-based facilities for follow-up observations. <P />Based
in part on observations obtained at the W. M. Keck Observatory, which
is operated by the University of California and the California Institute
of Technology. Keck time has been granted by NASA (N018Hr and N167Hr).
---------------------------------------------------------
Title: Confirmation spectroscopy of HATNet transiting exoplanet
candidates using Keck-I/HIRES
Authors: Bakos, Gaspar; Torres, Guillermo; Latham, David W.; Noyes,
Robert W.; Hartman, Joel D.
2011noao.prop..207B Altcode:
The HATNet project has produced dozens of high quality transiting
exoplanet (TEP) candidates around bright (V<13.0) stars. In order
to confirm their planetary nature, and perform accurate initial
characterization, they require high-precision radial velocity (RV)
observations and spectral line bisector analysis. Twenty-six HATNet
TEPs have been published or submitted so far based almost entirely
on Keck/HIRES observations; several more have been verified and
are in the process of being analyzed, some of these may require
additional observations if detailed analysis suggests the presence
of additional planets in the system or a non-zero eccentricity, ~20
more need further Keck/HIRES spectra for better characterization
leading to final confirmation, and ~12 more are ready for initial
HIRES observations. There is a continuous flow of dozens of high
quality candidates per semester. To date, 75% of the HIRES time is
spent on candidates that are eventually identified as hosting TEPs -
representing a very efficient use of Keck. We propose for 4 nights
on Keck-I/HIRES for 2011A to finish pending candidates and also to
perform a similar analysis on new targets. We are confident that this
effort will lead to the announcement of several new bright TEPs.
---------------------------------------------------------
Title: HAT-P-18b and HAT-P-19b: Two Low-density Saturn-mass Planets
Transiting Metal-rich K Stars
Authors: Hartman, J. D.; Bakos, G. Á.; Sato, B.; Torres, G.; Noyes,
R. W.; Latham, D. W.; Kovács, G.; Fischer, D. A.; Howard, A. W.;
Johnson, J. A.; Marcy, G. W.; Buchhave, L. A.; Füresz, G.; Perumpilly,
G.; Béky, B.; Stefanik, R. P.; Sasselov, D. D.; Esquerdo, G. A.;
Everett, M.; Csubry, Z.; Lázár, J.; Papp, I.; Sári, P.
2011ApJ...726...52H Altcode: 2010arXiv1007.4850H
We report the discovery of two new transiting extrasolar
planets. HAT-P-18b orbits the V = 12.759 K2 dwarf star GSC 2594-00646,
with a period P = 5.508023 ± 0.000006 days, transit epoch T<SUB>c</SUB>
= 2454715.02174 ± 0.00020 (BJD), and transit duration 0.1131 ± 0.0009
days. The host star has a mass of 0.77 ± 0.03 M <SUB>sun</SUB>,
radius of 0.75 ± 0.04 R <SUB>sun</SUB>, effective temperature
4803 ± 80 K, and metallicity [Fe/H] = +0.10 ± 0.08. The planetary
companion has a mass of 0.197 ± 0.013 M <SUB>J</SUB> and radius of
0.995 ± 0.052 R <SUB>J</SUB>, yielding a mean density of 0.25 ± 0.04
g cm<SUP>-3</SUP>. HAT-P-19b orbits the V = 12.901 K1 dwarf star GSC
2283-00589, with a period P = 4.008778 ± 0.000006 days, transit epoch
T<SUB>c</SUB> = 2455091.53417 ± 0.00034 (BJD), and transit duration
0.1182 ± 0.0014 days. The host star has a mass of 0.84 ± 0.04 M
<SUB>sun</SUB>, radius of 0.82 ± 0.05 R <SUB>sun</SUB>, effective
temperature 4990 ± 130 K, and metallicity [Fe/H] = +0.23 ± 0.08. The
planetary companion has a mass of 0.292 ± 0.018 M <SUB>J</SUB> and
radius of 1.132 ± 0.072 R <SUB>J</SUB>, yielding a mean density of
0.25 ± 0.04 g cm<SUP>-3</SUP>. The radial velocity residuals for
HAT-P-19 exhibit a linear trend in time, which indicates the presence
of a third body in the system. Comparing these observations with
theoretical models, we find that HAT-P-18b and HAT-P-19b are each
consistent with a hydrogen-helium-dominated gas giant planet with
negligible core mass. HAT-P-18b and HAT-P-19b join HAT-P-12b and
WASP-21b in an emerging group of low-density Saturn-mass planets,
with negligible inferred core masses. However, unlike HAT-P-12b and
WASP-21b, both HAT-P-18b and HAT-P-19b orbit stars with super-solar
metallicity. This calls into question the heretofore suggestive
correlation between the inferred core mass and host star metallicity
for Saturn-mass planets. <P />Based in part on observations obtained
at the W. M. Keck Observatory, which is operated by the University of
California and the California Institute of Technology. Keck time has
been granted by NOAO (A146Hr, A201Hr, and A264Hr), NASA (N018Hr, N049Hr,
N128Hr, and N167Hr), and by the NOAO Keck-Gemini time exchange program
(G329Hr). Based in part on data collected at Subaru Telescope, which is
operated by the National Astronomical Observatory of Japan. Based in
part on observations made with the Nordic Optical Telescope, operated
on the island of La Palma jointly by Denmark, Finland, Iceland, Norway,
and Sweden, in the Spanish Observatorio del Roque de los Muchachos of
the Instituto de Astrofisica de Canarias.
---------------------------------------------------------
Title: Hat-south: A Global Network Of Wide Angle Telescopes Searching
For Transiting Extrasolar Planets Around Bright Stars
Authors: Bakos, Gaspar; Csubry, Z.; Penev, K.; Afonso, C.; Bayliss,
D.; Beky, B.; Conroy, P.; Csak, B.; Henning, T.; Jordan, A.; Kovacs,
G.; Lazar, J.; Noyes, R.; Papp, I.; Rabus, M.; Sackett, P.; Sari,
P.; Sasselov, D.; Schmidt, B.; Suc, V.; Ueltzhoeffer, K.
2011AAS...21725302B Altcode: 2011BAAS...4325302B
HAT-South is the first global network dedicated to searching for
transiting planets. With stations in Chile, Australia, and Namibia
(managed by CfA/PUC, ANU and MPIA, respectively), it provides a
unique, high precision, 24-hour data-stream on stars brighter than
14th magnitude. The HAT-South instruments were installed in 2009,
and the network began preliminary operations in 2010. Each site hosts
a pair of telescope mounts, and each mount is equipped with four
0.18m diameter, f/2.8 reflectors and four 4Kx4K CCDs. This yields
a 8x8 degree mosaic field per mount, imaged onto 64 megapixels. We
describe further details of the instrument in our poster, including
the instrument control software environment responsible for the fully
automated operations. We also summarize the first year of operations,
data-flow, initial performance, and early results.
---------------------------------------------------------
Title: HAT-P-15b: A 10.9 Day Extrasolar Planet Transiting a
Solar-type Star
Authors: Kovács, G.; Bakos, G. Á.; Hartman, J. D.; Torres, G.; Noyes,
R. W.; Latham, D. W.; Howard, A. W.; Fischer, D. A.; Johnson, J. A.;
Marcy, G. W.; Isaacson, H.; Sasselov, D. D.; Stefanik, R. P.; Esquerdo,
G. A.; Fernandez, J. M.; Lázár, B. Béky J.; Papp, I.; Sári, P.
2010ApJ...724..866K Altcode: 2010arXiv1005.5300K
We report the discovery of HAT-P-15b, a transiting extrasolar planet in
the "period valley," a relatively sparsely populated period regime of
the known extrasolar planets. The host star, GSC 2883-01687, is a G5
dwarf with V= 12.16. It has a mass of 1.01 ± 0.04 M <SUB>sun</SUB>,
radius of 1.08 ± 0.04 R <SUB>sun</SUB>, effective temperature
5568 ± 90 K, and metallicity [Fe/H] = +0.22 ± 0.08. The planetary
companion orbits the star with a period P = 10.863502 ± 0.000027
days, transit epoch T<SUB>c</SUB> = 2454638.56019 ± 0.00048 (BJD),
and transit duration 0.2285 ± 0.0015 days. It has a mass of 1.946
± 0.066 M <SUB>J</SUB> and radius of 1.072 ± 0.043 R <SUB>J</SUB>
yielding a mean density of 1.96 ± 0.22 g cm<SUP>-3</SUP>. At an age of
6.8<SUP>+2.5</SUP> <SUB>-1.6</SUB> Gyr, the planet is H/He-dominated
and theoretical models require about 2% (10 M <SUB>⊕</SUB>) worth
of heavy elements to reproduce its measured radius. With an estimated
equilibrium temperature of ~820 K during transit, and ~1000 K at
occultation, HAT-P-15b is a potential candidate to study moderately cool
planetary atmospheres by transmission and occultation spectroscopy. <P
/>Based in part on observations obtained at the W. M. Keck Observatory,
which is operated by the University of California and the California
Institute of Technology.
---------------------------------------------------------
Title: HAT-P-24b: An Inflated Hot Jupiter on a 3.36 Day Period
Transiting a Hot, Metal-poor Star
Authors: Kipping, D. M.; Bakos, G. Á.; Hartman, J.; Torres, G.;
Shporer, A.; Latham, D. W.; Kovács, Géza; Noyes, R. W.; Howard,
A. W.; Fischer, D. A.; Johnson, J. A.; Marcy, G. W.; Béky, B.;
Perumpilly, G.; Esquerdo, G. A.; Sasselov, D. D.; Stefanik, R. P.;
Lázár, J.; Papp, I.; Sári, P.
2010ApJ...725.2017K Altcode: 2010arXiv1008.3389K
We report the discovery of HAT-P-24b, a transiting extrasolar
planet orbiting the moderately bright V = 11.818 F8 dwarf star GSC
0774-01441, with a period P = 3.3552464 ± 0.0000071 days, transit
epoch T<SUB>c</SUB> = 2455216.97669 ± 0.00024 (BJD)11, and transit
duration 3.653 ± 0.025 hr. The host star has a mass of 1.191 ±
0.042 M <SUB>sun</SUB>, radius of 1.317 ± 0.068 R <SUB>sun</SUB>,
effective temperature 6373 ± 80 K, and a low metallicity of [Fe/H]
= -0.16 ± 0.08. The planetary companion has a mass of 0.681 ±
0.031 M <SUB>J</SUB> and radius of 1.243 ± 0.072 R <SUB>J</SUB>
yielding a mean density of 0.439 ± 0.069 g cm<SUP>-3</SUP>. By
repeating our global fits with different parameter sets, we have
performed a critical investigation of the fitting techniques used for
previous Hungarian-made Automated Telescope planetary discoveries. We
find that the system properties are robust against the choice of
priors. The effects of fixed versus fitted limb darkening are also
examined. HAT-P-24b probably maintains a small eccentricity of e =
0.052<SUP>+0.022</SUP> <SUB>-0.017</SUB>, which is accepted over the
circular orbit model with false alarm probability 5.8%. In the absence
of eccentricity pumping, this result suggests that HAT-P-24b experiences
less tidal dissipation than Jupiter. Due to relatively rapid stellar
rotation, we estimate that HAT-P-24b should exhibit one of the largest
known Rossiter-McLaughlin effect amplitudes for an exoplanet (ΔV
<SUB>RM</SUB> ~= 95 m s<SUP>-1</SUP>) and thus a precise measurement of
the sky-projected spin-orbit alignment should be possible. <P />Based in
part on observations obtained at the W. M. Keck Observatory, which is
operated by the University of California and the California Institute
of Technology. Keck time has been granted by NOAO and NASA.
---------------------------------------------------------
Title: Asteroseismology of solar-type stars with Kepler I: Data
analysis
Authors: Karoff, C.; Chaplin, W. J.; Appourchaux, T.; Elsworth, Y.;
Garcia, R. A.; Houdek, G.; Metcalfe, T. S.; Molenda-Żakowicz, J.;
Monteiro, M. J. P. F. G.; Thompson, M. J.; Christensen-Dalsgaard, J.;
Gilliland, R. L.; Kjeldsen, H.; Basu, S.; Bedding, T. R.; Campante,
T. L.; Eggenberger, P.; Fletcher, S. T.; Gaulme, P.; Handberg, R.;
Hekker, S.; Martic, M.; Mathur, S.; Mosser, B.; Regulo, C.; Roxburgh,
I. W.; Salabert, D.; Stello, D.; Verner, G. A.; Belkacem, K.; Biazzo,
K.; Cunha, M. S.; Gruberbauer, M.; Guzik, J. A.; Kupka, F.; Leroy,
B.; Ludwig, H. -G.; Mathis, S.; Noels, A.; Noyes, R. W.; Roca Cortes,
T.; Roth, M.; Sato, K. H.; Schmitt, J.; Suran, M. D.; Trampedach,
R.; Uytterhoeven, K.; Ventura, R.
2010AN....331..972K Altcode: 2010arXiv1005.0507K
We report on the first asteroseismic analysis of solar-type stars
observed by Kepler. Observations of three G-type stars, made at
one-minute cadence during the first 33.5 days of science operations,
reveal high signal-to-noise solar-like oscillation spectra in all three
stars: About 20 modes of oscillation can clearly be distinguished
in each star. We discuss the appearance of the oscillation spectra,
including the presence of a possible signature of faculae, and the
presence of mixed modes in one of the three stars.
---------------------------------------------------------
Title: A large sample of photometric rotation periods for FGK
Pleiades stars
Authors: Hartman, J. D.; Bakos, G. Á.; Kovács, G.; Noyes, R. W.
2010MNRAS.408..475H Altcode: 2010MNRAS.tmp.1162H
Using data from the Hungarian-made Automated Telescope Network
(HATNet) survey for transiting exoplanets, we measure photometric
rotation periods for 368 Pleiades stars with 0.4 <~ M <~
1.3 M<SUB>solar</SUB>. We detect periodic variability for 74 per
cent of the cluster members in this mass range that are within our
field-of-view, and 93 per cent of the members with 0.7 <~ M <~
1.0 M<SUB>solar</SUB>. This increases, by a factor of 5, the number
of Pleiades members with measured periods. We compare these data to
the rich sample of spectroscopically determined projected equatorial
rotation velocities (v sini) available in the literature for this
cluster. Included in our sample are 14 newly identified probable
cluster members which have proper motions, photometry and rotation
periods consistent with membership. For stars with M >~ 0.85
M<SUB>solar</SUB> the rotation periods, v sini and radius estimates
are consistent with the stars having an isotropic distribution of
rotation axes, if a moderate differential rotation law is assumed. For
stars with M <~ 0.85 M<SUB>solar</SUB>, the inferred sini values
are systematically larger than 1.0. These observations imply that
the combination of measured parameters P(v sini)/R is too large by ~
24 per cent for low-mass stars in this cluster. By comparing our new
mass-period relation for the Pleiades to the slightly older cluster
M35, we confirm previous indications that the spin-down stalls at ~
100 Myr for the slowest rotating stars with 0.7 <~ M <~ 1.1
M<SUB>solar</SUB> - a fact which may indicate that the internal
transport of angular momentum is inefficient in slowly rotating
solar-mass stars.
---------------------------------------------------------
Title: Detection of the Secondary Eclipse of Exoplanet HAT-P-11b
Authors: Barry, R. K.; Bakos, G.; Harrington, J.; Madhusudhan, N.;
Noyes, R.; Seager, S.; Deming, L. D.
2010epsc.conf..342B Altcode:
No abstract at ADS
---------------------------------------------------------
Title: HAT-P-16b: A 4 M <SUB>J</SUB> Planet Transiting a Bright Star
on an Eccentric Orbit
Authors: Buchhave, L. A.; Bakos, G. Á.; Hartman, J. D.; Torres, G.;
Kovács, G.; Latham, D. W.; Noyes, R. W.; Esquerdo, G. A.; Everett, M.;
Howard, A. W.; Marcy, G. W.; Fischer, D. A.; Johnson, J. A.; Andersen,
J.; Fűrész, G.; Perumpilly, G.; Sasselov, D. D.; Stefanik, R. P.;
Béky, B.; Lázár, J.; Papp, I.; Sári, P.
2010ApJ...720.1118B Altcode: 2010arXiv1005.2009B
We report the discovery of HAT-P-16b, a transiting extrasolar planet
orbiting the V = 10.8 mag F8 dwarf GSC 2792-01700, with a period P =
2.775960 ± 0.000003 days, transit epoch T<SUB>c</SUB> = 2455027.59293
± 0.00031 (BJD<SUP>10</SUP>), and transit duration 0.1276 ± 0.0013
days. The host star has a mass of 1.22 ± 0.04 M <SUB>sun</SUB>,
radius of 1.24 ± 0.05 R <SUB>sun</SUB>, effective temperature 6158
± 80 K, and metallicity [Fe/H] = +0.17 ± 0.08. The planetary
companion has a mass of 4.193 ± 0.094 M <SUB>J</SUB> and radius
of 1.289 ± 0.066 R <SUB>J</SUB>, yielding a mean density of 2.42
± 0.35 g cm<SUP>-3</SUP>. Comparing these observed characteristics
with recent theoretical models, we find that HAT-P-16b is consistent
with a 1 Gyr H/He-dominated gas giant planet. HAT-P-16b resides in a
sparsely populated region of the mass-radius diagram and has a non-zero
eccentricity of e = 0.036 with a significance of 10σ. <P />Based in
part on observations made with the Nordic Optical Telescope, operated
on the island of La Palma jointly by Denmark, Finland, Iceland,
Norway, and Sweden, in the Spanish Observatorio del Roque de los
Muchachos of the Instituto de Astrofisica de Canarias. <P />Based in
part on observations obtained at the W. M. Keck Observatory, which is
operated by the University of California and the California Institute
of Technology. Keck time has been granted by NASA (N018Hr).
---------------------------------------------------------
Title: Confirmation spectroscopy of HATNet transiting exoplanet
candidates using Keck-I/HIRES
Authors: Bakos, Gaspar; Torres, Guillermo; Latham, David W.; Noyes,
Robert W.; Hartman, Joel D.
2010noao.prop..130B Altcode:
The HATNet project has produced dozens of transiting exoplanet (TEP)
candidates around bright (V<13.0) stars. In order to confirm their
planetary nature, and perform accurate initial characterization, they
require high-precision radial velocity (RV) observations and spectral
line bisector analysis. Fifteen HATNet TEPs have been published or
submitted so far based almost entirely on Keck/HIRES observations;
another 10 have been verified and are in the process of being analyzed,
some of these may require additional observations if detailed analysis
suggests the presence of additional planets in the system or a non-zero
eccentricity, ~15 more need further Keck/HIRES spectra for better
characterization leading to final confirmation, and ~15 more are
ready for initial HIRES observations. We expect dozens of additional
candidates per semester. These are high quality candidates: based on
statistics to date, 75% of the HIRES time is spent on candidates that
are eventually identified as hosting transiting planets- representing
a very efficient use of Keck. We propose for 4 nights on Keck-I/HIRES
for 2010B to finish pending candidates and also to perform a similar
analysis on new targets. We are confident that this effort will lead
to the announcement of several new TEPs.
---------------------------------------------------------
Title: A Large Sample of Photometric Rotation Periods for FGK
Pleiades Stars
Authors: Hartman, Joel D.; Bakos, Gáspár Á; Kovács, Géza; Noyes,
Robert W.
2010arXiv1006.0950H Altcode:
Using data from the HATNet survey for transiting exoplanets we measure
photometric rotation periods for 368 Pleiades stars with 0.4 Msun <
M < 1.3 Msun. We detect periodic variability for 74% of the cluster
members in this mass range that are within our field-of-view, and 93%
of the members with 0.7 Msun < M < 1.0 Msun. This increases,
by a factor of five, the number of Pleiades members with measured
periods. Included in our sample are 14 newly identified probable cluster
members which have proper motions, photometry, and rotation periods
consistent with membership. We compare this data to the rich sample of
spectroscopically determined projected equatorial rotation velocities
(vsini) available in the literature for this cluster. For stars with
M > 0.85 Msun the rotation periods, vsini and radius estimates are
consistent with the stars having an isotropic distribution of rotation
axes, if a moderate differential rotation law is assumed. For stars
with M < 0.85 Msun the inferred sini values are systematically
larger than 1.0. These observations imply that the combination of
measured parameters P(vsini)/R is too large by \sim 24% for low-mass
stars in this cluster. By comparing our new mass-period relation for
the Pleiades to the slightly older cluster M35, we confirm previous
indications that the spin-down stalls at \sim 100 Myr for the slowest
rotating stars with 0.7 Msun < M < 1.1 Msun a fact which may
indicate that the internal transport of angular momentum is inefficient
in slowly rotating solar mass stars.
---------------------------------------------------------
Title: HAT-P-14b: A 2.2 M <SUB>J</SUB> Exoplanet Transiting a Bright
F Star
Authors: Torres, G.; Bakos, G. Á.; Hartman, J.; Kovács, Géza;
Noyes, R. W.; Latham, D. W.; Fischer, D. A.; Johnson, J. A.; Marcy,
G. W.; Howard, A. W.; Sasselov, D. D.; Kipping, D.; Sipőcz, B.;
Stefanik, R. P.; Esquerdo, G. A.; Everett, M. E.; Lázár, J.; Papp,
I.; Sári, P.
2010ApJ...715..458T Altcode: 2010arXiv1003.2211T
We report the discovery of HAT-P-14b, a fairly massive transiting
extrasolar planet orbiting the moderately bright star GSC 3086-00152
(V = 9.98), with a period of P = 4.627669 ± 0.000005 days. The
transit is close to grazing (impact parameter 0.891<SUP>+0.007</SUP>
<SUB>-0.008</SUB>) and has a duration of 0.0912 ± 0.0017 days,
with a reference epoch of mid-transit of T<SUB>c</SUB> = 2, 454,
875.28938 ± 0.00047 (BJD). The orbit is slightly eccentric (e =
0.107 ± 0.013), and the orientation is such that occultations are
unlikely to occur. The host star is a slightly evolved mid-F dwarf
with a mass of 1.386 ± 0.045 M <SUB>sun</SUB>, a radius of 1.468
± 0.054 R <SUB>sun</SUB>, effective temperature 6600 ± 90 K, and
a slightly metal-rich composition corresponding to [Fe/H] = +0.11
± 0.08. The planet has a mass of 2.232 ± 0.059 M <SUB>J</SUB> and
a radius of 1.150 ± 0.052 R <SUB>J</SUB>, implying a mean density
of 1.82 ± 0.24 g cm<SUP>-3</SUP>. Its radius is well reproduced by
theoretical models for the 1.3 Gyr age of the system if the planet has
a heavy-element fraction of about 50 M <SUB>⊕</SUB> (7% of its total
mass). The brightness, near-grazing orientation, and other properties
of HAT-P-14 make it a favorable transiting system to look for changes in
the orbital elements or transit timing variations induced by a possible
second planet, and also to place meaningful constraints on the presence
of sub-Earth mass or Earth-mass exomoons, by monitoring it for transit
duration variations. <P />Based in part on observations obtained at
the W. M. Keck Observatory, which is operated by the University of
California and the California Institute of Technology.
---------------------------------------------------------
Title: The Asteroseismic Potential of Kepler: First Results for
Solar-Type Stars
Authors: Chaplin, W. J.; Appourchaux, T.; Elsworth, Y.; García,
R. A.; Houdek, G.; Karoff, C.; Metcalfe, T. S.; Molenda-Żakowicz,
J.; Monteiro, M. J. P. F. G.; Thompson, M. J.; Brown, T. M.;
Christensen-Dalsgaard, J.; Gilliland, R. L.; Kjeldsen, H.; Borucki,
W. J.; Koch, D.; Jenkins, J. M.; Ballot, J.; Basu, S.; Bazot, M.;
Bedding, T. R.; Benomar, O.; Bonanno, A.; Brandão, I. M.; Bruntt,
H.; Campante, T. L.; Creevey, O. L.; Di Mauro, M. P.; Doǧan,
G.; Dreizler, S.; Eggenberger, P.; Esch, L.; Fletcher, S. T.;
Frandsen, S.; Gai, N.; Gaulme, P.; Handberg, R.; Hekker, S.; Howe,
R.; Huber, D.; Korzennik, S. G.; Lebrun, J. C.; Leccia, S.; Martic,
M.; Mathur, S.; Mosser, B.; New, R.; Quirion, P. -O.; Régulo, C.;
Roxburgh, I. W.; Salabert, D.; Schou, J.; Sousa, S. G.; Stello, D.;
Verner, G. A.; Arentoft, T.; Barban, C.; Belkacem, K.; Benatti, S.;
Biazzo, K.; Boumier, P.; Bradley, P. A.; Broomhall, A. -M.; Buzasi,
D. L.; Claudi, R. U.; Cunha, M. S.; D'Antona, F.; Deheuvels, S.;
Derekas, A.; García Hernández, A.; Giampapa, M. S.; Goupil, M. J.;
Gruberbauer, M.; Guzik, J. A.; Hale, S. J.; Ireland, M. J.; Kiss,
L. L.; Kitiashvili, I. N.; Kolenberg, K.; Korhonen, H.; Kosovichev,
A. G.; Kupka, F.; Lebreton, Y.; Leroy, B.; Ludwig, H. -G.; Mathis, S.;
Michel, E.; Miglio, A.; Montalbán, J.; Moya, A.; Noels, A.; Noyes,
R. W.; Pallé, P. L.; Piau, L.; Preston, H. L.; Roca Cortés, T.;
Roth, M.; Sato, K. H.; Schmitt, J.; Serenelli, A. M.; Silva Aguirre,
V.; Stevens, I. R.; Suárez, J. C.; Suran, M. D.; Trampedach, R.;
Turck-Chièze, S.; Uytterhoeven, K.; Ventura, R.; Wilson, P. A.
2010ApJ...713L.169C Altcode: 2010arXiv1001.0506C
We present preliminary asteroseismic results from Kepler on three G-type
stars. The observations, made at one-minute cadence during the first
33.5 days of science operations, reveal high signal-to-noise solar-like
oscillation spectra in all three stars: about 20 modes of oscillation
may be clearly distinguished in each star. We discuss the appearance of
the oscillation spectra, use the frequencies and frequency separations
to provide first results on the radii, masses, and ages of the stars,
and comment in the light of these results on prospects for inference
on other solar-type stars that Kepler will observe.
---------------------------------------------------------
Title: HAT-P-11b: A Super-Neptune Planet Transiting a Bright K Star
in the Kepler Field
Authors: Bakos, G. Á.; Torres, G.; Pál, A.; Hartman, J.; Kovács,
Géza; Noyes, R. W.; Latham, D. W.; Sasselov, D. D.; Sipőcz, B.;
Esquerdo, G. A.; Fischer, D. A.; Johnson, J. A.; Marcy, G. W.; Butler,
R. P.; Isaacson, H.; Howard, A.; Vogt, S.; Kovács, Gábor; Fernandez,
J.; Moór, A.; Stefanik, R. P.; Lázár, J.; Papp, I.; Sári, P.
2010ApJ...710.1724B Altcode: 2009arXiv0901.0282B
We report on the discovery of HAT-P-11b, the smallest radius transiting
extrasolar planet (TEP) discovered from the ground, and the first
hot Neptune discovered to date by transit searches. HAT-P-11b orbits
the bright (V = 9.587) and metal rich ([Fe/H] = +0.31 ± 0.05) K4
dwarf star GSC 03561-02092 with P = 4.8878162 ± 0.0000071 days and
produces a transit signal with depth of 4.2 mmag, the shallowest found
by transit searches that is due to a confirmed planet. We present a
global analysis of the available photometric and radial velocity (RV)
data that result in stellar and planetary parameters, with simultaneous
treatment of systematic variations. The planet, like its near-twin
GJ 436b, is somewhat larger than Neptune (17 M <SUB>⊕</SUB>,
3.8 R <SUB>⊕</SUB>) both in mass M<SUB>p</SUB> = 0.081 ± 0.009 M
<SUB>J</SUB>(25.8 ± 2.9 M <SUB>⊕</SUB>) and radius R<SUB>p</SUB> =
0.422 ± 0.014 R <SUB>J</SUB>(4.73 ± 0.16 R <SUB>⊕</SUB>). HAT-P-11b
orbits in an eccentric orbit with e = 0.198 ± 0.046 and ω = 355fdg2
± 17fdg3, causing a reflex motion of its parent star with amplitude
11.6 ± 1.2 m s<SUP>-1</SUP>, a challenging detection due to the high
level of chromospheric activity of the parent star. Our ephemeris for
the transit events is T<SUB>c</SUB> = 2454605.89132 ± 0.00032 (BJD),
with duration 0.0957 ± 0.0012 days, and secondary eclipse epoch of
2454608.96 ± 0.15 days (BJD). The basic stellar parameters of the host
star are M <SUB>sstarf</SUB> = 0.809<SUP>+0.020</SUP> <SUB>-0.027</SUB>
M <SUB>sun</SUB>, R <SUB>sstarf</SUB> = 0.752 ± 0.021 R <SUB>sun</SUB>,
and T <SUB>effsstarf</SUB> = 4780 ± 50 K. Importantly, HAT-P-11 will
lie on one of the detectors of the forthcoming Kepler mission; this
should make possible fruitful investigations of the detailed physical
characteristic of both the planet and its parent star at unprecedented
precision. We discuss an interesting constraint on the eccentricity
of the system by the transit light curve and stellar parameters. This
will be particularly useful for eccentric TEPs with low-amplitude
RV variations in Kepler's field. We also present a blend analysis,
that for the first time treats the case of a blended transiting hot
Jupiter mimicking a transiting hot Neptune, and proves that HAT-P-11b
is not such a blend. <P />Based in part on observations obtained at
the W. M. Keck Observatory, which is operated by the University of
California and the California Institute of Technology. Keck time has
been granted by NOAO (A285Hr) and NASA (N128Hr).
---------------------------------------------------------
Title: Refined stellar, orbital and planetary parameters of the
eccentric HAT-P-2 planetary system
Authors: Pál, András; Bakos, Gáspár Á.; Torres, Guillermo; Noyes,
Robert W.; Fischer, Debra A.; Johnson, John A.; Henry, Gregory W.;
Butler, R. Paul; Marcy, Geoffrey W.; Howard, Andrew W.; Sipőcz,
Brigitta; Latham, David W.; Esquerdo, Gilbert A.
2010MNRAS.401.2665P Altcode: 2009arXiv0908.1705P; 2009MNRAS.tmp.1781P
We present refined parameters for the extrasolar planetary system
HAT-P-2 (also known as HD147506), based on new radial velocity and
photometric data. HAT-P-2b is a transiting extrasolar planet that
exhibits an eccentric orbit. We present a detailed analysis of the
planetary and stellar parameters, yielding consistent results for
the mass and radius of the star, better constraints on the orbital
eccentricity and refined planetary parameters. The improved parameters
for the host star are M<SUB>*</SUB> = 1.36 +/- 0.04M<SUB>solar</SUB>
and R<SUB>*</SUB> = 1.64 +/- 0.08 R<SUB>solar</SUB>, while the planet
has a mass of M<SUB>p</SUB> = 9.09 +/- 0.24M<SUB>Jup</SUB> and radius
of R<SUB>p</SUB> = 1.16 +/- 0.08R<SUB>Jup</SUB>. The refined transit
epoch and period for the planet are E = 2454387.49375 +/- 0.00074(BJD)
and P = 5.6334729 +/- 0.0000061(d), and the orbital eccentricity and
argument of periastron are e = 0.5171 +/- 0.0033 and . These orbital
elements allow us to predict the timings of secondary eclipses with
a reasonable accuracy of ~15min. We also discuss the effects of this
significant eccentricity including the characterization of the asymmetry
in the transit light curve. Simple formulae are presented for the above,
and these, in turn, can be used to constrain the orbital eccentricity
using purely photometric data. These will be particularly useful for
very high precision, space-borne observations of transiting planets.
---------------------------------------------------------
Title: HAT-P-13b,c: A Transiting Hot Jupiter with a Massive Outer
Companion on an Eccentric Orbit
Authors: Bakos, G. Á.; Howard, A. W.; Noyes, R. W.; Hartman, J.;
Torres, G.; Kovács, Géza; Fischer, D. A.; Latham, D. W.; Johnson,
J. A.; Marcy, G. W.; Sasselov, D. D.; Stefanik, R. P.; Sipőcz, B.;
Kovács, Gábor; Esquerdo, G. A.; Pál, A.; Lázár, J.; Papp, I.;
Sári, P.
2009ApJ...707..446B Altcode: 2009arXiv0907.3525B
We report on the discovery of a planetary system with a close-in
transiting hot Jupiter on a near circular orbit and a massive outer
planet on a highly eccentric orbit. The inner planet, HAT-P-13b,
transits the bright V = 10.622 G4 dwarf star GSC 3416 - 00543 every
P = 2.916260 ± 0.000010 days, with transit epoch T<SUB>c</SUB>
= 2454779.92979 ± 0.00038 (BJD) and duration 0.1345 ± 0.0017
days. The outer planet HAT-P-13c orbits the star every P <SUB>2</SUB>
= 428.5 ± 3.0 days with a nominal transit center (assuming zero
impact parameter) of T <SUB>2c </SUB> = 2454870.4 ± 1.8 (BJD) or
time of periastron passage T <SUB>2,peri</SUB> = 2454890.05 ± 0.48
(BJD). Transits of the outer planet have not been observed, and may
not be present. The host star has a mass of 1.22<SUP>+0.05</SUP>
<SUB>-0.10</SUB> M <SUB>sun</SUB>, radius of 1.56 ± 0.08 R
<SUB>sun</SUB>, effective temperature of 5653 ± 90 K, and is rather
metal-rich with [Fe/H] = +0.41 ± 0.08. The inner planetary companion
has a mass of 0.853<SUP>+0.029</SUP> <SUB>-0.046</SUB> M <SUB>J</SUB>,
and radius of 1.281 ± 0.079 R <SUB>J</SUB>, yielding a mean density
of 0.498<SUP>+0.103</SUP> <SUB>-0.069</SUB> g cm<SUP>-3</SUP>. The
outer companion has m <SUB>2</SUB>sin i <SUB>2</SUB> = 15.2 ± 1.0 M
<SUB>J</SUB>, and orbits on a highly eccentric orbit of e <SUB>2</SUB>
= 0.691 ± 0.018. While we have not detected significant transit timing
variations of HAT-P-13b, due to gravitational and light-travel time
effects, future observations will constrain the orbital inclination
of HAT-P-13c, along with its mutual inclination to HAT-P-13b. The
HAT-P-13 (b, c) double-planet system may prove extremely valuable
for theoretical studies of the formation and dynamics of planetary
systems. <P />Based in part on observations obtained at the W. M. Keck
Observatory, which is operated by the University of California and the
California Institute of Technology. Keck time has been granted by NOAO
(A146Hr,A264Hr) and NASA (N128Hr,N145Hr).
---------------------------------------------------------
Title: HAT-P-12b: A Low-Density Sub-Saturn Mass Planet Transiting
a Metal-Poor K Dwarf
Authors: Hartman, J. D.; Bakos, G. Á.; Torres, G.; Kovács, Géza;
Noyes, R. W.; Pál, A.; Latham, D. W.; Sipőcz, B.; Fischer, D. A.;
Johnson, J. A.; Marcy, G. W.; Butler, R. P.; Howard, A. W.; Esquerdo,
G. A.; Sasselov, D. D.; Kovács, Gábor; Stefanik, R. P.; Fernandez,
J. M.; Lázár, J.; Papp, I.; Sári, P.
2009ApJ...706..785H Altcode: 2009arXiv0904.4704H
We report on the discovery of HAT-P-12b, a transiting extrasolar planet
orbiting the moderately bright V ≈ 12.8 K4 dwarf GSC 03033 - 00706,
with a period P = 3.2130598 ± 0.0000021 d, transit epoch T<SUB>c</SUB>
= 2454419.19556 ± 0.00020 (BJD), and transit duration 0.0974 ±
0.0006 d. The host star has a mass of 0.73 ± 0.02 M <SUB>sun</SUB>,
radius of 0.70<SUP>+0.02</SUP> <SUB>-0.01</SUB> R <SUB>sun</SUB>,
effective temperature 4650 ± 60 K, and metallicity [Fe/H] = -0.29
± 0.05. We find a slight correlation between the observed spectral
line bisector spans and the radial velocity, so we consider, and rule
out, various blend configurations including a blend with a background
eclipsing binary, and hierarchical triple systems where the eclipsing
body is a star or a planet. We conclude that a model consisting of
a single star with a transiting planet best fits the observations,
and show that a likely explanation for the apparent correlation
is contamination from scattered moonlight. Based on this model,
the planetary companion has a mass of 0.211 ± 0.012 M <SUB>J</SUB>
and radius of 0.959<SUP>+0.029</SUP> <SUB>-0.021</SUB> R <SUB>J</SUB>
yielding a mean density of 0.295 ± 0.025 g cm<SUP>-3</SUP>. Comparing
these observations with recent theoretical models, we find that
HAT-P-12b is consistent with a ~1-4.5 Gyr, mildly irradiated,
H/He-dominated planet with a core mass M<SUB>C</SUB> lsim 10 M
<SUB>⊕</SUB>. HAT-P-12b is thus the least massive H/He-dominated
gas giant planet found to date. This record was previously held by
Saturn. <P />Based in part on observations obtained at the W. M. Keck
Observatory, which is operated by the University of California and the
California Institute of Technology. Keck time has been granted by NOAO
(A264Hr, A146Hr) and NASA (N162Hr, N128Hr).
---------------------------------------------------------
Title: Discovery of a Transiting Planet and Eight Eclipsing Binaries
in HATNet Field G205
Authors: Latham, David W.; Bakos, Gáspár Á.; Torres, Guillermo;
Stefanik, Robert P.; Noyes, Robert W.; Kovács, Géza; Pál, András;
Marcy, Geoffrey W.; Fischer, Debra A.; Butler, R. Paul; Sipőcz,
Brigitta; Sasselov, Dimitar D.; Esquerdo, Gilbert A.; Vogt, Steven S.;
Hartman, Joel D.; Kovács, Gábor; Lázár, József; Papp, István;
Sári, Pál
2009ApJ...704.1107L Altcode: 2008arXiv0812.1161L
We report the discovery of HAT-P-8b, a transiting planet with mass M
<SUB>p</SUB> = 1.52<SUP>+0.18</SUP> <SUB>-0.16</SUB> M <SUB>J</SUB>,
radius R <SUB>p</SUB> = 1.50<SUP>+0.08</SUP> <SUB>-0.06</SUB>
R <SUB>J</SUB>, and photometric period P = 3.076 days. HAT-P-8b
has a somewhat inflated radius for its mass, and a somewhat large
mass for its period. The host star is a solar-metallicity F dwarf,
with mass M <SUB>sstarf</SUB> = 1.28 ± 0.04 M <SUB>sun</SUB>
and R <SUB>sstarf</SUB> = 1.58<SUP>+0.08</SUP> <SUB>-0.06</SUB>
R <SUB>sun</SUB>. HAT-P-8b was initially identified as one of the
32 transiting-planet candidates in HATNet field G205. We describe
the procedures that we have used to follow up these candidates with
spectroscopic and photometric observations, and we present a status
report on our interpretation for 28 of the candidates. Eight are
eclipsing binaries with orbital solutions whose periods are consistent
with their photometric ephemerides; two of these spectroscopic
orbits are single-lined and six are double-lined. <P />Based in part
on observations obtained at the W. M. Keck Observatory, which is
operated by the University of California and the California Institute
of Technology. Keck time has been granted by NOAO (A285Hr).
---------------------------------------------------------
Title: Independent Confirmation and Refined Parameters of the Hot
Jupiter XO-5b
Authors: Pál, A.; Bakos, G. Á.; Fernandez, J.; Sipőcz, B.; Torres,
G.; Latham, D. W.; Kovács, Géza; Noyes, R. W.; Marcy, G. W.; Fischer,
D. A.; Butler, R. P.; Sasselov, D. D.; Esquerdo, G. A.; Shporer, A.;
Mazeh, T.; Stefanik, R. P.; Isaacson, H.
2009ApJ...700..783P Altcode: 2008arXiv0810.0260P
We present HATNet observations of XO-5b, confirming its planetary
nature based on evidence beyond that described in the announcement
of Burke et al., namely, the lack of significant correlation between
spectral bisector variations and orbital phase. In addition, using
extensive spectroscopic measurements spanning multiple seasons,
we investigate the relatively large scatter in the spectral line
bisectors. We also examine possible blended stellar configurations
(hierarchical triples, chance alignments) that can mimic the planet
signals, and we are able to show that none are consistent with the
sum of all the data. The analysis of the S activity index shows no
significant stellar activity. Our results for the planet parameters
are consistent with values in Burke et al., and we refine both the
stellar and the planetary parameters using our data. XO-5b orbits a
slightly evolved, late G type star with mass M <SUB>sstarf</SUB> =
0.88 ± 0.03 M <SUB>sun</SUB>, radius R <SUB>sstarf</SUB> = 1.08 ±
0.04 R <SUB>sun</SUB>, and metallicity close to solar. The planetary
mass and radius are 1.059 ± 0.028 M <SUB>J</SUB> and 1.109 ± 0.050
R <SUB>J</SUB>, respectively, corresponding to a mean density of
0.96_{-0.11}^{+0.14} g cm^{-3}. The ephemeris for the orbit is P =
4.187757 ± 0.000011 days, E = 2454552.67168 ± 0.00029 (BJD) with
transit duration of 0.1307 ± 0.0013 days. By measuring four individual
transit centers, we found no signs for transit timing variations. The
planet XO-5b is notable for its anomalously high Safronov number and
has a high surface gravity when compared to other transiting exoplanets
with similar period. <P />Based in part on observations obtained at
the W. M. Keck Observatory, which is operated by the University of
California and the California Institute of Technology. Keck time has
been granted by NOAO and NASA (programs N162Hr, N128Hr, and A264Hr).
---------------------------------------------------------
Title: HAT-P-10b: A Light and Moderately Hot Jupiter Transiting A
K Dwarf
Authors: Bakos, G. Á.; Pál, A.; Torres, G.; Sipőcz, B.; Latham,
D. W.; Noyes, R. W.; Kovács, Géza; Hartman, J.; Esquerdo, G. A.;
Fischer, D. A.; Johnson, J. A.; Marcy, G. W.; Butler, R. P.; Howard,
A. W.; Sasselov, D. D.; Kovács, Gábor; Stefanik, R. P.; Lázár,
J.; Papp, I.; Sári, P.
2009ApJ...696.1950B Altcode: 2008arXiv0809.4295B
We report on the discovery of HAT-P-10b, one of the lowest mass
(0.487 ± 0.018 M <SUB>J</SUB>) transiting extrasolar planets (TEPs)
discovered to date by transit searches. HAT-P-10b orbits the moderately
bright V = 11.89 K dwarf GSC 02340-01714, with a period P = 3.7224747 ±
0.0000065 days, transit epoch T<SUB>c</SUB> = 2454759.68683 ± 0.00016
(BJD), and duration 0.1090 ± 0.0008 days. HAT-P-10b has a radius
of 1.005<SUP>+0.032</SUP> <SUB>-0.027</SUB> R <SUB>J</SUB> yielding
a mean density of 0.594 ± 0.052 g cm<SUP>-3</SUP>. Comparing these
observations with recent theoretical models we find that HAT-P-10b is
consistent with a ~4.5 Gyr, almost pure hydrogen and helium gas giant
planet with a 10 M <SUB>⊕</SUB> core. With an equilibrium temperature
of T <SUB>eq</SUB> = 1020 ± 17 K, HAT-P-10b is one of the coldest
TEPs. Curiously, its Safronov number θ = 0.053 ± 0.002 falls close
to the dividing line between the two suggested TEP populations. <P
/>Based in part on observations obtained at the W. M. Keck Observatory,
which is operated by the University of California and the California
Institute of Technology. Keck time has been granted by NOAO (A285Hr)
and NASA (N128Hr).
---------------------------------------------------------
Title: Exoplanet HAT-P-11b Secondary Transit Observations
Authors: Barry, Richard; Deming, Drake; Bakos, Gaspar; Deming,
L. Drake; Harrington, Joseph; Madhusudhan, Nikku; Noyes, Robert;
Seager, Sarah
2009sptz.prop60063B Altcode:
We propose to conduct secondary eclipse observations of exoplanet
HAT-P-11b, recently discovered by proposal Co-Investigator G. Bakos
and his colleagues. HAT-P-11b is the smallest transiting extrasolar
planet yet found and one of only two known exo-Neptunes. We will
observe the system at 3.6 microns for a period of 22 hours centered
on the anticipated secondary eclipse time, to detect the eclipse
and determine its phase. Once the secondary eclipse is located, we
will make a more focused series of observations in both the 3.6 and
4.5 micron bands to fully characterize it. HAT-P-11b has a period of
4.8878 days, radius of 0.422 RJ, mass of 0.081 MJ and semi-major axis
0.053 AU. Measurements of the secondary eclipse will clarify two key
issues; 1) the planetary brightness temperature and the nature of its
atmosphere, and 2) the eccentricity of its orbit, with implications
for its dynamical evolution. A precise determination of the orbit
phase for the secondary eclipse will also be of great utility for
Kepler observations of this system at visible wavelengths.
---------------------------------------------------------
Title: Determination of stellar, orbital and planetary parameters
using complete Monte-Carlo analysis the case of HAT-P-7b
Authors: Pál, András; Bakos, Gáspár Á.; Noyes, Robert W.;
Torres, Guillermo
2009IAUS..253..428P Altcode: 2008arXiv0807.1530P
The recently discovered transiting very hot Jupiter, HAT-P-7b, a
planet detected by the telescopes of HATNet, turned out to be among
the ones subjected to the highest irradiation from the parent star. In
order to best characterize this particular planet, we carried out an
analysis based on a complete and simultaneous Monte-Carlo solution
using all available data. We included the discovery light curves,
partial follow-up light curves, the radial velocity data, and we used
the stellar evolution models to infer the stellar properties. <P />This
self-consistent way of modeling provides the most precise estimate
of the a posteriori distributions of all of the system parameters of
interest, and avoids making assumptions on the values and uncertainties
of any of the internally derived variables describing the system. This
analysis demonstrates that even partial light curve information can
be valuable. This may become very important for future discoveries
of planets with longer periods and therefore longer transit durations
where the chance of observing a full event is small.
---------------------------------------------------------
Title: Search for Transiting Exoplanets with HATNet
Authors: Bakos, G. Á.; Noyes, R. W.; Kovács, G.; Latham, D. W.;
Torres, G.; Sasselov, D.; Pál, A.; Sipőcz, B.; Kovács, Gábor
2009IAUS..253...21B Altcode:
HATNet is a network of six identical, fully automated wide field
telescopes, four of which are located in Arizona, and two at
Hawaii. The purpose of the network is to search for transiting
extrasolar planets around relatively bright stars (8 < I <
12). The longitudinal coverage of 3.5 hours greatly enhances transit
detection efficiency. HATNet has been operational since 2004, and has
taken more than 1/2 million science frames at 5-min integrations,
covering about 7% of the sky. Photometric precision reaches 3mmag
rms at 5.5 min cadence at I ≈ 8, and is 1% at I ≈ 11.3. Hundreds
of transit candidates have been detected in the data, and have been
subject to vigorous follow-up by various 1m-class facilities, both
spectroscopy and follow-up photometry. A fraction of the candidates
that have survived these steps as not being false alarms have been
observed by high resolution and precision spectrographs (primarily
Keck/HIRES), to confirm their planetary nature and characterize their
properties. So far nine transiting planets have been reported, making
HATNet a very successful survey.
---------------------------------------------------------
Title: HAT-South: A Global Network of Southern Hemisphere Automated
Telescopes to Detect Transiting Exoplanets
Authors: Bakos, G.; Afonso, C.; Henning, T.; Jordán, A.; Holman, M.;
Noyes, R. W.; Sackett, P. D.; Sasselov, D.; Kovács, Gábor; Csubry,
Z.; Pál, A.
2009IAUS..253..354B Altcode:
HAT-South is a network of six identical, fully automated wide field
telescopes, to be located at three sites (Chile: Las Campanas,
Australia: Siding Springs, and Namibia: HESS site) in the Southern
hemisphere. The primary purpose of the network is to detect and
characterize a large number of extra-solar planets transiting nearby
bright stars, and to explore their diversity. Operation of HAT-South is
a collaboration among the Harvard-Smithsonian Center for Astrophysics
(CfA), Max Planck Institute for Astronomy (MPIA) and the Australian
National University (ANU). The network is expected to be ready for
initial science operations in 2009. The three sites will permit near
round-the-clock monitoring of selected fields, and the continuous
data-stream will greatly enhance recovery of transits. HAT-South
will be sensitive to planetary transits down to R≈14 across a 128
square-degrees combined field of view, thereby targeting a large number
of dwarfs with feasible confirmation-mode follow-up. We anticipate a
yearly detection rate of approximately 25 planets transiting bright
stars.
---------------------------------------------------------
Title: Obituary: Edmond M. Reeves, 1934-2008
Authors: Noyes, Robert; Parkinson, William
2009BAAS...41..576N Altcode:
With great sadness we report that Edmond (Ed) M. Reeves, a former
leader of solar space research projects at Harvard College Observatory
[HCO] and the Harvard-Smithsonian Center for Astrophysics [CfA], died
on 8 August 2008, in Arlington, Virginia, after a long and heroic
struggle with cancer. <P />Ed was born in London, Ontario, Canada,
on 14 January 1934. During his undergraduate and graduate years at the
University of Western Ontario [UWO], he was in the Royal Canadian Navy
(Reserve) as a Cadet (1952-1956), then as Instructing Officer, HMCS
Prevost (1956-1959), and Lieutenant, Royal Canadian Navy (Reserve)
retired. He received a Ph.D. in 1959 from the UWO, specializing in
atomic and molecular physics. After two years of postdoctoral research
in ultraviolet atomic spectroscopy at the Department of Physics,
Imperial College, London, England, Ed joined the HCO Solar Satellite
project, working with Leo Goldberg, Director of HCO, and pioneer in
solar spectroscopy. <P />In 1968, Ed was appointed Senior Research
Associate at HCO, and in 1973 he received a joint appointment as
Physicist at the Smithsonian Astrophysical Observatory [SAO] when the
CfA was initiated under George Field. During his seventeen years at
the Observatory, Ed led a large and vibrant group of engineers and
scientists in the Solar Satellite Project, developing a series of
space missions to explore the extreme ultraviolet emission from the
Sun. <P />Ed also maintained his interest and research in laboratory
atomic and molecular astrophysics and enjoyed a vigorous involvement
in the HCO Shock Tube Laboratory. In the early 1960s, in the area of
molecular spectroscopy, Ed and Bill Parkinson photographed the vacuum
ultraviolet absorption spectrum of CO (the Fourth Positive system),
which was produced at high temperature in a shock tube. This laboratory
spectrum shortly led to the discovery of CO as an important source
of opacity in the solar ultraviolet. Goldberg, who first identified
CO vibration-rotation bands in the infrared solar spectrum in 1951,
recognized at around 180 nm the prominent CO features in the shock tube
spectra and in the solar spectra. The identification was confirmed by
comparing the high-temperature laboratory spectra with published solar
spectra taken by the Naval Research Laboratory with a rocket-borne
spectrograph. <P />Ed's work for the Solar Satellite Project included
planning and carrying out laboratory, Vacuum UV absolute-intensity
calibrations of the early rocket and satellite spectrometers. He
set the requirement that the solar spectroscopic instruments have
radiometric calibrations in the Vacuum UV, traceable to a laboratory
standard. <P />The space missions began with rocket experiments in
the early 1960s, progressed to the Orbiting Solar Observatory [OSO]
program in the mid-1960s, and culminated in the Extreme Ultraviolet
Spectroheliometer on the Apollo Telescope Mount [ATM] of the Skylab
missions in 1973 and 1974. Ed received NASA's Exceptional Scientific
Achievement Medal in 1974. This sequence of space instruments laid much
of the early groundwork for our current understanding of the outer solar
atmosphere. For example, the OSO observations revealed for the first
time coronal "holes," which we now know are the seat of the fast solar
wind. <P />Another experiment of particular interest and importance
to solar physics resulted from the launch of a rocket-borne objective
grating spectrograph into the path of totality of a solar eclipse from
Wallops Island, Virginia, on 7 March 1970. This lucky "rocket group"
included Ralph Nicholls from York University, Canada; Reg Garton and
Bob Speer from Imperial College, London; Bob Wilson, then from Culham
in the UK; and, of course, Leo Goldberg and colleagues from HCO, a group
made up of mentors, advisors, teachers, and friends of Ed's. The eclipse
spectrogram revealed strong emission from neutral hydrogen (Lyman-alpha)
in the solar corona. The discovery of the Lyman-alpha corona inspired
the project for a Lyman-alpha coronagraph. At a Retirement Symposium
dedicated to Ralph Nicholls in 1992, Ed recalled that at a coffee break
about twenty years earlier, during the Skylab program at Houston, he,
Bob Noyes, and Bob MacQueen outlined the need to develop a rocket-borne
coronagraph to observe the hydrogen Lyman-alpha corona. Later, after
returning to the CfA, Ed, Bob Noyes, and Bill Parkinson planned a
rocket-borne spectrograph to image the extended corona, expecting to use
a circular occulter. John Kohl joined the fledgling coronagraph project,
and he realized that a linear external occulter would be better and
also would match a spectrometer slit. This project became the origin of
the Lyman-Alpha Coronagraph series of rocket and Spacelab experiments
under John Kohl's leadership, culminating in the still-operating
Ultraviolet Coronagraph Spectrometer [UVCS] experiment on the SOHO
spacecraft. <P />In 1978, Ed joined the High Altitude Observatory in
Boulder, Colorado, where he was Head of Administration and Support
before moving to NASA Headquarters in 1982. There he became Director
of the Flight Systems Office in the Office of Life and Microgravity
Sciences and Applications, with responsibility for integrated planning
and science operations for research using the Spacelab, Spacehab, and
Mir missions. He led the activities for the research requirements and
planning for the International Space Station and served as the Space
Station Senior Scientist, the Executive Secretary of the Space Station
Utilization Advisory Subcommittee, and the Executive Secretary of the
Space Station Utilization Board at NASA Headquarters He also served
as NASA's representative to the international Users Operations Panel,
which coordinates the utilization planning for the Station across the
international partners. Ed retired from NASA in 1998. <P />Ed was an
outdoors man who enjoyed camping, canoeing, and cross-country skiing
with his family. He is survived by his wife Vivian, son Dr. Geoffrey
Reeves, daughter Laurie Webster, and three grandchildren. Ed's son Geoff
is Group Leader for Space Science and Atmospheric Science at Los Alamos
National Laboratory, Los Alamos, New Mexico. A funeral service took
place on Friday, 15 August at The Falls Church, Falls Church, Virginia.
---------------------------------------------------------
Title: HAT-P-9b: A Low-Density Planet Transiting a Moderately Faint
F Star
Authors: Shporer, Avi; Bakos, Gáspár Á.; Bouchy, Francois; Pont,
Frederic; Kovács, Géza; Latham, Dave W.; Sipöcz, Brigitta; Torres,
Guillermo; Mazeh, Tsevi; Esquerdo, Gilbert A.; Pál, András; Noyes,
Robert W.; Sasselov, Dimitar D.; Lázár, József; Papp, István;
Sári, Pál; Kovács, Gábor
2009ApJ...690.1393S Altcode: 2008arXiv0806.4008S
We report the discovery of a planet transiting a moderately faint (V =
12.3 mag) late F star, with an orbital period of 3.92289 ± 0.00004
days. From the transit light curve and radial velocity measurements,
we determine that the radius of the planet is R<SUB>p</SUB> = 1.40
± 0.06 R <SUB>Jup</SUB> and that the mass is M<SUB>p</SUB> = 0.78
± 0.09 M <SUB>Jup</SUB>. The density of the new planet, ρ<SUB>
p </SUB> = 0.35 ± 0.06 g cm<SUP>-3</SUP>, fits to the low-density
tail of the currently known transiting planets. We find that the
center of transit is at T <SUB>c</SUB> = 2454417.9077 ± 0.0003
(HJD), and the total transit duration is 0.143 ± 0.004 days. The
host star has M <SUB>sstarf</SUB> = 1.28 ± 0.13 M <SUB>sun</SUB>
and R <SUB>sstarf</SUB> = 1.32 ± 0.07 R <SUB>sun</SUB>. <P />Based in
part on radial velocities obtained with the SOPHIE spectrograph mounted
on the 1.93 m telescope at the Observatoire de Haute Provence, France
(runs 07A.PNP.MAZE, 07B.PNP.MAZE, 08A.PNP.MAZE).
---------------------------------------------------------
Title: NStED: Exo-Planet Transit Survey HATNet Search
Authors: Hartman, J. D.; Bakos, G. Á.; Noyes, R. W.; Sipöcz, B.;
Kovács, G.; Mazeh, T.; Shporer, A.; Pál, A.
2009nsted.cat....8H Altcode: 2009arXiv0907.2924H
Using light curves from the HATNet survey for transiting extrasolar
planets we investigate the optical broad-band photometric variability
of a sample of 27,560 field K and M dwarfs selected by color and
proper-motion. A total of 2120 stars exhibit potential variability,
including 95 stars with eclipses and 60 stars with flares. Based on
a visual inspection of these light curves and an automated blending
classification, we select 1568 stars, including 78 eclipsing binaries,
as secure variable star detections that are not obvious blends. We
estimate that a further ~26% of these stars may be blends with fainter
variables, though most of these blends are likely to be among the
hotter stars in our sample. We find that only 38 of the 1568 stars,
including 5 of the eclipsing binaries, have previously been identified
as variables or are blended with previously identified variables. One
of the newly identified eclipsing binaries is 1RXS J154727.5+450803,
a known P = 3.55 day, late M-dwarf SB2 system, for which we derive
preliminary estimates for the component masses and radii of M_1 =
M_2 = 0.258 +- 0.008 M_Sun and R_1 = R_2 = 0.289 +- 0.007 R_Sun. The
radii of the component stars are larger than theoretical expectations
if the system is older than ~200 Myr. The majority of the variables
are heavily spotted BY Dra-type stars for which we determine rotation
periods. Using this sample, we investigate the relations between period,
color, age, and activity measures, including optical flaring, for K and
M dwarfs., finding that many of the well-established relations for F,
G and K dwarfs continue into the M dwarf regime (Abridged).
---------------------------------------------------------
Title: Confirmation spectroscopy of HATNet transiting exoplanet
candidates using Keck-I/HIRES
Authors: Bakos, G.; Torres, G.; Latham, D.; Noyes, R.
2008noao.prop...99B Altcode:
Wide-field photometric observations of the HATNet project over the past
years, along with a massive follow-up effort, have produced dozens
of transiting exoplanet (TEP) candidates around bright (V<12.5)
stars. In order to confirm their planetary nature, along with accurate
initial characterization, they require high-precision radial velocity
observations and spectral-line bisector analysis. Based on Keck/HIRES
observations, seven of these candidates have been announced as TEPs
(HAT-P-1 through 7), 4 more have been verified and are being readied
for publication, and ~13 more remain strong candidates but need
more HIRES spectra for final confirmation, while ≳10 more await
initial HIRES observations. We expect an additional ~20 high quality
candidates to come out by mid-2008. Based on statistics to date,
60% of those subjected to HIRES observations have been identified as
hosting TEPs. We propose for 4 nights on Keck-I/HIRES for semester
2008B to finish pending candidates and also to analyze new targets. We
are confident that this effort will lead to the announcement of ≳12
new transiting exoplanets.
---------------------------------------------------------
Title: HAT-P-7b: An Extremely Hot Massive Planet Transiting a Bright
Star in the Kepler Field
Authors: Pál, A.; Bakos, G. Á.; Torres, G.; Noyes, R. W.; Latham,
D. W.; Kovács, Géza; Marcy, G. W.; Fischer, D. A.; Butler, R. P.;
Sasselov, D. D.; Sipőcz, B.; Esquerdo, G. A.; Kovács, Gábor;
Stefanik, R.; Lázár, J.; Papp, I.; Sári, P.
2008ApJ...680.1450P Altcode: 2008arXiv0803.0746P
We report on the latest discovery of the HATNet project: a very hot
giant planet orbiting a bright (V = 10.5) star with a small semimajor
axis of a = 0.0377 +/- 0.0005 AU. Ephemeris for the system is P =
2.2047299 +/- 0.0000040 days, midtransit time E = 2,453,790.2593 +/-
0.0010 (BJD). Based on the available spectroscopic data on the host star
and photometry of the system, the planet has a mass of M<SUB>p</SUB>
= 1.78<SUP>+ 0.08</SUP><SUB>-0.05</SUB> M<SUB>J</SUB> and radius of
R<SUB>p</SUB> = 1.36<SUP>+ 0.20</SUP><SUB>-0.09</SUB> R<SUB>J</SUB>. The
parent star is a slightly evolved F6 star with M<SUB>star</SUB> =
1.47<SUP>+ 0.08</SUP><SUB>-0.05</SUB> M<SUB>⊙</SUB>, R<SUB>star</SUB>
= 1.84<SUP>+ 0.23</SUP><SUB>-0.11</SUB> R<SUB>⊙</SUB>, T<SUB>eff</SUB>
= 6350 +/- 80 K, and metallicity [ Fe/H ] = + 0.26 +/- 0.08. The
relatively hot and large host star, combined with the close orbit
of the planet, yield a very high planetary irradiance of 4.71<SUP>+
1.44</SUP><SUB>-0.05</SUB> × 10<SUP>9</SUP> erg cm<SUP>-2</SUP>
s<SUP>-1</SUP>, which places the planet near the top of the pM class
of irradiated planets as defined by Fortney et al. If as predicted
by Fortney et al. the planet reradiates its absorbed energy before
distributing it to the night side, the day-side temperature should
be about 2730<SUP>+ 150</SUP><SUB>-100</SUB> K. Because the host
star is quite bright, measurement of the secondary eclipse should be
feasible for ground-based telescopes, providing a good opportunity
to compare the predictions of current hot Jupiter atmospheric models
with the observations. Moreover, the host star falls in the field of
the upcoming Kepler mission; hence extensive space-borne follow-up,
including not only primary transit and secondary eclipse observations
but also asteroseismology, will be possible. <P />Based in part
on observations obtained at the W. M. Keck Observatory, which is
operated by the University of California and the California Institute
of Technology. Keck time has been in part granted by NOAO.
---------------------------------------------------------
Title: HAT-P-6b: A Hot Jupiter Transiting a Bright F Star
Authors: Noyes, R. W.; Bakos, G. Á.; Torres, G.; Pál, A.; Kovács,
Géza; Latham, D. W.; Fernández, J. M.; Fischer, D. A.; Butler,
R. P.; Marcy, G. W.; Sipőcz, B.; Esquerdo, G. A.; Kovács, Gábor;
Sasselov, D. D.; Sato, B.; Stefanik, R.; Holman, M.; Lázár, J.;
Papp, I.; Sári, P.
2008ApJ...673L..79N Altcode: 2007arXiv0710.2894N
In the ongoing HATNet survey we have detected a giant planet,
with radius 1.33 ± 0.06 R<SUB>Jup</SUB> and mass 1.06 +/-
0.12 M<SUB>Jup</SUB>, transiting the bright (V = 10.5) star GSC
03239-00992. The planet is in a circular orbit with period 3.852985 +/-
0.000005 days and midtransit epoch 2,454,035.67575 ± 0.00028 (HJD). The
parent star is a late F star with mass 1.29 +/- 0.06 M<SUB>⊙</SUB>,
radius 1.46 +/- 0.06 R<SUB>⊙</SUB>, T<SUB>eff</SUB> ~ 6570 +/- 80 K ,
[ Fe/H ] = - 0.13 +/- 0.08, and age ~2.3<SUP>+ 0.5</SUP><SUB>-0.7</SUB>
Gyr. With this radius and mass, HAT-P-6b has somewhat larger radius
than theoretically expected. We describe the observations and their
analysis to determine physical properties of the HAT-P-6 system,
and briefly discuss some implications of this finding. <P />Based in
part on observations obtained at the W. M. Keck Observatory, which is
operated by the University of California and the California Institute
of Technology. Keck time has been in part granted by NASA (run N162Hr)
and NOAO (run A285Hr).
---------------------------------------------------------
Title: HAT-P-5b: A Jupiter-like Hot Jupiter Transiting a Bright Star
Authors: Bakos, G. Á.; Shporer, A.; Pál, A.; Torres, G.; Kovács,
Géza; Latham, D. W.; Mazeh, T.; Ofir, A.; Noyes, R. W.; Sasselov,
D. D.; Bouchy, F.; Pont, F.; Queloz, D.; Udry, S.; Esquerdo, G.;
Sipőcz, B.; Kovács, Gábor; Stefanik, R.; Lázár, J.; Papp, I.;
Sári, P.
2007ApJ...671L.173B Altcode: 2007arXiv0710.1841B
We report the discovery of a planet transiting a moderately bright
(V=12.00) G star, with an orbital period of 2.788491+/-0.000025
days. From the transit light curve we determine that the radius of
the planet is R<SUB>p</SUB>=1.257+/-0.053 R<SUB>J</SUB>. HAT-P-5b
has a mass of M<SUB>p</SUB>=1.06+/-0.11 M<SUB>J</SUB>, similar to
the average mass of previously known transiting exoplanets, and a
density of ρ<SUB>p</SUB>=0.66+/-0.11 g cm<SUP>-3</SUP>. We find that
the center of transit is T<SUB>c</SUB>=2,454,241.77663+/-0.00022 days
(HJD), and the total transit duration is 0.1217+/-0.0012 days. <P
/>Based in part on observations obtained with the SOPHIE spectrograph
mounted on the 1.93 m telescope at the Haute Provance Observatory.
---------------------------------------------------------
Title: HD 147506b: A Supermassive Planet in an Eccentric Orbit
Transiting a Bright Star
Authors: Bakos, G. Á.; Kovács, G.; Torres, G.; Fischer, D. A.;
Latham, D. W.; Noyes, R. W.; Sasselov, D. D.; Mazeh, T.; Shporer,
A.; Butler, R. P.; Stefanik, R. P.; Fernández, J. M.; Sozzetti,
A.; Pál, A.; Johnson, J.; Marcy, G. W.; Winn, J. N.; Sipőcz, B.;
Lázár, J.; Papp, I.; Sári, P.
2007ApJ...670..826B Altcode: 2007arXiv0705.0126B
We report the discovery of a massive (M<SUB>p</SUB>=9.04+/-0.50
M<SUB>J</SUB>) planet transiting the bright (V=8.7) F8 star
HD 147506, with an orbital period of 5.63341+/-0.00013 days
and an eccentricity of e=0.520+/-0.010. From the transit
light curve we determine that the radius of the planet
is R<SUB>p</SUB>=0.982<SUP>+0.038</SUP><SUB>-0.105</SUB>
R<SUB>J</SUB>. HD 147506b (also coined HAT-P-2b) has a mass about 9
times the average mass of previously known transiting exoplanets and
a density of ρ<SUB>p</SUB>~12 g cm<SUP>-3</SUP>, greater than that
of rocky planets like the Earth. Its mass and radius are marginally
consistent with theories of structure of massive giant planets
composed of pure H and He, and accounting for them may require a
large (>~100 M<SUB>⊕</SUB>) core. The high eccentricity causes
a ninefold variation of insolation of the planet between peri-
and apastron. Using follow-up photometry, we find that the center of
transit is T<SUB>mid</SUB>=2,454,212.8559+/-0.0007 (HJD) and the transit
duration is 0.177+/-0.002 days. <P />Some of the data presented herein
were obtained at the W. M. Keck Observatory, which is operated as a
scientific partnership among the California Institute of Technology,
the University of California, and the National Aeronautics and Space
Administration. The Observatory was made possible by the generous
financial support of the W. M. Keck Foundation. The authors wish to
recognize and acknowledge the very significant cultural role and
reverence that the summit of Mauna Kea has always had within the
indigenous Hawaiian community. We are most fortunate to have the
opportunity to conduct observations from this mountain. Keck time has
been in part granted by NASA.
---------------------------------------------------------
Title: HAT-P-4b: A Metal-rich Low-Density Transiting Hot Jupiter
Authors: Kovács, G.; Bakos, G. Á.; Torres, G.; Sozzetti, A.; Latham,
D. W.; Noyes, R. W.; Butler, R. P.; Marcy, G. W.; Fischer, D. A.;
Fernández, J. M.; Esquerdo, G.; Sasselov, D. D.; Stefanik, R. P.;
Pál, A.; Lázár, J.; Papp, I.; Sári, P.
2007ApJ...670L..41K Altcode: 2007arXiv0710.0602K
We describe the discovery of HAT-P-4b, a low-density extrasolar planet
transiting BD +36 2593, a V=11.2 mag slightly evolved metal-rich
late F star. The planet's orbital period is 3.056536+/-0.000057 days
with a midtransit epoch of 2,454,245.8154 +/- 0.0003 (HJD). Based on
high-precision photometric and spectroscopic data, and by using transit
light curve modeling, spectrum analysis, and evolutionary models, we
derive the following planet parameters: M<SUB>p</SUB>=0.68+/-0.04
M<SUB>J</SUB>, R<SUB>p</SUB>=1.27+/-0.05 R<SUB>J</SUB>,
ρ<SUB>p</SUB>=0.41+/-0.06 g cm<SUP>-3</SUP>, and a=0.0446+/-0.0012
AU. Because of its relatively large radius, together with its assumed
high metallicity (that of its parent star), this planet adds to the
theoretical challenges of explaining inflated extrasolar planets. <P
/>Based in part on observations obtained at the W. M. Keck Observatory,
which is operated by the University of California and the California
Institute of Technology. Keck time has been in part granted by NASA.
---------------------------------------------------------
Title: HAT-P-3b: A Heavy-Element-rich Planet Transiting a K Dwarf Star
Authors: Torres, G.; Bakos, G. Á.; Kovács, G.; Latham, D. W.;
Fernández, J. M.; Noyes, R. W.; Esquerdo, G. A.; Sozzetti, A.;
Fischer, D. A.; Butler, R. P.; Marcy, G. W.; Stefanik, R. P.; Sasselov,
D. D.; Lázár, J.; Papp, I.; Sári, P.
2007ApJ...666L.121T Altcode: 2007arXiv0707.4268T
We report the discovery of a Jupiter-size planet transiting a
relatively bright (V=11.56) and metal-rich early K dwarf star
with a period of ~2.9 days. On the basis of follow-up photometry
and spectroscopy we determine the mass and radius of the planet,
HAT-P-3b, to be M<SUB>p</SUB>=0.599+/-0.026 M<SUB>Jup</SUB> and
R<SUB>p</SUB>=0.890+/-0.046 R<SUB>Jup</SUB>. The relatively small
size of the object for its mass implies the presence of about 75
M<SUB>⊕</SUB> worth of heavy elements (~1/3 of the total mass)
based on current theories of irradiated extrasolar giant planets,
similar to the mass of the core inferred for the transiting
planet HD 149026b. The bulk density of HAT-P-3b is found to be
ρ<SUB>p</SUB>=1.06+/-0.17 g cm<SUP>-3</SUP>, and the planet orbits the
star at a distance of 0.03894 AU. Ephemerides for the transit centers
are T<SUB>c</SUB>=2,454,218.7594+/-0.0029+N×(2.899703+/-0.000054)
(HJD).
---------------------------------------------------------
Title: The Mass and Radius of the Unseen M Dwarf Companion in the
Single-Lined Eclipsing Binary HAT-TR-205-013
Authors: Beatty, Thomas G.; Fernández, José M.; Latham, David W.;
Bakos, Gáspár Á.; Kovács, Géza; Noyes, Robert W.; Stefanik,
Robert P.; Torres, Guillermo; Everett, Mark E.; Hergenrother, Carl W.
2007ApJ...663..573B Altcode: 2007arXiv0704.0059B
We derive masses and radii for both components in the single-lined
eclipsing binary HAT-TR-205-013, which consists of an F7 V primary
and a late M dwarf secondary. The system's period is short,
P=2.230736+/-0.000010 days, with an orbit indistinguishable from
circular, e=0.012+/-0.021. We demonstrate generally that the surface
gravity of the secondary star in a single-lined binary undergoing
total eclipses can be derived from characteristics of the light
curve and spectroscopic orbit. This constrains the secondary to
a unique line in the mass-radius diagram, with M/R<SUP>2</SUP> =
constant. For HAT-TR-205-013, we assume the orbit has been tidally
circularized and that the primary's rotation has been synchronized
and aligned with the orbital axis. Our observed line broadening,
V<SUB>rot</SUB>sini<SUB>rot</SUB>=28.9+/-1.0 km s<SUP>-1</SUP>, gives
a primary radius of R<SUB>A</SUB>=1.28+/-0.04 R<SUB>solar</SUB>. Our
light-curve analysis leads to the radius of the secondary,
R<SUB>B</SUB>=0.167+/-0.006 R<SUB>solar</SUB>, and the semimajor axis
of the orbit, a=7.54+/-0.30 R<SUB>solar</SUB>=0.0351+/-0.0014 AU. Our
single-lined spectroscopic orbit and the semimajor axis then yield
the individual masses M<SUB>B</SUB>=0.124+/-0.010 M<SUB>solar</SUB>
and M<SUB>A</SUB>=1.04+/-0.13 M<SUB>solar</SUB>. Our result for
HAT-TR-205-013 B lies above the theoretical mass-radius models from
the Lyon group, consistent with results from double-lined eclipsing
binaries. The method we describe offers the opportunity to study the
very low end of the stellar mass-radius relation.
---------------------------------------------------------
Title: HAT-P-2b: A Direct Glimpse at the Stormiest Exoplanet
Authors: Bakos, Gaspar; Charbonneau, David; Fischer, Debra; Holman,
Matthew; Laughlin, Gregory; Noyes, Robert; Sasselov, Dimitar
2007sptz.prop..297B Altcode:
The HATNet project has just discovered an unusual transiting exoplanet
(TEP), called HAT-P-2b (Bakos et al. 2007). This is the longest period
(Porb = 5.63 days), by far the most massive (Mp = 8MJ), most eccentric
(e = 0.5) and highest surface gravity (~ 149m s-2 ) TEP so far, and
it orbits a bright (K = 7.6) F8 star. The high eccentricity means that
the stellar distance during the orbit varies by a factor of 3, and the
stellar insolation by a factor 9. Another consequence of the strongly
varying angular orbital velocity is that the planet's spin period cannot
be synchronized with its orbit period. Instead, tidal evolution will
have brought it into spin-pseudo-synchronization in which it maintains
approximate co-rotation at periastron (with spin period Prot ~ 1.96
days). The orientation of the orbit, with its major axis in the sky
plane (omega ~ 180 deg) is very fortuitous. After the primary transit,
the planet reaches periastron in only 13 hours, and gets occulted by
the star in another 13 hours. At transit the insolation is ~1600 Solar
Constants (SC's); it more than doubles to 3600 SC's at periastron, then
drops back to 1600 SC's at secondary eclipse. The unique properties of
this object, along with the chance orientation of the orbit, combined
with large expected fluxes, make HAT-P-2b the stormiest exoplanet,
and the best of its kind for weather study by Spitzer. We propose to
take advantage of the fact that in just 34 hours - a small fraction
of the total orbital period - we can use the huge thermal forcing to
study the radiative response of the planetary atmosphere. Side-results
will be precise determinations of the orbital eccentricity, longitude
of periastron, and the planetary radius.
---------------------------------------------------------
Title: HAT-P-1b: A Large-Radius, Low-Density Exoplanet Transiting
One Member of a Stellar Binary
Authors: Bakos, G. Á.; Noyes, R. W.; Kovács, G.; Latham, D. W.;
Sasselov, D. D.; Torres, G.; Fischer, D. A.; Stefanik, R. P.; Sato,
B.; Johnson, J. A.; Pál, A.; Marcy, G. W.; Butler, R. P.; Esquerdo,
G. A.; Stanek, K. Z.; Lázár, J.; Papp, I.; Sári, P.; Sipőcz, B.
2007ApJ...656..552B Altcode: 2006astro.ph..9369B
Using small automated telescopes in Arizona and Hawaii, the HATNet
project has detected an object transiting one member of the double star
system ADS 16402. This system is a pair of G0 main-sequence stars with
age about 3 Gyr at a distance of ~139 pc and projected separation of
~1550 AU. The transit signal has a period of 4.46529 days and depth of
0.015 mag. From follow-up photometry and spectroscopy, we find that the
object is a “hot Jupiter” planet with mass about 0.53M<SUB>J</SUB>
and radius ~1.36R<SUB>J</SUB> traveling in an orbit with semimajor
axis 0.055 AU and inclination about 85.9°, thus transiting the
star at impact parameter 0.74 of the stellar radius. Based on a
data set spanning 3 yr, ephemerides for the transit center are
T<SUB>C</SUB>=2453984.397+N<SUB>tr</SUB>×4.46529. The planet,
designated HAT-P-1b, appears to be at least as large in radius, and
smaller in mean density, than any previously known planet. <P />Based
in part on data collected at the Subaru Telescope, which is operated
by the National Astronomical Observatory of Japan. <P />Based in
part on observations obtained at the W. M. Keck Observatory, which is
operated by the University of California and the California Institute
of Technology. Keck time has been granted by NASA.
---------------------------------------------------------
Title: Using Stellar Limb-Darkening to Refine the Properties of
HD 209458b
Authors: Knutson, Heather A.; Charbonneau, David; Noyes, Robert W.;
Brown, Timothy M.; Gilliland, Ronald L.
2007ApJ...655..564K Altcode: 2006astro.ph..3542K
We use multiband photometry to refine estimates for the planetary
radius and orbital inclination of the transiting planet system HD
209458. We gathered 1066 spectra over four distinct transits with the
STIS spectrometer on the Hubble Space Telescope using two gratings
with a resolution R=1500 and a combined wavelength range of 290-1030
nm. We divide the spectra into 10 spectrophotometric bandpasses,
five for each grating, of equal wavelength span within each grating,
and fit a transit curve over all bandpasses simultaneously. In our fit
we use theoretical values for the stellar limb-darkening to further
constrain the planetary radius. We find that the radius of HD 209458b is
(1.320+/-0.025)R<SUB>Jup</SUB>, which is a factor of 2 more precise
than current estimates. We also obtain improved estimates for the
orbital period P and time of center of transit T<SUB>C</SUB>. Although
in principle the photon-limited precision of the STIS data should allow
us to measure the timing of individual transits to a precision of 2-7 s,
we find that uncertainties in the stellar limb-darkening coefficients
and residual noise in the data degrade these measurements to a typical
precision of +/-14 s. Within this level of error, we find no significant
variations in the timing of the eight events examined in this work.
---------------------------------------------------------
Title: Refined Parameters of the Planet Orbiting HD 189733
Authors: Bakos, G. Á.; Knutson, H.; Pont, F.; Moutou, C.; Charbonneau,
D.; Shporer, A.; Bouchy, F.; Everett, M.; Hergenrother, C.; Latham,
D. W.; Mayor, M.; Mazeh, T.; Noyes, R. W.; Queloz, D.; Pál, A.;
Udry, S.
2006ApJ...650.1160B Altcode: 2006astro.ph..3291B
We report on the BVRI multiband follow-up photometry of the transiting
extrasolar planet HD 189733b. We revise the transit parameters and
find a planetary radius of R<SUB>P</SUB>=1.154+/-0.033R<SUB>J</SUB>
and an inclination of i<SUB>P</SUB>=85.79d+/-0.24d. The new density
(~1 g cm<SUP>-3</SUP>) is significantly higher than the former
estimate (~0.75 g cm<SUP>-3</SUP>) this shows that from the current
sample of nine transiting planets, only HD 209458 (and possibly
OGLE-10b) have anomalously large radii and low densities. We note
that due to the proximity of its parent star, HD 189733b currently
has one of the most precise radius determinations among extrasolar
planets. We calculate new ephemerides, P=2.218573+/-0.000020 days and
T<SUB>0</SUB>=2453629.39420+/-0.00024 (HJD), and estimate the timing
offsets of the 11 distinct transits with respect to the predictions
of a constant orbital period, which can be used to reveal the presence
of additional planets in the system.
---------------------------------------------------------
Title: A Stellar Companion in the HD 189733 System with a Known
Transiting Extrasolar Planet
Authors: Bakos, Gáspár Á.; Pál, András; Latham, David W.; Noyes,
Robert W.; Stefanik, Robert P.
2006ApJ...641L..57B Altcode: 2006astro.ph..2136B
We show that the very close-by (19 pc) K0 star HD 189733, already
found to be orbited by a transiting giant planet, is the primary of
a double star system, with the secondary being a mid-M dwarf with
projected separation of about 216 AU from the primary. This conclusion
is based on astrometry, proper-motion and radial velocity measurements,
spectral type determination, and photometry. We also detect differential
proper motion of the secondary. The data appear consistent with the
secondary's orbiting the primary in a clockwise orbit, lying nearly
in the plane of the sky (i.e., nearly perpendicular to the orbital
plane of the transiting planet), and with period of about 3200 years.
---------------------------------------------------------
Title: Extrasolar planet search with the HAT network
Authors: Bakos, G.; Noyes, R. W.; Latham, D. W.; Csák, B.; Gálfi,
G.; Pál, A.
2006tafp.conf..184B Altcode:
We summarize the current status of the HAT Network project. Started
up in 2003 with a single telescope, HATNet has grown to an array of
six almost identical, fully automated, wide-field telescopes spread in
geographical longitude, plus a higher resolution photometry follow-up
instrument called TopHAT. The instruments are maintained and controlled
from the Center for Astrophysics, and are fully dedicated to planetary
transit and variability search. Photometric precision reaches 3mmag
for stars at I≈8, and data from separate stations can be readily
combined. TopHAT is able to achieve millimag follow-up photometry. As
of June 2005, 100000 stars have been thoroughly analyzed (30000 with
photometry better than 1%); numerous transit candidates have been
found and followed up by spectroscopy or photometry. Most of these
turned out to be false positives, with a few cases still pending.
---------------------------------------------------------
Title: Transit Photometry of the Core-dominated Planet HD 149026b
Authors: Charbonneau, David; Winn, Joshua N.; Latham, David W.; Bakos,
Gáspár; Falco, Emilio E.; Holman, Matthew J.; Noyes, Robert W.;
Csák, Balázs; Esquerdo, Gilbert A.; Everett, Mark E.; O'Donovan,
Francis T.
2006ApJ...636..445C Altcode: 2005astro.ph..8051C
We report g, V, and r photometric time series of HD 149026
spanning predicted times of transit of the Saturn-mass
planetary companion, which was recently discovered by Sato and
collaborators. We present a joint analysis of our observations
and the previously reported photometry and radial velocities
of the central star. We refine the estimate of the transit ephemeris to
T<SUB>c</SUB>=(2,453,527.87455<SUP>+0.00085</SUP><SUB>-0.00091</SUB>)+(2.87598<SUP>+0.00012</SUP><SUB>-0.00017</SUB>)N
(HJD). Assuming that the star has a radius of 1.45+/-0.10
R<SUB>solar</SUB> and a mass of 1.30+/-0.10 M<SUB>solar</SUB>, we
estimate the planet radius to be (0.726+/-0.064)R<SUB>Jup</SUB>,
which implies a mean density of 1.07<SUP>+0.42</SUP><SUB>-0.30</SUB>
g cm<SUP>-3</SUP>. This density is significantly greater than predicted
for models that include the effects of stellar insolation and in which
the planet has only a small core of solid material. Thus, we confirm
that this planet likely contains a large core and that the ratio of
core mass to total planet mass is more akin to that of Uranus and
Neptune than to either Jupiter or Saturn.
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Title: VizieR Online Data Catalog: Ca II H and K Measurements Made
at MWO (Duncan+ 1991)
Authors: Duncan, D. K.; Vaughan, A. H.; Wilson, O. C.; Preston,
G. W.; Frazer, J.; Lanning, H. H.; Misch, A.; Mueller, J.; Soyumer,
D.; Woodard, L.; Baliunas, S. L.; Noyes, R. W.; Hartmann, L. W.;
Porter, A.; Zwaan, K.; Middelkoop, F.; Rutter, R.; Mihalas, D.
2005yCat.3159....0D Altcode:
Summaries are presented of the photoelectric measurements of stellar
CaII H and K line intensity made at Mount Wilson Observatory during
the years 1966-1983. These results are derived from 65,263 individual
observations of 1296 stars. For each star, for each observing season,
the maximum, minimum, mean, and variation of the instrumental H and
K index "S" are given, as well as a measurement of the accuracy of
observation. A total of 3110 seasonal summaries are reported. <P />These
observations were obtained with two instruments, HKP-1 and HKP-2. The
HKP-2 instrument is a four-channel chopping spectrometer which records
counts in 1.09{AA} FWHM triangular bandpasses centered in the H and
K lines as well as in two 20{AA} reference bandpasses centered on
3901.067 and 4001.067{AA}. The stellar activity is expressed by the
index S defined as <P />S = {alpha} (Nh+Nk)/(Nr+Nv) <P />where Nh and
Nk are the counts (corrected from background) in the H and K lines,
Nr and Nv those in the reference continuum bandpasses, and {alpha}
is a constant of proportionality used to correct for night-to-night
instrumental variations. Higher values of S generally correspond to
higher levels of chromospehric activities. <P />Factors which effect the
ability to detect stellar activity variations and accurately measure
their amplitudes such as the accuracy of the H and K measurements and
scattered light contamination are discussed. Relations are given which
facilitate intercomparison of "S" values with residual intensities
from ordinary spectrophotometry, and for converting measurements to
absolute fluxes. <P />(1 data file).
---------------------------------------------------------
Title: Measurement of Spin-Orbit Alignment in an Extrasolar Planetary
System
Authors: Winn, Joshua N.; Noyes, Robert W.; Holman, Matthew J.;
Charbonneau, David; Ohta, Yasuhiro; Taruya, Atsushi; Suto, Yasushi;
Narita, Norio; Turner, Edwin L.; Johnson, John A.; Marcy, Geoffrey W.;
Butler, R. Paul; Vogt, Steven S.
2005ApJ...631.1215W Altcode: 2005astro.ph..4555W
We determine the stellar, planetary, and orbital properties of the
transiting planetary system HD 209458 through a joint analysis of
high-precision radial velocities, photometry, and timing of the
secondary eclipse. Of primary interest is the strong detection of
the Rossiter-McLaughlin effect, the alteration of photospheric line
profiles that occurs because the planet occults part of the rotating
surface of the star. We develop a new technique for modeling this
effect and use it to determine the inclination of the planetary orbit
relative to the apparent stellar equator (λ=-4.4d+/-1.4d), and the
line-of-sight rotation speed of the star (vsinI<SUB>*</SUB>=4.70+/-0.16
km s<SUP>-1</SUP>). The uncertainty in these quantities has been reduced
by an order of magnitude relative to the pioneering measurements by
Queloz and collaborators. The small but nonzero misalignment is probably
a relic of the planet formation epoch, because the expected timescale
for tidal coplanarization is larger than the age of the star. Our
determination of vsinI<SUB>*</SUB> is a rare case in which rotational
line broadening has been isolated from other broadening mechanisms.
---------------------------------------------------------
Title: A Program to Detect and Characterize Extra-Solar Giant Planets
Authors: Noyes, Robert W.
2005STIN...0517097N Altcode:
This is the final report for this NASA grant. Work under the first
three years of the Grant (from May 1 2001 through April 30 2004) has
been described in previous annual reports. Here we briefly summarize
that work, and then focus on activities between May 1 2004 (the start
of a 1-year no-cost extension period) and April 30 2005, the end of
the Grant period.
---------------------------------------------------------
Title: VizieR Online Data Catalog: HATNET variability survey
(Hartman+, 2004)
Authors: Hartman, J. D.; Bakos, G.; Stanek, K. Z.; Noyes, R. W.
2005yCat..51281761H Altcode:
The data were obtained in 2003 June and July using the HAT-5 telescope
located at the Fred Lawrence Whipple Observatory (FLWO). <P />(2
data files).
---------------------------------------------------------
Title: A trend filtering algorithm for wide-field variability surveys
Authors: Kovács, Géza; Bakos, Gáspár; Noyes, Robert W.
2005MNRAS.356..557K Altcode: 2004MNRAS.tmp..644K; 2004astro.ph.11724K
We show that various systematics related to certain instrumental
effects and data reduction anomalies in wide-field variability surveys
can be efficiently corrected by a trend filtering algorithm (TFA)
applied to the photometric time-series produced by standard data
pipelines. Statistical tests, performed on the data base of the HAT
Network project, show that by the application of this filtering method
the cumulative detection probability of periodic transits increases
by up to 0.4 for variables brighter than 11 mag, with a trend of
increasing efficiency toward brighter magnitudes. We also show that
the TFA can be used for the reconstruction of periodic signals by
iteratively filtering out systematic distortions.
---------------------------------------------------------
Title: HATNET Variability Survey in the High Stellar Density “Kepler
Field” with Millimagnitude Image Subtraction Photometry
Authors: Hartman, J. D.; Bakos, G.; Stanek, K. Z.; Noyes, R. W.
2004AJ....128.1761H Altcode: 2004astro.ph..5597H
The Hungarian-made Automated Telescope Network (HATnet) is an ongoing
project to detect transiting extrasolar planets using small-aperture
(11 cm diameter) robotic telescopes. In this paper, we present the
results from using image subtraction photometry to reduce a crowded
stellar field observed with one of the HATnet telescopes (HAT-5). This
field was chosen to overlap with the planned Kepler mission. We obtained
I-band light curves for 98,000 objects in a 67 square degree field of
view centered at J2000 (α,δ) = (19<SUP>h</SUP>44<SUP>m</SUP>00s0,
+37°32'00.0"), near the Galactic plane in the constellations Cygnus
and Lyra. These observations include 788 exposures of 5 minutes' length
over 30 days. For the brightest stars (I~8.0) we achieved a precision
of 3.5 mmag, falling to 0.1 mag at the faint end (I~14). From these
light curves we identify 1617 variable stars, of which 1439 are newly
discovered. The fact that nearly 90% of the variables were previously
undetected further demonstrates the vast number of variables yet to
be discovered even among fairly bright stars in our Galaxy. We also
discuss some of the most interesting cases. These include V1171 Cyg,
a triple system with the inner two stars in a P=1.462 day period
eclipsing orbit and the outer star a P=4.86 day Cepheid; HD 227269,
an eccentric eclipsing system with a P=4.86 day period that also
shows P=2.907 day pulsations; WW Cyg, a well-studied eclipsing binary;
V482 Cyg, an R Coronae Borealis star; and V546 Cyg, a PV Telescopii
variable. We also detect a number of small-amplitude variables, in
some cases with full amplitude as low as 10 mmag.
---------------------------------------------------------
Title: HAT Variability Search in the High Stellar Density "Kepler
Field" with Millimagnitude Image Subtraction Photometry
Authors: Hartman, J. D.; Bakos, G.; Stanek, K. Z.; Noyes, R. W.
2004AAS...204.0604H Altcode: 2004BAAS...36..743H
The Hungarian-made Automated Telescope network (HATnet) is an ongoing
project to detect transiting extra-solar planets using small aperture,
robotic telescopes. In this poster we present the results from
using image subtraction photometry to reduce a crowded stellar field
(chosen to coincide with the planned field of the Kepler mission). We
obtained I-band lightcurves for 98,000 objects in a 67-square-degree
Field of View centered at (295.92, 37.54), along the galactic plane
in the constellations Lyra and Cygnus. These observations include 800
5-minute exposures spanning a 30 day period. For the brightest stars
(I 8.0) we achieved a precision of 3 millimagnitudes, falling to
0.04 magnitudes at the faint end (I 14.5). From these lightcurves we
identify several hundred variable stars, and we discuss some of the
most interesting cases.
---------------------------------------------------------
Title: Wide-Field Millimagnitude Photometry with the HAT: A Tool
for Extrasolar Planet Detection
Authors: Bakos, G.; Noyes, R. W.; Kovács, G.; Stanek, K. Z.; Sasselov,
D. D.; Domsa, I.
2004PASP..116..266B Altcode: 2004astro.ph..1219B
We discuss the system requirements for obtaining millimagnitude
photometric precision over a wide field using small-aperture,
short focal length telescope systems such as those being developed
by a number of research groups to search for transiting extrasolar
planets. We describe a Hungarian Automated Telescope (HAT) system,
which attempts to meet these requirements. The attainable precision
of HAT has been significantly improved by a technique in which
the telescope is made to execute small pointing steps during each
exposure so as to broaden the effective point-spread function (PSF)
of the system to a value more compatible with the pixel size of our
CCD detector. Experiments during a preliminary survey (spring 2003)
of two star fields with the HAT-5 instrument allowed us to optimize
the HAT photometric precision using this method of PSF broadening;
in this way we have been able to achieve a precision as good as 2
mmag on brighter stars. We briefly describe development of a network
of longitudinally spaced HAT telescopes (HATNet).
---------------------------------------------------------
Title: Probing the Outskirts of an Extrasolar Planet with HST
Time-Series Photometry
Authors: Charbonneau, David; Brown, Timothy M.; Gilliland, Ronald L.;
Noyes, Robert W.; Burrows, Adam
2004IAUS..202...72C Altcode:
No abstract at ADS
---------------------------------------------------------
Title: The ELODIE survey for northern extra-solar planets. II. A
Jovian planet on a long-period orbit around GJ 777 A
Authors: Naef, D.; Mayor, M.; Korzennik, S. G.; Queloz, D.; Udry,
S.; Nisenson, P.; Noyes, R. W.; Brown, T. M.; Beuzit, J. L.; Perrier,
C.; Sivan, J. P.
2003A&A...410.1051N Altcode: 2003astro.ph..6586N
We present radial-velocity measurements obtained with the ELODIE
and AFOE spectrographs for <ASTROBJ>GJ 777 A</ASTROBJ> (<ASTROBJ>HD
190360</ASTROBJ>), a metal-rich ([Fe/H] = 0.25) nearby (d = 15.9 pc)
star in a stellar binary system. A long-period low radial-velocity
amplitude variation is detected revealing the presence of a Jovian
planetary companion. Some of the orbital elements remain weakly
constrained because of the smallness of the signal compared to our
instrumental precision. The detailed orbital shape is therefore
not well established. We present our best fitted orbital solution:
an eccentric (e = 0.48) 10.7-year orbit. The minimum mass of the
companion is 1.33 M<SUB>Jup</SUB>. <P />Based on observations made
with the ELODIE echelle spectrograph mounted on the 1.93-m Telescope
at the Observatoire de Haute-Provence (CNRS) and with the AFOE
spectrograph mounted on the 1.5-m Telescope at the Fred Lawrence
Whipple Observatory (SAO). <P />The ELODIE and AFOE measurements
discussed in this paper are only available in electronic form at the
CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via
http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/410/1051
---------------------------------------------------------
Title: VizieR Online Data Catalog: ELODIE survey for northern
extra-solar planets. II. (Naef+, 2003)
Authors: Naef, D.; Mayor, M.; Korzennik, S. G.; Queloz, D.; Udry,
S.; Nisenson, P.; Noyes, R. W.; Brown, T. M.; Beuzit, J. L.; Perrier,
C.; Sivan, J. P.
2003yCat..34101051N Altcode:
Here are the 69 radial-velocity measurements of GJ 777A (HD 190360)
used for deriving the orbital solution of this star. These velocities
were obtained using the ELODIE echelle spectrograph mounted on the
1.93-m Telescope at Observatoire de Haute-Provence (France) and the
AFOE spectrograph mounted on the 1.5-m Telescope at the Fred Lawrence
Whipple Observatory (USA). <P />(1 data file).
---------------------------------------------------------
Title: The Extrasolar Planet Imager (ESPI)
Authors: Nisenson, P.; Melnick, G. J.; Geary, J.; Holman, M.;
Korzennik, S. G.; Noyes, R. W.; Papaliolios, C.; Sasselov, D. D.;
Fischer, D.; Gezari, D.; Lyon, R. G.; Gonsalves, R.; Hardesty, C.;
Harwit, M.; Marley, M. S.; Neufeld, D. A.; Ridgway, S. T.
2003ASPC..294..633N Altcode: 2002astro.ph.10046N
ESPI has been proposed for direct imaging and spectral analysis of
giant planets orbiting solar-type stars. ESPI extends the concept
suggested by Nisenson and Papaliolios (2001) for a square aperture
apodized telescope that has sufficient dynamic range to directly
detect extrasolar planets. With a 1.5-meter square mirror, ESPI can
deliver high dynamic range imagery as close as 0.3 arcseconds to bright
sources, permitting a sensitive search for extrasolar planets around
nearby stars and a study of their characteristics in reflected light.
---------------------------------------------------------
Title: Detection of an Extrasolar Planet Atmosphere
Authors: Charbonneau, David; Brown, Timothy M.; Noyes, Robert W.;
Gilliland, Ronald L.
2002ApJ...568..377C Altcode: 2001astro.ph.11544C
We report high-precision spectrophotometric observations of four
planetary transits of HD 209458, in the region of the sodium resonance
doublet at 589.3 nm. We find that the photometric dimming during
transit in a bandpass centered on the sodium feature is deeper by
(2.32+/-0.57)×10<SUP>-4</SUP> relative to simultaneous observations
of the transit in adjacent bands. We interpret this additional dimming
as absorption from sodium in the planetary atmosphere, as recently
predicted from several theoretical modeling efforts. Our model for
a cloudless planetary atmosphere with a solar abundance of sodium in
atomic form predicts more sodium absorption than we observe. There are
several possibilities that may account for this reduced amplitude,
including reaction of atomic sodium into molecular gases and/or
condensates, photoionization of sodium by the stellar flux, a low
primordial abundance of sodium, and the presence of clouds high in
the atmosphere. Based on observations with the NASA/ESA Hubble Space
Telescope (HST), obtained at the Space Telescope Science Institute,
which is operated by the Association of Universities for Research in
Astronomy, Inc. under NASA contract NAS 5-26555.
---------------------------------------------------------
Title: The Extra-Solar Planet Imager (ESPI): A Proposed MIDEX Mission
Authors: Melnick, G. J.; Fischer, D.; Geary, J. C.; Gezari, D. Y.;
Hardesty, C.; Harwit, M.; Holman, M.; Korzennik, S. G.; Lyon, R. G.;
Marley, M. S.; McElroy, M. B.; Neufeld, D. A.; Nisenson, P.; Noyes,
R. W.; Papaliolios, C.; Ridgway, S. T.; Sasselov, D. D.
2001AAS...199.0910M Altcode: 2002BAAS...34..559M
ESPI is a project that has been proposed as a NASA MIDEX for direct
imaging and spectral analysis of giant planets orbiting solar-type
stars. ESPI extends the concept suggested by Nisenson and Papaliolios
(2001) for a square aperture apodized telescope that has sufficient
dynamic range to directly detect exo-planets. ESPI can deliver high
dynamic range imagery as close as 0.32 arcseconds to bright sources,
permitting a sensitive search for exoplanets around nearby stars and
a study of their characteristics in reflected light. It also permits
unique observations of many Galactic, extragalactic and cosmological
sources. The ESPI Survey will be conducted with a square 1.5 x 1.5-meter
telescope mirror, operated in conjunction with a Jacquinot apodization
mask that has a throughput of more than 30 percent. The system is
capable of detecting Jupiter-like planets in relatively long-period
orbits around as many as 160 to 175 stars with a signal-to-noise
ratio greater than 5. In addition to the survey, ESPI will also
study a few of the brightest discovered planets spectroscopically
and spectrophotometrically to distinguish ice giants like Uranus and
Neptune from gas giants like Jupiter and Saturn, and to determine
whether super-Earth and super-Venus planets exist. Nisenson, P. and
Papaliolios, C. 2001, ApJ, 548, L 201.
---------------------------------------------------------
Title: Stellar Pollution in the Solar Neighborhood
Authors: Murray, N.; Chaboyer, B.; Arras, P.; Hansen, B.; Noyes, R. W.
2001ApJ...555..801M Altcode: 2000astro.ph.11530M
We study spectroscopically determined iron abundances of 640 solar-type
stars to search for the signature of accreted iron-rich material. We
find that the metallicity [Fe/H] of a subset of 466 main-sequence stars,
when plotted as a function of stellar mass, mimics the pattern seen
in lithium abundances in open clusters. Using Monte Carlo models,
we find that, on average, these stars appear to have accreted ~0.5
M<SUB>⊕</SUB> of iron while on the main-sequence. A consistency check
is provided by a much smaller sample of 19 stars in the Hertzsprung
gap, which are slightly evolved and the convection zones of which
are significantly more massive; they have lower average [Fe/H], and
their metallicity shows no clear variation with stellar mass. We
argue that our Sun is likely to have accreted a similar amount of
iron; in this respect, most systems resemble ours rather than the
currently known extrasolar planetary systems. These findings suggest
that terrestrial-type material is common around solar-type stars.
---------------------------------------------------------
Title: Hubble Space Telescope Time-Series Photometry of the Transiting
Planet of HD 209458
Authors: Brown, Timothy M.; Charbonneau, David; Gilliland, Ronald L.;
Noyes, Robert W.; Burrows, Adam
2001ApJ...552..699B Altcode: 2001astro.ph..1336B
We have observed four transits of the planet of HD 209458 using
the STIS spectrograph on the Hubble Space Telescope (HST). Summing
the recorded counts over wavelength between 582 and 638 nm yields a
photometric time series with 80 s time sampling and relative precision
of about 1.1×10<SUP>-4</SUP> per sample. The folded light curve can
be fitted within observational errors using a model consisting of an
opaque circular planet transiting a limb-darkened stellar disk. In
this way we estimate the planetary radius R<SUB>p</SUB>=1.347+/-0.060
R<SUB>Jup</SUB>, the orbital inclination i=86.6d+/-0.14d, the stellar
radius R<SUB>*</SUB>=1.146+/-0.050 R<SUB>solar</SUB>, and one parameter
describing the stellar limb darkening. Our estimated radius is smaller
than those from earlier studies but is consistent within measurement
errors and also with theoretical estimates of the radii of irradiated
Jupiter-like planets. Satellites or rings orbiting the planet would, if
large enough, be apparent from distortions of the light curve or from
irregularities in the transit timings. We find no evidence for either
satellites or rings, with upper limits on satellite radius and mass
of 1.2 R<SUB>⊕</SUB> and 3 M<SUB>⊕</SUB>, respectively. Opaque
rings, if present, must be smaller than 1.8 planetary radii in
radial extent. The high level of photometric precision attained in
this experiment confirms the feasibility of photometric detection of
Earth-sized planets circling Sun-like stars. Based on observations with
the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope
Science Institute, which is operated by the Association of Universities
for Research in Astronomy, Inc. under NASA contract NAS 5-26555.
---------------------------------------------------------
Title: Donald H. Menzel: Scientist, Educator Builder
Authors: Pasachoff, J. M.; Gingerich, O.; Layzer, D.; Noyes, R. W.;
Parkinson, W. H.; Welther, B.
2001AGUSM..SH41B26P Altcode:
A centennial symposium in honor of Donald H. Menzel was held at the
Harvard-Smithsonian Center for Astrophysics on May 11, 2001. Menzel
was known especially for his studies of the solar chromosphere, for
his theoretical work on gaseous nebulae, and for his role in founding
the Sacramento Peak and High Altitude observatories and in bringing the
Smithsonian Astrophysical Observatory to Cambridge. Menzel received his
Ph.D. at Princeton, where he was fascinated and excited by the lectures
of Henry Norris Russell about the new theoretical astrophysics. At
Lick Observatory, Menzel investigated the solar chromosphere using
solar eclipse spectra, and published the results in a major volume
in 1931. The value for the mean molecular weight he deduced for the
lower chromosphere helped persuade Russell and others that hydrogen
was the major constituent of the solar atmosphere, as Cecilia Payne had
intimated earlier. Menzel's studies of solar eclipse spectra also led
him to propose, in a paper written with R. T. Birge, that hydrogen had
an isotope of mass 2, a suggestion that motivated Harold Urey to isolate
the isotope (deuterium) chemically. Menzel joined the Harvard faculty
in 1932. His interest in investigating the sun led him to observe
more than a dozen solar eclipses, to exploit the coronagraph, and to
found two solar observatories: at Climax, Colorado, and at Sunspot, New
Mexico. He served as Director of the Harvard College Observatory from
1952 to 1966. During this time he suggested bringing and arranged to
bring the Smithsonian Astrophysical Observatory to Harvard. Speakers at
the symposium on Menzel's life, times, and scientific legacy included
Donald Osterbrock, David DeVorkin, David Layzer, Jay Pasachoff,
Barbara Welther, Thomas Bogdan, Jack Zirker, and France Cordova. The
organizing committee was Owen Gingerich, David Layzer, Robert Noyes,
William Parkinson, Jay Pasachoff, and Barbara Welther.
---------------------------------------------------------
Title: A Program To Detect and Characterize Extra-Solar Giant Planets
Authors: Noyes, Robert W.
2001STIN...0234979N Altcode:
This grant report highlights activity in the following areas: (1)
Improvement in Precise Radial Velocity (PRV) analysis code; (2)
Reanalysis of previous data; (3) Improvements to the AFOE (Advanced
Fiber Optic Echelle) spectrograph; (4) Development of PRV capabilities
for the Hectochelle; (5) Extra-solar planet studies; (6) Longer-term
plans for the AFOE; (7) Completion and publication of the analysis of
the transiting gas-giant planet HD 209458b.
---------------------------------------------------------
Title: Seeking the Atmospheric Transmission Spectrum of HD209458b
Authors: Brown, T. M.; Butler, R. P.; Charbonneau, D.; Noyes, R. W.;
Sasselov, D.; Libbrecht, K. G.; Marcy, G. W.; Seager, S.; Vogt, S. S.
2000AAS...197.1105B Altcode: 2000BAAS...32Q1417B
Transiting extrasolar giant planets such as HD209458b should impress
a spectroscopic signature on the light that is transmitted through
the outer parts of their atmospheres. Theory suggests that the depths
of absorption features resulting from this effect may be as large as
about 10<SUP>-3</SUP> of the parent star's continuum intensity. Such
spectral features could provide important diagnostics concerning the
composition and physical state of the planetary atmosphere. Accordingly,
we have obtained low-noise spectra of HD209458 during two transits
of its planet, once in visible light using the HIRES spectrograph at
the Keck I telescope, and once in the near infrared using the NIRSPEC
spectrograph at Keck II. We describe the methods employed and the
results of searches for spectral signatures of neutral atomic sodium,
carbon monoxide, and other atomic and molecular species.
---------------------------------------------------------
Title: A High-Eccentricity Low-Mass Companion to HD 89744
Authors: Korzennik, Sylvain G.; Brown, Timothy M.; Fischer, Debra A.;
Nisenson, Peter; Noyes, Robert W.
2000ApJ...533L.147K Altcode: 2000astro.ph..3045K
HD 89744 is an F7 V star with a mass of 1.4 M<SUB>solar</SUB>, an
effective temperature of 6166 K, an age of 2.0 Gyr, and metallicity
[Fe/H]=0.18. The radial velocity of the star has been monitored
with the Advanced Fiber-Optic Echelle spectrograph at the Whipple
Observatory since 1996, and evidence has been found for a low-mass
companion. The data were complemented by additional data from the
Hamilton spectrograph at Lick Observatory during the companion's
periastron passage in the fall of 1999. As a result, we have
determined the star's orbital wobble to have a period P=256 days,
an orbital amplitude K=257 m s<SUP>-1</SUP>, and an eccentricity
e=0.7. From the stellar mass, we infer that the companion has a
minimum mass m<SUB>2</SUB>sini=7.2 M<SUB>J</SUB> in an orbit with a
semimajor axis a<SUB>2</SUB>=0.88 AU. The eccentricity of the orbit,
among the highest known for extrasolar planets, continues the trend
that extrasolar planets with semimajor axes greater than about 0.15 AU
tend to have much higher eccentricities than are found in our solar
system. The high metallicity of the parent star reinforces the trend
that parent stars of extrasolar planets tend to have high metallicity.
---------------------------------------------------------
Title: Present and Near-Future Reflected-Light Searches for Close-In
Planets (Contributed Talk)
Authors: Charbonneau, D.; Noyes, R. W.
2000ASPC..219..461C Altcode: 2000astro.ph..2489C; 2000dpp..conf..461C
Close-in extrasolar giant planets may be directly detectable by
their reflected light, due to the proximity of the planet to the
illuminating star. The spectrum of the system will contain a reflected
light component that varies in amplitude and Doppler shift as the
planet orbits the star. Intensive searches for this effect have been
carried out for only one extrasolar planet system, tau Boo. There
exist several other attractive targets, including the transiting planet
system HD 209458.
---------------------------------------------------------
Title: Evidence for Multiple Companions to υ Andromedae
Authors: Butler, R. Paul; Marcy, Geoffrey W.; Fischer, Debra A.;
Brown, Timothy M.; Contos, Adam R.; Korzennik, Sylvain G.; Nisenson,
Peter; Noyes, Robert W.
1999ApJ...526..916B Altcode:
The bright F8 V star υ Andromedae was previously reported to have
a 4.6 day Doppler velocity periodicity, consistent with having a
Jupiter-mass companion orbiting at 0.059 AU. Follow-up observations
by both the Lick and Advanced Fiber-Optic Echelle spectrometer (AFOE)
planet survey programs confirm this periodicity and reveal additional
periodicities at 241 and 1267 days. These periodicities are consistent
with Keplerian orbital motion and imply two additional companions
orbiting at 0.83 and 2.5 AU, with minimum (Msini) masses of 2.0 and
4.6 M<SUB>JUP</SUB>, respectively. Non-Keplerian explanations for the
observed Doppler velocity variations, including radial and nonradial
pulsations, rotational modulation of surface features, and stellar
magnetic cycles, are examined. These explanations seem unlikely
based on the observed photometric and chromospheric stability of the
star. This putative three-planet system is found to be dynamically
stable by both analytic techniques and numerical simulations. The
outer two companions both reside in eccentric orbits, as do all nine
known extrasolar planet candidates in distant orbits. If real, this
multiple-planet system is the first around a main-sequence star, and
its study should offer insights into planet formation, planet-planet
interactions, and the observed eccentricities of planetary orbits. <P
/>Based on observations obtained at Lick Observatory, operated by the
University of California, and at the Whipple Observatory, operated by
the Smithsonian Astrophysical Observatory.
---------------------------------------------------------
Title: Evidence for a system of planets orbiting Upsilon Andromedae.
Authors: Noyes, R. W.; Korzennik, S. G.; Nisenson, P.; Holman, M. J.;
Contos, A.; Brown, T. M.
1999BAAS...31.1236N Altcode:
No abstract at ADS
---------------------------------------------------------
Title: An Upper Limit on the Reflected Light from the Planet Orbiting
the Star τ Bootis
Authors: Charbonneau, David; Noyes, Robert W.; Korzennik, Sylvain G.;
Nisenson, Peter; Jha, Saurabh; Vogt, Steven S.; Kibrick, Robert I.
1999ApJ...522L.145C Altcode: 1999astro.ph..7195C
The planet orbiting τ Boo at a separation of 0.046 AU could produce
a reflected light flux as bright as 1×10<SUP>-4</SUP> relative to
that of the star. A spectrum of the system will contain a reflected
light component which varies in amplitude and Doppler shift as the
planet orbits the star. Assuming the secondary spectrum is primarily
the reflected stellar spectrum, we can limit the relative reflected
light flux to be less than 5×10<SUP>-5</SUP>. This implies an upper
limit of 0.3 for the planetary geometric albedo near 480 nm, assuming a
planetary radius of 1.2 R<SUB>Jup</SUB>. This albedo is significantly
less than that of any of the giant planets of the solar system and is
not consistent with certain published theoretical predictions.
---------------------------------------------------------
Title: Evidence for a System of Planets Orbiting Upsilon Andromedae
Authors: Noyes, R. W.; Korzennik, S. G.; Nisenson, P.; Holman, M. J.;
Contos, A.; Brown, T. M.
1999AAS...194.1404N Altcode: 1999BAAS...31..847N
Using the Advanced Fiber Optic Echelle (AFOE) spectrograph at SAO's
Whipple Observatory, we have monitored the radial velocity of Upsilon
Andromedae since September 1994. Similar observations were made by the
"Lick" group (P. Butler, G. Marcy, D. Fischer; see Paper 14.02).The AFOE
data show, in addition to the already known close-in “hot Jupiter”
in a 4.6-day circular orbit, two additional companions. The middle
companion has a well-defined orbit, with semi-major axis about
0.83 AU, period 243.5 days, eccentricity 0.22, and minimum mass
(M sin i) of 2 Jupiter masses. This is in very close agreement with
independent findings by the Lick group. The AFOE data alone do not
yield well-determined orbital parameters for the outer companion,
because the total observing span encompasses only about one period of
its orbit. However, the data are consistent with parameters derived
for that companion by the Lick group from data with a longer time span,
and when combined with the Lick data yield a semi-major axis of 2.5 AU,
orbital period of 1267 days, eccentricity of 0.41, and minimum mass
about 4.6 Jupiter masses. These results, independently obtained by two
different groups with different instruments and analysis methodologies,
together give strong indications that a true planetary “system” has
now been discovered around a star like our own. We have carried out
numerical integrations which show that this system can be stable, but
only for certain combinations of periods, masses, and eccentricities
of the outer two companions. The stability requirement thus provides
a prediction that can be tested as the orbital elements of the outer
companion are refined. In addition, it imposes an upper limit on the
actual planetary masses, and on the difference in orbital inclination of
the two outer planets. Finally, the numerical integrations imply that
the longitudes of periastron of the two outer companions are locked to
nearly the same value, in accord with the present observations. This
work was supported by NASA, NSF, and the Smithsonian Institution.
---------------------------------------------------------
Title: Doppler Imaging of Stellar Oscillations: Multi-Site
Observations of Epsilon Cephei
Authors: Kennelly, E. J.; Brown, T. M.; Ehrenfreund, P.; Foing,
B.; Hao, J.; Horner, S.; Korzennik, S.; Nisenson, P.; Noyes, R.;
Sonnentrucker, P.
1999ASPC..185..264K Altcode: 1999IAUCo.170..264K; 1999psrv.conf..264K
We investigate the oscillation properties of ɛ Cep using a series of
specialized techniques designed to extract and analyze time variations
in absorption line profiles. To obtain the necessary temporal coverage
for this investigation, multi-site observations were collected at
3 sites (China, France, Arizona) all equipped with high-resolution
echelle spectrographs. From these observations, we find evidence for
a very rich spectrum of modes in ɛ Cep.
---------------------------------------------------------
Title: The Advanced Fiber-Optic Echelle (AFOE) and Extra-Solar
Planet Searches
Authors: Nisenson, P.; Contos, A.; Korzennik, S.; Noyes, R.; Brown, T.
1999ASPC..185..143N Altcode: 1999IAUCo.170..143N; 1999psrv.conf..143N
The Advanced Fiber-Optic Echelle (AFOE) is a fiber-fed bench-top
spectrograph specifically designed for precise radial velocity
observations. The AFOE is permanently located at the 1.5-m telescope
at Smithsonian's Whipple Observatory in Arizona and is regularly used
for monitoring exo-planet candidate stars and for asteroseismology
observations. In this paper, we discuss the status of the instrument,
as well as an upgrade to the instrument, a Fabry-Perot reference,
which may prove important both for the AFOE and for all precise radial
velocity (PRV) facilities.
---------------------------------------------------------
Title: The Planet Orbiting ρ Coronae Borealis
Authors: Noyes, R. W.; Contos, A. R.; Korzennik, S. G.; Nisenson,
P.; Brown, T. M.; Horner, S. D.
1999ASPC..185..162N Altcode: 1999IAUCo.170..162N; 1999psrv.conf..162N
Continuing precise radial velocity observations of ρ Coronae Borealis
have allowed the determination of updated parameters of the 40-day
orbit of its Jupiter-mass companion. This confirms the near-zero
eccentricity of the orbit, and provides improved predictions for the
times of possible transit of the companion in front of the star. The
new data provide more stringent upper limits to the mass of a possible
second companion to the system. The orbital parameters are discussed in
the light of several different scenarios for the origin and migration
of extra-solar giant planets.
---------------------------------------------------------
Title: Dynamics of Magnetic Flux Elements in the Solar Photosphere
Authors: van Ballegooijen, A. A.; Nisenson, P.; Noyes, R. W.; Löfdahl,
M. G.; Stein, R. F.; Nordlund, Å.; Krishnakumar, V.
1998ApJ...509..435V Altcode: 1998astro.ph..2359V
The interaction of magnetic fields and convection is investigated in
the context of the coronal heating problem. We study the motions of
photospheric magnetic elements using a time series of high-resolution
G-band and continuum filtergrams obtained at the Swedish Vacuum
Solar Telescope at La Palma. The G-band images show bright points
arranged in linear structures (“filigree”) located in the lanes
between neighboring granule cells. We measure the motions of these
bright points using an object tracking technique, and we determine
the autocorrelation function describing the temporal variation of
the bright point velocity. The correlation time of the velocity is
about 100 s. To understand the processes that determine the spatial
distribution of the bright points, we perform simulations of horizontal
motions of magnetic flux elements in response to solar granulation
flows. Models of the granulation flow are derived from the observed
granulation intensity images using a simple two-dimensional model
that includes both inertia and horizontal temperature gradients; the
magnetic flux elements are assumed to be passively advected by this
granulation flow. The results suggest that this passive advection model
is in reasonable agreement with the observations, indicating that on
a timescale of 1 hr the flux tubes are not strongly affected by their
anchoring at large depth. Finally, we use potential-field modeling
to extrapolate the magnetic and velocity fields to larger height. We
find that the velocity in the chromosphere can be locally enhanced at
the separatrix surfaces between neighboring flux tubes. The predicted
velocities are several km s<SUP>-1</SUP>, significantly larger than
those of the photospheric flux tubes. The implications of these results
for coronal heating are discussed.
---------------------------------------------------------
Title: Spectral Line Distortions in the Presence of a Close-in Planet
Authors: Charbonneau, David; Jha, Saurabh; Noyes, Robert W.
1998ApJ...507L.153C Altcode: 1998astro.ph..9099C
We discuss the interpretation of the distortions to the stellar spectral
lines, with particular attention to line bisectors in the presence of
an orbiting planetary companion. We present a simple model whereby light
reflected by the companion can cause temporal variations to the observed
line profiles. These distortions have a characteristic signature that
depends on the inclination angle of the system. For the known close-in
extrasolar giant planets, the expected amplitude of the effect might
not be far from current detection capabilities. This method could
be used to detect the presence of the companion directly, yielding
the orbital inclination and hence the planetary mass. Futhermore,
a detection would measure a combination of the planetary radius and
albedo, from which a minimum radius may be deduced.
---------------------------------------------------------
Title: Exoplanets or Dynamic Atmospheres? The Radial Velocity and
Line Shape Variations of 51 Pegasi and τ Bootis
Authors: Brown, Timothy M.; Kotak, Rubina; Horner, Scott D.;
J. Kennelly, Edward; Korzennik, Sylvain; Nisenson, P.; Noyes, Robert W.
1998ApJS..117..563B Altcode: 1998astro.ph..1166B
The stars 51 Pegasi and τ Bootis show radial velocity variations that
have been interpreted as resulting from companions with roughly Jovian
mass and orbital periods of a few days. Gray and Gray & Hatzes
reported that the radial velocity signal of 51 Peg is synchronous with
variations in the shape of the line λ6253 Fe I; thus, they argue that
the velocity signal arises not from a companion of planetary mass but
from dynamic processes in the atmosphere of the star, possibly nonradial
pulsations. Here we seek confirming evidence for line shape or strength
variations in both 51 Peg and τ Boo, using R = 50,000 observations
taken with the Advanced Fiber Optic Echelle. Because of our relatively
low spectral resolution, we compare our observations with Gray's line
bisector data by fitting observed line profiles to an expansion in terms
of orthogonal (Hermite) functions. To obtain an accurate comparison,
we model the emergent line profiles from rotating and pulsating stars,
taking the instrumental point-spread function into account. We describe
this modeling process in detail. We find no evidence for line profile or
strength variations at the radial velocity period in either 51 Peg or in
τ Boo. For 51 Peg, our upper limit for line shape variations with 4.23
day periodicity is small enough to exclude with 10 σ confidence the
bisector curvature signal reported by Gray & Hatzes; the bisector
span and relative line depth signals reported by Gray are also not seen,
but in this case with marginal (2 σ) confidence. We cannot, however,
exclude pulsations as the source of 51 Peg's radial velocity variation
because our models imply that line shape variations associated with
pulsations should be much smaller than those computed by Gray &
Hatzes; these smaller signals are below the detection limits both for
Gray & Hatzes's data and for our own. τ Boo's large radial velocity
amplitude and v sin i make it easier to test for pulsations in this
star. Again we find no evidence for periodic line shape changes, at a
level that rules out pulsations as the source of the radial velocity
variability. We conclude that the planet hypothesis remains the most
likely explanation for the existing data.
---------------------------------------------------------
Title: Study of Magnetic Structure in the Solar Photosphere and
Chromosphere
Authors: Noyes, Robert W.; Avrett, Eugene; Nisenson, Peter; Uitenbroek,
Han; van Ballegooijen, Adriaan
1998nasa.reptV....N Altcode:
This grant funded an observational and theoretical program to study the
structure and dynamics of the solar photosphere and low chromosphere,
and the spectral signatures that result. The overall goal is to learn
about mechanisms that cause heating of the overlying atmosphere, and
produce variability of solar emission in spectral regions important
for astrophysics and space physics. The program exploited two new
ground-based observational capabilities: one using the Swedish Solar
Telescope on La Palma for very high angular resolution observations
of the photospheric intensity field (granulation) and proxies of the
magnetic field (G-band images); and the other using the Near Infrared
Magnetograph at the McMath-Pierce Solar Facility to map the spatial
variation and dynamic behavior of the solar temperature minimum
region using infrared CO lines. We have interpreted these data using
a variety of theoretical and modelling approaches, some developed
especially for this project. Previous annual reports cover the work
done up to 31 May 1997. This final report summarizes our work for the
entire period, including the period of no-cost extension from 1 June
1997 through September 30 1997. In Section 2 we discuss observations
and modelling of the photospheric flowfields and their consequences
for heating of the overlying atmosphere, and in Section 3 we discuss
imaging spectroscopy of the CO lines at 4.67 mu.
---------------------------------------------------------
Title: The Oscillations of Tau Pegasi
Authors: Kennelly, E. J.; Brown, T. M.; Kotak, R.; Sigut, T. A. A.;
Horner, S. D.; Korzennik, S. G.; Nisenson, P.; Noyes, R. W.; Walker,
A.; Yang, S.
1998ApJ...495..440K Altcode:
We present extensive spectroscopic time series observations of the
multiperiodic, rapidly rotating, δ Scuti star τ Pegasi. Information
about the oscillations is contained within the patterns of line-profile
variation of the star's blended absorption-line spectrum. We introduce
the new technique of Doppler deconvolution with which to extract these
patterns by modeling the intrinsic stellar spectrum and the broadening
functions for each spectrum in the time series. Frequencies and modes
of oscillation are identified from the variations using the technique
of Fourier-Doppler imaging and a two-dimensional least-squares cleaning
algorithm. We find a rich mode spectrum with degrees up to l = 20 and
with frequencies below about 35 cycles day<SUP>-1</SUP>. Those modes
with the largest amplitudes have frequencies that lie within a narrow
band. We conclude that the observed spectrum can be explained if the
modes of τ Peg propagate in the prograde direction with l ~= |m| and
with frequencies that are about equal in the corotating frame of the
star. We discuss the implications of these results for the prospect
of δ Scuti seismology.
---------------------------------------------------------
Title: A Search for Line Shape and Depth Variations in 51 Pegasi
and τ Bootis
Authors: Brown, Timothy M.; Kotak, Rubina; Horner, Scott D.; Kennelly,
Edward J.; Korzennik, Sylvain; Nisenson, P.; Noyes, Robert W.
1998ApJ...494L..85B Altcode: 1997astro.ph.12279B
Spectroscopic observations of 51 Pegasi and τ Bootis show no periodic
changes in the shapes of their line profiles; these results for 51
Peg are in significant conflict with those reported by Gray &
Hatzes. Our detection limits are small enough to rule out nonradial
pulsations as the cause of the variability in τ Boo, but not in 51
Peg. The absence of line shape changes is consistent with these stars'
radial velocity variability arising from planetary mass companions.
---------------------------------------------------------
Title: The Stellar and Planetary Explorer (SPEX) Mission
Authors: Schou, J.; Scherrer, P. H.; Brown, T. M.; Frandsen, S.;
Horner, S. D.; Korzennik, S. G.; Noyes, R. W.; Tarbell, T. D.; Title,
A. M.; Walker, A. B. C., II; Weiss, W. W.; Bogart, R. S.; Bush, R. I.;
Christensen-Dalsgaard, J.; Hoeksema, J. T.; Jones, A.; Kjeldsen, H.
1998ESASP.418..401S Altcode: 1998soho....6..401S
The Stellar and Planetary Explorer (SPEX) is a mission designed
to search for terrestrial sized planets around sun-like stars using
precise photometry. The planets will be detected by searching for the
decrease in brightness associated with transits of the planets in front
of their parent stars. One of the secondary scientific objective of
SPEX is to do asteroseismology on a number of sun-like stars. SPEX
is designed as a secondary payload on a commercial communications
satellite and will have a design life time of three years. We will
provide an overview of the SPEX scientific objectives and design,
with particular emphasis on the prospects for doing asteroseismology.
---------------------------------------------------------
Title: Exoplanet Research with the Advanced Fiber Optic Echelle
Authors: Korzennik, S. G.; Brown, T. M.; Contos, A. R.; Horner, S.;
Jha, S.; Kennelly, T.; Krockenberger, M.; Nisenson, P.; Noyes, R. W.
1998ASPC..154.1876K Altcode: 1998csss...10.1876K
The AFOE is a fiber-fed bench-top echelle spectrometer installed
at the Mt. Hopkins 1.5 m telescope for research in exoplanets,
asteroseismology, and other topics requiring precise radial velocity
measurements. Here we describe the instrumentation, observing programs,
and data reduction techniques for exoplanet research with the AFOE. We
also summarize recent results of our search for and characterization
of exoplanets. Further information on the AFOE can be found on the
Web at http://cfa-www.harvard.edu/afoe.
---------------------------------------------------------
Title: Temperatures of Cepheids from Line-Depth Ratios
Authors: Krockenberger, M.; Sasselov, D.; Noyes, R.; Korzennik, S.;
Nisenson, P.; Brown, T.; Kennelly, T.; Horner, S.
1998ASPC..154..791K Altcode: 1998csss...10..791K
We present observations of 11 Cepheids and 16 non-variable supergiants
with the Advanced Fiber Optics Echelle (AFOE) spectrograph. We measure
the effective temperatures of Cepheids and supergiants using spectral
line depth ratios and Kurucz's model atmospheres. For the Cepheids we
use the fact that the reddening is constant as a function of phase as an
additional constraint. We find errors in the mean temperature as small
as 10 K for the best sampled Cepheids. Our temperatures and surface
brightnesses disagree with the results of the Barnes-Evans method.
---------------------------------------------------------
Title: 51 Pegasi and Tau Bootis: Planets or Pulsations?
Authors: Horner, S. D.; Brown, T. M.; Kennelly, E. J.; Kotak, R.; Jha,
S.; Korzennik, S. G.; Krockenberger, M.; Nisenson, P.; Noyes, R. W.
1998ASPC..135..206H Altcode: 1998hcsp.conf..206H
It has recently been suggested (Gray 1997) that the radial velocity
variations observed in the spectra of 51 Pegasi are the result of
stellar pulsations as opposed to the reflex motion due to an orbital
companion. The AFOE group has confirmed the radial velocity variations
in 51 Pegasi and t Bootis. Here we discuss the results of a search for
evidence of pulsations in the AFOE data for these two stars, as well
as attempt to clear up misconceptions regarding pulsations circulated
as a result of the current debate about the nature of the 51 Pegasi
radial velocity variations.
---------------------------------------------------------
Title: 51 Pegasi and Tau Bootis: Planets or Pulsations?
Authors: Horner, S. D.; Brown, T. M.; Kennedy, E. J.; Kotak, R.; Jha,
S.; Korzennik, S. G.; Krockenberger, M.; Nisenson, P.; Noyes, R. W.
1998ASPC..154.1860H Altcode: 1998csss...10.1860H
Using data from the AFOE and simulations of pulsating stars, we are able
to rule out pulsations as the cause of the radial velocity variations
seen in tau Bootis and conclude that it is unlikely that pulsations
are the cause of radial velocity variations seen in 51 Pegasi. Orbital
companions are still the most probable causes of the radial velocity
variations observed in these systems.
---------------------------------------------------------
Title: Asteroseismology of Procyon with the AFOE
Authors: Horner, S. D.; Brown, T. M.; Kennelly, E. J.; Korzennik,
S.; Nisenson, P.; Noyes, R. W.
1997AAS...191.4310H Altcode: 1997BAAS...29R1276H
The Advanced Fiber Optic Echelle (AFOE) is a bench-mounted,
fiber-fed echelle spectrograph designed for precision radial velocity
observations. Located at the 1.5m Tillinghast telescope at Whipple
Observatory, the AFOE is used to detect exoplanets and is involved in
several projects in asteroseismology, including asteroseismology of
Sun-like stars. Procyon has been a prime target for asteroseismology
of Sun-like stars due to its proximity and its spectral type
(F5 IV-V). Theory predicts that due to its low surface gravity
and inefficient surface convection, the amplitudes of its p-mode
pulsation modes should be relatively large, though still less than 1
m\ s(-1) . While the velocity of individual modes is extremely small,
observations of Procyon with the AFOE show excess power in the frequency
range between 0.5 to 1.5 MHz. This power may be the result of p-mode
oscillations on Procyon, and is consistent with previous results (Brown
et al. 1991). However, mode identification is required to interpret
the ramifications of the observations for the star's structure, which
is the goal of asteroseismology. These single-site data are limited
in frequency resolution, which may prevent clear identification of
individual modes.
---------------------------------------------------------
Title: Erratum: A Planet Orbiting the Star Rho Coronae Borealis:
Authors: Noyes, Robert W.; Jha, Saurabh; Korzennik, Sylvain G.;
Krockenberger, Martin; Nisenson, Peter; Brown, Timothy M.; Kennelly,
Edward J.; Horner, Scott D.
1997ApJ...487L.195N Altcode:
In the Letter, “A Planet Orbiting the Star ρ Coronae Borealis”
by Robert W. Noyes, Saurabh Jha, Sylvain G. Korzennik, Martin
Krockenberger, Peter Nisenson, Timothy M. Brown, Edward J. Kennelly,
and Scott D. Horner (ApJ, 483, L111 [1997]), a software error caused
the sign of the reported radial velocity variations of ρ Coronae
Borealis to be reversed. This error has no effect on the period,
amplitude, or eccentricity of the derived orbit and thus does not
affect the main conclusion of the paper. However, the longitude ω
of periastron reported in Table 1 is off by 180°, and the predicted
time of a possible planetary transit T<SUB>transit</SUB> is off by
approximately 1/2 period. The correct values are ω = 30° +/- 74°
and T<SUB>transit</SUB> = 2,450,657.88 +/- 0.54 HJD.
---------------------------------------------------------
Title: Mesosphere Sodium Column Density and the Sodium Laser Guide
Star Brightness
Authors: Ge, Jian; Angel, J. R. P.; Jacobsen, B. D.; Roberts, T.;
Martinez, T.; Livingston, W.; McLeod, B.; Lloyd-Hart, M.; McGuire,
P.; Noyes, R.
1997astro.ph..8275G Altcode:
The first time simultaneous measurements of sodium column density
and the absolute flux from a sodium laser guide star, created by
a monochromatic 3 W cw laser, tuned to the peak of the sodium D2
hyperfine structure, were conducted at the MMT and CFA 60 inch
telescope in 1997. The results show that linearly and circularly
polarized laser returns are proportional to the simultaneous sodium
column density. Moreover, circularly polarized laser provides about
30% increase in fluorescent return over linearly polarized laser. A
laser guide star with R = 10.3 mag. or absolute flux of 8.4x10^5
photons/s/m^2, could be formed from a 1 watt projected circularly
polarized sodium laser beam when sodium layer abundance N(Na) = 3.7x10^9
/cm^2. Together with the distributed column density measurements
(e.g. seasonal and diurnal variations), we can project laser power
requirements for any specified guide star brightness. The mesosphere
sodium column density variation was measured above Tucson sky throughout
the year, through sodium absorption line measurements in stellar and
solar spectra. Previous measurements, e.g. Papen et al, 1996, have
not been made at this latitude (32 degrees). Further, our absorption
method is more direct and may be more accurate than the lidar methods
normally used. The seasonal variation amplitude is smaller than that
at higher latitudes. While the annual mean sodium column density tends
to be lower than at higher latitudes. Diurnal sodium column density
tends to vary by as much as a factor of two within an hour.
---------------------------------------------------------
Title: A Planet Orbiting the Star ρ Coronae Borealis
Authors: Noyes, Robert W.; Jha, Saurabh; Korzennik, Sylvain G.;
Krockenberger, Martin; Nisenson, Peter; Brown, Timothy M.; Kennelly,
Edward J.; Horner, Scott D.
1997ApJ...483L.111N Altcode: 1997astro.ph..4248N
We report the discovery of near-sinusoidal radial velocity variations
of the G0V star ρ CrB, with period 39.6 days and amplitude 67 m
s<SUP>-1</SUP>. These variations are consistent with the existence
of an orbital companion in a circular orbit. Adopting a mass of 1.0
M<SUB>solar</SUB> for the primary, the companion has minimum mass
about 1.1 Jupiter masses and orbital radius about 0.23 AU. Such an
orbital radius is too large for tidal circularization of an initially
eccentric orbit during the lifetime of the star, and hence we suggest
that the low eccentricity is primordial, as would be expected for a
planet formed in a dissipative circumstellar disk.
---------------------------------------------------------
Title: Radii and Distances of Cepheids. I. Method and Measurement
Errors
Authors: Krockenberger, Martin; Sasselov, Dimitar D.; Noyes, Robert W.
1997ApJ...479..875K Altcode: 1996astro.ph.11123K
We develop a formulation of the Baade-Wesselink method which uses
the Fourier coefficients of the observables. We derive an explicit,
analytic expression to determine the mean radius from each Fourier
order. The simplicity of this method allows us to derive the uncertainty
in the mean radius due to measurement errors. <P />Using simulations
and a recent data set we demonstrate that the precision of the radius
measurement with optical magnitudes is in most cases limited by the
accuracy of the measurement of the phase difference between the light
and the color index curve. In this case it is advantageous to determine
the inverse radius, because it has normal errors.
---------------------------------------------------------
Title: A Radial Velocity Search for p-Mode Pulsations in η Bootis
Authors: Brown, Timothy M.; Kennelly, Edward J.; Korzennik, Sylvain
G.; Nisenson, Peter; Noyes, Robert W.; Horner, Scott D.
1997ApJ...475..322B Altcode:
The subgiant η Boo (G5 IV) has been reported to show p-mode pulsations,
as evidenced by variations in the equivalent width of its hydrogen
Balmer lines (reported by Kjeldsen et al.). In an attempt to confirm
this report, we observed η Boo's radial velocity with the AFOE
spectrograph for a total of 22 hours spread over seven successive
nights in 1995 March. We find no evidence for the presence of excess
power at the frequencies reported by Kjeldsen et al.; our upper limit
corresponds to typical mode amplitudes of 0.5 m s<SUP>-1</SUP>, about 3
times smaller than the velocity amplitudes they inferred. Signals with
amplitudes larger than 0.5 m s<SUP>-1</SUP> may be present at other
frequencies within the 0-1000 μHz range, but evidence for such signals
is scanty, and typical mode amplitudes greater than 1.5 m s<SUP>-1</SUP>
are clearly inconsistent with our observations.
---------------------------------------------------------
Title: The AFOE Program of Extra-Solar Planet Research
Authors: Noyes, R.; Jha, S.; Korzennik, S.; Krockenberger, M.;
Nisenson, P.; Brown, T.; Kennelly, E.; Horner, S.
1997ASPC..119..119N Altcode: 1997pbss.conf..119N
No abstract at ADS
---------------------------------------------------------
Title: A radial velocity search for p-modes in Procyon.
Authors: Brown, T. M.; Kennelly, E. J.; Noyes, R. W.; Korzennik,
S. G.; Nisenson, P.; Horner, S. D.; Catala, C.
1996BAAS...28..917B Altcode:
No abstract at ADS
---------------------------------------------------------
Title: The oscillation modes of ɛ Cep and τ Peg.
Authors: Horner, S. D.; Kennelly, E. J.; Brown, T. M.; Noyes, R. W.;
Korzennik, S. G.; Nisenson, P.; Yang, S.; Walker, A. R.
1996BAAS...28..916H Altcode:
No abstract at ADS
---------------------------------------------------------
Title: The Global Oscillation Network Group (GONG) Project
Authors: Harvey, J. W.; Hill, F.; Hubbard, R. P.; Kennedy, J. R.;
Leibacher, J. W.; Pintar, J. A.; Gilman, P. A.; Noyes, R. W.; Title,
A. M.; Toomre, J.; Ulrich, R. K.; Bhatnagar, A.; Kennewell, J. A.;
Marquette, W.; Patron, J.; Saa, O.; Yasukawa, E.
1996Sci...272.1284H Altcode:
Helioseismology requires nearly continuous observations of the
oscillations of the solar surface for long periods of time in
order to obtain precise measurements of the sun's normal modes of
oscillation. The GONG project acquires velocity images from a network
of six identical instruments distributed around the world. The GONG
network began full operation in October 1995. It has achieved a duty
cycle of 89 percent and reduced the magnitude of spectral artifacts by
a factor of 280 in power, compared with single-site observations. The
instrumental noise is less than the observed solar background.
---------------------------------------------------------
Title: The Oscillation Modes of epsilon CEP and tau Peg
Authors: Horner, S. D.; Kennelly, E. J.; Brown, T. M.; Noyes, R. W.;
Korzennik, S. G.; Nisenson, P.; Yang, S.; Walker, A.
1996AAS...188.5901H Altcode: 1996BAAS...28Q.917H
Asteroseismology of delta Scuti stars offers an attractive prospect for
determining the interior properties of main sequence and slightly more
evolved A- and F-type stars. Here we present detailed identifications
of oscillation modes in the rapidly rotating delta Scuti stars epsilon
Cep and tau Peg based on extensive observations carried out at two
North American sites. Using cross-correlation and Fourier techniques
we analyze the line-profile variations and the variations in the
line-profile moments. A solution to the mode spectrum is sought using
a genetic-based search algorithm and a line profile simulation model
to reproduce the observed variations.
---------------------------------------------------------
Title: Use of Temperature-Sensitive Line Ratios for Stellar Seismology
Authors: Noyes, R. W.; Korzennik, S. G.; Krockenberger, M.; Nisenson,
P.; Brown, T.; Kennelly, T.; Horner, S.
1996AAS...188.5906N Altcode: 1996BAAS...28..918N
The line depths of virtually all stellar spectral lines are sensitive
to small changes in stellar temperature T<SUB>eff</SUB> induced by
pulsations, with varying degrees (and signs) depending on the mean
T<SUB>eff</SUB> and the line ionization and excitation state. For
large-amplitude pulsators, such as Cepheids, temperatures obtained
from individual line pairs are sufficiently accurate and invariant
to reddening to play an important role in distance measurements. For
small-amplitude pulsators, this technique is inadequate. However,
by combining the information from a very large number of spectral
lines recorded with high spectral resolution, such as can be provided
by a cross-dispersed echelle spectrograph, it should be possible to
measure temperature changes to a precision considerably greater than
can be obtained by comparing single pairs of lines. We explore this
possibility by using a grid of synthetic stellar spectra to provide the
run of temperature sensitivity as a function of wavelength throughout
the spectrum, and make specific application to spectra obtained with
the Advanced Fiber Optic Echelle (AFOE) spectrograph.
---------------------------------------------------------
Title: A Radial Velocity Search for p-modes in Procyon
Authors: Brown, T. M.; Kennelly, E. J.; Noyes, R. W.; Korzennik,
S. G.; Nisenson, P.; Horner, S. D.; Catala, C.
1996AAS...188.5902B Altcode: 1996BAAS...28R.917B
Procyon (alpha CMi F5 IV) has long been a promising candidate for
detection of solar-like p-modes. Although several authors have reported
evidence for low-amplitude (<= 10) m/s pulsations in this star,
none of the existing observations are conclusive. A clear detection
of such pulsations would be a significant step for asteroseismology
of Sun-like stars, allowing refined estimates of the star's properties
and paving the way for the study of fainter stars of similar spectral
type. Identification of oscillation modes in subgiants like Procyon is
expected to be difficult, however, because both the amplitudes and the
frequency separations of the modes are expected to be small. To address
these difficulties, we organized a joint observing campaign involving
the AFOE spectrograph located at the Whipple Observatory (Mt. Hopkins,
AZ) and the MUSICOS spectrograph located at Pic du Midi. Both
instruments are capable of providing Doppler measurements with the
required precision of a few m/s, and the 7 hour longitude separation
between them allows the acquisition of relatively long uninterrupted
data strings. In the event, bad weather prevented more than sporadic
observations from Pic du Midi. At Mt. Hopkins, however, we obtained
good observations on each of 6 consecutive nights 3-8 Feb 1996, for
a total of 47 h of observing time. We discuss here the interpretation
of this data set in terms of possible p-mode oscillations.
---------------------------------------------------------
Title: Study of Magnetic Motions in the Solar Photosphere and Their
Implications for Heating the Solar Atmosphere
Authors: Noyes, Robert W.
1996sao..rept.....N Altcode:
Dynamic modeling of CO line formation, and the development of a
two-dimensional radiative transfer code that includes the effects of
partial frequency redistribution, are described.
---------------------------------------------------------
Title: HD 3346
Authors: Noyes, R.; Korzennik, S.; Nisenson, P.; Jha, S.;
Krockenberger, M.; Brown, T.; Kennelly, T.; Rowland, C.; Horner, S.
1996IAUC.6316....1N Altcode: 1996IAUC.6316Q...1N
R. Noyes, S. Korzennik, P. Nisenson, S. Jha, and M. Krockenberger,
Smithsonian Astrophysical Observatory; T. Brown, T. Kennelly, and
C. Rowland, High Altitude Observatory; and S. Horner, Pennsylvania State
University, report the detection of large short- term radial-velocity
variations in the K5 III star HD 3346 = HR 152. Irregularly spaced
observations were made with the Advanced Fiber Optic Echelle (AFOE)
spectrometer at the 1.5-m telescope of the Whipple Observatory during
the last quarters of 1993, 1994, and 1995, with more intensive
observations in December 1995 and February 1996. A long-period
radial-velocity variation similar to that already reported by McClure
et al. (1985, PASP 97, 740) is seen with amplitude of order 500 m/s
and period of order 650 days. This is consistent with a companion to HD
3346 at orbital distance about 2.5 AU. If the mass of HD 3346 is 5 solar
masses, then this already-reported companion would have projected mass
m sin i about 60 Jupiter masses. The AFOE data reveal the presence of
shorter- term radial-velocity variations superimposed on the 650-day
variation. The amplitude of the variations is in the range 150-300
m/s. Near-nightly observations in December 1995 and February 1996 show
the variations to be consistent with those produced by a second orbital
companion. The window function of the data would allow for its period
to be near 14, 18, 24, or 40 days. Such a short period would imply that
the second companion's orbit would have a semimajor axis between 0.2 and
0.4 AU; the amplitude of the variation implies that (again, if HD 3346
has a mass of 5 solar masses) this second companion has m sin i about
10 Jupiter masses. Acoustic pulsations may be an alternative source of
the short-term radial-velocity variations. However, the fundamental
period of acoustic pulsations in giants is expected to be only a few
days; the present data could be explained by acoustic pulsations only
if the star has a mass much lower than suggested by standard stellar-
evolution theory. Spurious signals due to rotation of starspots appear
to be unlikely because of the low reported rotational velocity for HD
3346. A definitive period for the short-period radial-velocity variation
may be determinable if other contemporaneous precise radial-velocity
observations of this star exist or can be obtained before the star
disappears behind the sun for this observing season.
---------------------------------------------------------
Title: Olin C. Wilson and the solar-stellar connection
Authors: Noyes, R. W.
1996ASPC..109....3N Altcode: 1996csss....9....3N
No abstract at ADS
---------------------------------------------------------
Title: Infrared MG I lines in cool giant and supergiant stars
Authors: Uitenbroek, H.; Noyes, R. W.
1996ASPC..109..723U Altcode: 1996csss....9..723U
No abstract at ADS
---------------------------------------------------------
Title: Precise Photometry Mission -- Measuring Stellar
Microvariability from Space
Authors: Brown, T. M.; Borucki, W.; Frandsen, S.; Gilliland, R. L.;
Jones, A.; Noyes, R. W.; Tarbell, T.; Title, A.; Ulrich, R. K.
1995AAS...187.7111B Altcode: 1995BAAS...27R1385B
Atmospheric scintillation limits the precision attainable by
ground-based photometry; this limitation is a major obstacle to
progress in several fields, notably asteroseismology of Sun-like
stars. A space-borne photometric telescope could operate near the shot
noise limit, removing this obstacle and providing new opportunities
for inquiry. As part of the program for New Mission Concepts in
Astrophysics, we are studying the scientific rewards and technological
challenges associated with a Precise Photometry Mission (PPM). The
baseline performance goal for the PPM is to measure solar-like
pulsations (amplitude 3 mu mag) in G stars in the Hyades with a S/N
ratio of 4 in 10 days of observing time. This performance would also
allow detection of transits of Earth-sized planets of main-sequence
stars, extremely precise characterization of the light curves of
micro-lensing events, and other novel applications. The technical
approach envisioned for the PPM is wide-band CCD photometry. The study
that is underway focuses on two aspects of the required technology: (1)
Are CCD detectors able to provide the necessary very high S/N within
the spacecraft operating environment? (2) Can new lightweight mirror
and telescope structure technology be applied to yield significant
reductions in mission cost? We are addressing both questions with
laboratory tests, including time-series performance tests of suitable
CCDs, and thermal and mechanical tests of a SiC telescope mirror. In
addition to describing PPM's scientific aims and technical rationale,
we report preliminary results of the CCD tests.
---------------------------------------------------------
Title: A Radial Velocity Search for p-mode Pulsations in eta Bootis
Authors: Noyes, R. W.; Korzennik, S. G.; Nisenson, P.; Brown, T. M.;
Kennelly, E. J.; Horner, S. D.
1995AAS...18710211N Altcode: 1995BAAS...27.1429N
Kjeldsen et al. 1994 (Astron. J 109, 1313 ) have reported the presence
of p-mode pulsations in Balmer line equivalent widths measured in
the spectrum of eta Boo (G5 IV); they give accurate frequencies for
13 modes of oscillation, and estimate velocity amplitudes for these
modes of typically 1.6 m/s. We report here time-series observations of
the radial velocity of eta Boo obtained with the Advanced Fiber Optic
Echelle (AFOE) spectrograph. In March 1995 we obtained 555 spectra
of eta Boo for a total of 21.6 hours of observing time spread over
7 consecutive nights. The radial velocity time series clearly shows
the night-to-night orbital motion of eta Boo; the residual velocities
after removing this motion are typically 10 m/s for single spectra,
a value that is roughly consistent with shot noise limits. The power
spectrum of the time series shows no evidence for Kjeldsen et al.'s
frequencies. With 95 % confidence, we can rule out the presence of these
13 frequencies with typical amplitudes of 0.5 m/s or more. The spectrum
is consistent with pure photon noise, but also with the presence of
pulsations having other frequencies (not those given by Kjeldsen et
al.) and with typical amplitudes as large as about 1.5 m/s. Possible
explanations for the discrepancy between the two results are (a) an
incorrect conversion between the amplitudes of equivalent width and
Doppler pulsations, and (b) a fluke in the noise behavior of one or
both observations.
---------------------------------------------------------
Title: Determining the AFOE's Radial Velocity Precision with Solar
Observations
Authors: Horner, S. D.; Brown, T. M.; Kennelly, E. J.; Noyes, R. W.;
Korzennik, S. G.; Nisenson, P.; Krockenberger, M.
1995AAS...187.7006H Altcode: 1995BAAS...27.1380H
The Advanced Fiber Optic Echelle (AFOE) is an instrument designed
for high precision radial velocity observations to detect extra-solar
planets and study stellar structure through asteroseismology. A 320 mu
m optical fiber is used to obtain solar observations during the day to
determine the precision of the instrument, and to study the relationship
between stellar activity and measured radial velocities. Here we
present the results of our analysis of solar data to determine the
short and long term radial velocity precision of the AFOE.
---------------------------------------------------------
Title: 51 Pegasi
Authors: Mayor, M.; Queloz, D.; Marcy, G.; Butler, P.; Noyes, R.;
Korzennik, S.; Krockenberger, M.; Nisenson, P.; Brown, T.; Kennelly,
T.; Rowland, C.; Horner, S.; Burki, G.; Burnet, M.; Kunzli, M.
1995IAUC.6251....1M Altcode:
M. Mayor and D. Queloz, Geneva Observatory, have reported the discovery
of a Jupiter-mass object in orbit around the solar-type star 51 Peg. The
announcement was made in Florence on Oct. 6 at the Ninth "Cambridge"
Workshop on "Cool Stars, Stellar Systems, and the Sun". The claim is
based on 18 months of precise Doppler measurements made with the ELODIE
spectrograph of the Observatoire de Haute-Provence. The parameters
of the orbital motion are as follows: P = 4.2293 +/- 0.0011 days,
e = 0 (assumed), K = 0.059 +/- 0.003 km/s, T0 = 2449797.773 +/-
0.036. The minimum mass of the companion is 0.47 +/- 0.02 Jupiter
mass. Alternative explanations for the radial-velocity variation
(pulsation or spot rotation) seem to be ruled out by the absence of any
significant corresponding photometric variation. Following the Oct. 6
announcement, confirmation of the 4.2-day radial-velocity variation
was obtained in mid-October by G. Marcy and P. Butler (San Francisco
State University, University of California at Berkeley) at the Lick
Observatory, as well as by a joint team from the Harvard-Smithsonian
Center for Astrophysics (R. Noyes, S. Korzennik, M. Krockenberger and
P. Nisenson), the High Altitude Observatory (T. Brown, T. Kennelly and
C. Rowland) and Pennsylvania State University (S. Horner). G. Burki,
M. Burnet and M. Kuenzli, Geneva Observatory and Lausanne University,
communicate: "Intensive photometric monitoring of 51 Peg has been
carried out at the European Southern Observatory. There is no evidence
for eclipses in the system. The rms of the V magnitude (on 17 nights)
is 0.037, two comparison stars being used. A 4.2-day photometric
variability larger than 0.002 mag can be ruled out."
---------------------------------------------------------
Title: Spots and Flares. (Book Reviews: Solar and Stellar Activity
Cycles.)
Authors: Noyes, Robert W.
1995Sci...269.1290W Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Spots and Flares. (Book Reviews: Solar and Stellar Activity
Cycles.)
Authors: Noyes, Robert W.
1995Sci...269.1290N Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Vorticity and Divergence in the Solar Photosphere
Authors: Wang, Yi; Noyes, Robert W.; Tarbell, Theodore D.; Title,
Alan M.
1995ApJ...447..419W Altcode:
We have studied an outstanding sequence of continuum images of the
solar granulation from Pic du Midi Observatory. We have calculated the
horizontal vector flow field using a correlation tracking algorithm,
and from this determined three scalar fields: the vertical component of
the curl, the horizontal divergence, and the horizontal flow speed. The
divergence field has substantially longer coherence time and more power
than does the curl field. Statistically, curl is better correlated
with regions of negative divergence that is, the vertical vorticity is
higher in downflow regions, suggesting excess vorticity in intergranular
lanes. The average value of the divergence is largest (i.e., outflow
is largest) where the horizontal speed is large; we associate these
regions with exploding granules. A numerical simulation of general
convection also shows similar statistical differences between curl
and divergence. Some individual small bright points in the granulation
pattern show large local vorticities.
---------------------------------------------------------
Title: Nightly Variations of Nonradial Oscillations in the Delta
Scuti Star upsilon Ursae Majoris
Authors: Korzennik, S. G.; Noyes, R. W.; Brown, T.; Nisenson, P.;
Horner, S.
1995ApJ...443L..25K Altcode:
We obtained spectra of the rapidly rotating Delta Scuti star
upsilon UMa with the Advanced Fiber Optic Echelle Spectrometer
(AFOE) on five successive nights in 1993 April, at a cadence of one
spectrum every 5 minutes over time periods averaging 4 hours on each
night. Cross-correlations of the spectra with a template spectrum from
a slowly rotating star of similar spectral type yielded the pattern
of features propagating across the lines, averaged over all spectral
lines recorded. The spacing of the features in wavelength and their
speed of motion across the line profile depend on the azimuthal order
m and frequency v of propagating oscillation modes. Using a Doppler
imaging analysis, we computed nightly absolute value of m-v diagrams;
these show several resolved modes with effective azimuthal order m
ranging from about 2 up to about 11, and frequencies between 130 and
170 microHz (i.e., periods between 2.1 and 1.6 hours). We identify
the observed modes as propagating prograde modes; the corresponding
retrograde modes are not observed. Viewed in a frame corotating
with the star with rotation speed of 116 km/s as derived from these
data, modes with m approximately 7 and with m approximately 11 have
approximately the same frequency (70 microHz). However, their relative
amplitude changes substantially from night to night, suggesting that
(1) the coherence time of the modes is not longer than about 1 day, or
(2) a possible coupling between modes of similar intrinsic frequencies
causes an alternating pattern of modal amplitude, or (3) beats are being
observed between unresolved modes of similar wavelength and frequency.
---------------------------------------------------------
Title: Chromospheric Variations in Main-Sequence Stars. II.
Authors: Baliunas, S. L.; Donahue, R. A.; Soon, W. H.; Horne, J. H.;
Frazer, J.; Woodard-Eklund, L.; Bradford, M.; Rao, L. M.; Wilson,
O. C.; Zhang, Q.; Bennett, W.; Briggs, J.; Carroll, S. M.; Duncan,
D. K.; Figueroa, D.; Lanning, H. H.; Misch, T.; Mueller, J.; Noyes,
R. W.; Poppe, D.; Porter, A. C.; Robinson, C. R.; Russell, J.; Shelton,
J. C.; Soyumer, T.; Vaughan, A. H.; Whitney, J. H.
1995ApJ...438..269B Altcode:
The fluxes in passbands 0.1 nm wide and centered on the Ca II H
and K emission cores have been monitored in 111 stars of spectral
type F2-M2 on or near the main sequence in a continuation of an
observing program started by O. C. Wilson. Most of the measurements
began in 1966, with observations scheduled monthly until 1980, when
observations were scheduled sevral times per week. The records, with
a long-term precision of about 1.5%, display fluctuations that can be
identified with variations on timescales similar to the 11 yr cycle of
solar activity as well as axial rotation, and the growth and decay of
emitting regions. We present the records of chromospheric emission and
general conclusions about variations in surface magnetic activity on
timescales greater than 1 yr but less than a few decades. The results
for stars of spectral type G0-K5 V indicate a pattern of change in
rotation and chromospheric activity on an evolutionary timescale, in
which (1) young stars exhibit high average levels of activity, rapid
rotation rates, no Maunder minimum phase and rarely display a smooth,
cyclic variation; (2) stars of intermediate age (approximately 1-2
Gyr for 1 solar mass) have moderate levels of activity and rotation
rates, and occasional smooth cycles; and (3) stars as old as the Sun
and older have slower rotation rates, lower activity levels and smooth
cycles with occasional Maunder minimum-phases.
---------------------------------------------------------
Title: Local Helioseismology: Analysis of Localized Time-Distance
Diagrams from Quiet and Active Regions
Authors: Korzennik, S. G.; Noyes, R. W.; Ziskin, V.
1995ASPC...76..268K Altcode: 1995gong.conf..268K
No abstract at ADS
---------------------------------------------------------
Title: The AFOE: A Spectrograph for Precision Doppler Studies
Authors: Brown, Timothy M.; Noyes, Robert W.; Nisenson, Peter;
Korzennik, Sylvain G.; Horner, Scott
1994PASP..106.1285B Altcode:
The Advanced Fiber Optic Echelle (AFOE) is a fiber-fed echelle
spectrograph designed for the measurement of stellar Doppler
shifts. Using a 2k x 2k CCD detector, it samples about 55% of the
wavelength range between 450 nm and 700 nm (20 echelle orders) at a
single shot, with spectral resolution R = 32000 to 70000 at 500 nm,
depending on the slit width employed. The AFOE employs a number of
devices to assure that the calibrations necessary for accurate Doppler
measurements can be properly performed. The most important of these
are: (1) coupling to the telescope via a double-scrambling optical
fiber system; (2) continuous calibration of the wavelength scale and
point-spread function by means of an atomic emission lamp entering the
spectrograph via a separate fiber and/or a molecular iodine absorption
cell; (3) availability of fiber-coupled sunlight for regular calibration
against the solar spectrum; (4) appropriate mechanical design and active
thermal control, yielding good mechanical stability. The AFOE is coupled
to the Tillinghast 1.5-m telescope at the F. L. Whipple Observatory. It
presently achieves S/N = 500 in the continuum near 500 nm in 60s when
observing Arcturus (alpha-Boo, m_V = -0.04). This noise level sets
a limit of about 0.7 ms^-1 to the Doppler precision attainable in
this length of observing time. Currently, our actual frame-to-frame
repeatability is worse than the photon noise limited value by about a
factor of 3 for this bright star, and about 1.5 for stars with m_V =
4. Work is continuing to refine data processing methods so that the
ultimate noise limit may be approached more closely, and to improve
the spectrograph's relatively low efficiency. (SECTION: Astronomical
Instrumentation )
---------------------------------------------------------
Title: Polaris the Cepheid: still pulsating.
Authors: Krockenberger, M.; Noyes, R. W.; Sasselov, D. D.
1994AAS...185.3603K Altcode: 1994BAAS...26.1366K
No abstract at ADS
---------------------------------------------------------
Title: Imaging spectroscopy of the solar CO lines at 4.67 microns
Authors: Uitenbroek, Han; Noyes, R. W.; Rabin, Douglas
1994ApJ...432L..67U Altcode:
We analyze spatially and temporally resolved spectra of the fundamental
vibration-rotation transitions of carbon monoxide (CO) in the solar
spectrum at 4.67 micrometers. Our observations imply that, in the quiet
Sun, spatial variations in CO intensity are largely dynamical in nature,
reinforcing the suggestion that dynamical effects play a key role in
the formation of the dark CO cores. Time sequences of resolved spectra
exhibit mainly 3 minute power in line-core intensity but mainly a 5
minute period in Doppler shift. The weak 7-6 R68 line shows normal
Evershed flow in the penumbra of a sunspot; we find evidence for the
onset of inverse Evershed flow in the strong 3-2 R14 line. Spectra at
the limb indicate that 3-2 R14 emission extends approximately 360 km
beyond the continuum limb.
---------------------------------------------------------
Title: 12 MU M Observations at the 1991 Eclipse
Authors: Jennings, D. E.; Deming, D.; McCabe, G.; Noyes, R.;
Wiedeinann, G.; Espenak, F.
1994IAUS..154..151J Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Velocity Fields in the Solar Atmosphere I. Preliminary Report
Authors: Leighton, R. B.; Noyes, R. W.; Simon, G. W.
1994snft.book..382L Altcode:
No abstract at ADS
---------------------------------------------------------
Title: New insight in the solar Tmin region from the CO lines at
4.67 micron
Authors: Uitenbroek, H.; Noyes, R. W.
1994chdy.conf..129U Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Recent array-detector Observations of the solar CO Fundamental
vibration--rotation Transitions at 4.67 microns
Authors: Uitenbroek, H.; Noyes, R. W.; Rabin, D.
1993AAS...183.5902U Altcode: 1993BAAS...25.1386U
We present recent observations of lines of the fundamental
vibration--rotation transitions of carbon monoxide (CO) in the solar
atmosphere obtained with the 256(2) infrared array detector at the
McMath telescope on Kitt Peak. Standard, plane parallel, solar models
have these lines form in LTE around the temperature minimum region;
they should be indicative of electron temperatures there. However,
matching observed line profiles in a standard solar model requires
temperatures as low as 3700 K which are not confirmed by any other
spectral diagnostic. We investigate whether this discrepancy can be
solved by invoking spatial inhomogeneities or temporal variations
or a combination of both. To this end we obtained series of
spectra-spectroheliograms at different positions on the disk as well
as time series of slit-spectra at a single position. The former type
of observations allow us to study spatial inhomogeneities in stronger
and weaker lines and the IR continuum at 4.6 microns and to distinguish
between variations due to the 5-minute oscillations and the more steady
patterns due to magnetic fields by comparing heliograms taken several
minutes apart. We also obtained spectra with the slit crossing the limb
giving us a more rigid registration of the intensity variations above
the limb as compared to previous single-detector measurements. Early
analysis shows that high and low excitation lines behave differently
at the limb which may bear information on the temperature structure
of the atmosphere just above the minimum.
---------------------------------------------------------
Title: Nightly Variations of Non-Radial Oscillations in the Delta
Scuti Star upsilon UMa
Authors: Korzennik, S.; Noyes, R.; Brown, T.; Nisenson, P.; Horner, S.
1993AAS...183.8405K Altcode: 1993BAAS...25.1423K
We observed the rapidly rotating Delta Scuti star upsilon UMa with the
Advanced Fiber Optic Echelle (AFOE) spectrometer at the Mt. Hopkins
1.5-m telescope on 5 successive nights in April 1993. Spectra covering
a total of 730 Angstroms were obtained at a 5-min cadence over about 4
hours on each night. The rotationally-broadened profiles of unblended
strong lines clearly show previously-seen “bumps" propagating from
the blue side to the red side of the lines. We isolated moving features
for each individual spectrum by subtracting the spectrum from the mean
spectrum for that night, normalizing to the latter. We then calculated
the cross-correlation function between each difference spectrum and
a standard template spectrum, which was a very high signal-to-noise
spectrum of a slowly-rotating star (Procyon) of similar spectral type,
obtained with the same instrument. The cross-correlation combines
the information from all the bumps moving across all spectral lines
(including rotationally-blended lines) into a single function of
displacement from line center, thereby significantly increasing
the signal-to-noise ratio of the moving features. Analysis of
the time-series of cross-correlation functions yields the rate of
propagation of features and their separation in velocity, which may be
interpreted in terms of effective azimuthal wavenumber and oscillation
frequency. Modes are identified by remapping the cross-correlation
functions in terms of longitude and performing two-dimensional Fourier
transforms. For each night a different modal pattern was found, usually
with several modes. The modes have effective azimuthal order m ranging
from about 2 up to about 12, and frequencies between 120 and 170 uHz
(i.e., 2.3 to 1.6 hours), with frequency gradually increasing with
increasing m. The relative amplitude of the different modes changes
substantially from night to night, suggesting either that the coherence
time of the modes is not longer than about a day, or that beats are
being observed between modes of similar wavelength and frequency.
---------------------------------------------------------
Title: Vorticity and Divergence in the Solar Granulation
Authors: Wang, Y.; Noyes, R. W.
1993BAAS...25.1184W Altcode:
No abstract at ADS
---------------------------------------------------------
Title: The Mechanisms of Solar Variability (MSV) program
Authors: Leibacher, John W.; Noyes, Robert W.; Simon, George W.;
Neidig, Donald F.
1993STIN...9328585L Altcode:
The Mechanisms of Solar Variability (MSV) Program aims toward
understanding physical causes of variations in the radiative, magnetic,
and particle emissions from the Sun. Solar particle and field variations
influence the interplanetary medium and the magnetosphere; UV and X-ray
variations affect the Earth's upper atmosphere; and total irradiance
variations are a possibly significant perturber of tropospheric
climate. Solar magnetic variability provides a close-up arena for
studying important but otherwise unobservable astrophysical phenomena
as well. The MSV program will advance our understanding of the causes
of solar variability through high angular resolution observations
of the interaction of solar surface magnetic fields and convective
motions, as well as related x-ray, ultraviolet, and visible brightness
variations. Through these high resolution studies, MSV will complement
national programs aimed at monitoring integrated solar outputs, thus
contributing to the better understanding and ultimate predictability
of global solar variability.
---------------------------------------------------------
Title: An Advanced Fiber Optic Echelle Spectrograph for
Asteroseismology
Authors: Noyes, R. W.; Brown, T. M.; Horner, S.; Korzennik, S.;
Nisenson, P.
1993ASPC...42..485N Altcode: 1993gong.conf..485N
No abstract at ADS
---------------------------------------------------------
Title: The AFOE - a new instrument for asteroseismology
Authors: Noyes, R. W.; Brown, T. M.; Horner, S.; Korzennik, S.;
Nisenson, P.
1993ASPC...40..752N Altcode: 1993IAUCo.137..752N; 1993ist..proc..752N
No abstract at ADS
---------------------------------------------------------
Title: Key issues - A round table discussion
Authors: Brown, T. M.; Demarque, P.; Noyes, R.; Praderie, F.; Roxburgh,
I. W.; Schatzman, E.
1993ASPC...40..776B Altcode: 1993ist..proc..776B; 1993IAUCo.137..776B
An overview of a round table discussion on the internal dynamics of
stars, some problems in stellar structure and evolution, a study of
stellar activity mechanisms using PRISMA, the seismology of sunlike
stars, and directions of future research is presented. It is concluded
that models that take into account just one physical process generally
do not agree with the observations. This provides evidence for the
presence of other physical processes. In each phenomenon which is
considered, a variety of physical processes are involved. All physical
processes should be taken into account simultaneously. Stars need to
be considered globally. It is recommended that attention be given to
such unsolved problems as the helium content of the sun, the abundance
of lithium in fast rotating stars, and the origin and evolution of
stellar magnetic fields.
---------------------------------------------------------
Title: Limb Observations of the 12.32 Micron Solar Emission Line
during the 1991 July Total Eclipse
Authors: Deming, Drake; Jennings, Donald E.; McCabe, George; Noyes,
Robert; Wiedemann, Gunter; Espenak, Fred
1992ApJ...396L..53D Altcode:
The limb profile of the Mg I 12.32-micron emission line is determined by
occultation in the July 11, 1991 total solar eclipse over Mauna Kea. It
is shown that the emission peaks are very close to the 12-micron
continuum limb, as predicted by recent theory for this line as a
non-LTE photospheric emission. The increase in optical depth for this
extreme limb-viewing situation indicates that most of the observed
emission arises from above the chromospheric temperature minimum,
and it is found that this emission is extended to heights well in
excess of the model predictions. The line emission can be observed
as high as 2000 km above the 12-micron continuum limb, whereas theory
predicts it to remain observable no higher than about 500 km above the
continuum limb. The substantial limb extension observed in this line
is quantitatively consistent with limb extensions seen in the far-IR
continuum, and it is concluded that it is indicative of departures
from gravitational hydrostatic equilibrium, or spatial inhomogeneities,
in the upper solar atmosphere.
---------------------------------------------------------
Title: Observational and theoretical investigations in solar
seismology
Authors: Noyes, Robert W.
1992sao..reptQ....N Altcode:
This is the final report on a project to develop a theoretical basis for
interpreting solar oscillation data in terms of the interior dynamics
and structure of the Sun. The topics covered include the following:
(1) studies of the helioseismic signatures of differential rotation
and convection in the solar interior; (2) wave generation by turbulent
convection; and (3) the study of antipodal sunspot imaging of an active
region tomography.
---------------------------------------------------------
Title: Non-LTE Effects on MG I Line Profiles in the Infrared Solar
Spectrum
Authors: Chang, E. S.; Avrett, E. H.; Mauas, P. J.; Noyes, R. W.;
Loeser, R.
1992ASPC...26..521C Altcode: 1992csss....7..521C
No abstract at ADS
---------------------------------------------------------
Title: Formation of the Infrared Emission Lines of MG i in the
Solar Atmosphere
Authors: Chang, E. S.; Avrett, E. H.; Mauas, P. J.; Noyes, R. W.;
Loeser, R.
1991ApJ...379L..79C Altcode:
A non-LTE radiative transfer investigation of the emission lines
is conducted at 7 and 12 microns using a realistic atomic model for
neutral magnesium. An average quiet sun atmospheric model is used to
calculate emission-line profiles that resemble the observed ones,
i.e., broad absorption troughs with narrow central emission, and
significant limb brightening. The charge exchange rates are found
to be significant, but the effects of high-n coupling between Mg
and Mg(+) together with radiative low-n transitions are of greater
importance. It is confirmed that the emission cores are formed no
higher than the temperature minimum region, and that the emission is
caused by non-LTE effects rather than by the chromospheric temperature
rise. It is inferred from the model calculations that the line core is
sensitive to magnetic fields located almost 400 km above those measured
in ordinary magnetograms; the gas pressure decreases 20-fold between
these two heights.
---------------------------------------------------------
Title: CA II H and K Measurements Made at Mount Wilson Observatory,
1966--1983
Authors: Duncan, Douglas K.; Vaughan, Arthur H.; Wilson, Olin C.;
Preston, George W.; Frazer, James; Lanning, Howard; Misch, Anthony;
Mueller, Jean; Soyumer, David; Woodard, L.; Baliunas, Sallie L.;
Noyes, Robert W.; Hartmann, Lee W.; Porter, Alain; Zwaan, Cornelis;
Middelkoop, Frans; Rutten, Rene G. M.; Mihalas, Dimitri
1991ApJS...76..383D Altcode:
Summaries are presented of the photoelectric measurements of stellar
Ca II H and K line intensity made at Mount Wilson Observatory during
the years 1966-1983. These results are derived from 65,263 individual
observations of 1296 stars. For each star, for each observing season,
the maximum, minimum, mean, and variation of the instrumental H and
K index 'S' are given, as well as a measurement of the accuracy of
observation. A total of 3110 seasonal summaries are reported. Factors
which affect the ability to detect stellar activity variations and
accurately measure their amplitudes, such as the accuracy of the H and K
measurements and scattered light contamination, are discussed. Relations
are given which facilitate intercomparison of 'S' values with residual
intensities derived from ordinary spectrophotometry, and for converting
measurements to absolute fluxes.
---------------------------------------------------------
Title: Formation of the Infrared Emission Lines of Mg I in the
Solar Atmosphere
Authors: Chang, E. S.; Avrett, E. H.; Mauas, P. J.; Loeser, R.; Noyes,
R. W.
1991BAAS...23.1029C Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Detection of Possible p-Mode Oscillations on Procyon
Authors: Brown, Timothy M.; Gilliland, Ronald L.; Noyes, Robert W.;
Ramsey, Lawrence W.
1991ApJ...368..599B Altcode:
In the course of a search for solar-like oscillations in bright
late-type stars, Doppler variability was observed in the F5 subgiant
Procyon. The variations have frequencies within a 1.1 mHz range
centered at 0.9 mHz, and a total rms amplitude within that range
of 2.5 m/s. Observations of Arcturus and scattered sunlight made
with the same equipment during the same time interval show no such
variation, indicating that the variations seen on Procyon are of stellar
origin. The Doppler signal seen is entirely consistent with solar-like
p-modes on Procyon, with maximum mode amplitudes of about 50 cm/s
and periods around 20 minutes. Several statistical tests support the
identification for the signal with narrow-band oscillations, but none
does so conclusively. Assuming that the signal does arise from p-modes,
there is evidence that the frequency splitting nu(0) is 71 micro-Hz. The
data do not permit a definite estimate of this quantity, and other
values of nu(0) fit the observations about equally well. In order to
clarify the sources of ambiguity in this and similar observations,
the data acquisition, reduction, and interpretation are described.
---------------------------------------------------------
Title: A new technique for study of radial velocity changes.
Authors: Ramsey, L.; Brown, T.; Gilliand, R.; Noyes, R.
1991ASPC...20..614R Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Working papers. Astronomy and astrophysics panel reports.
Authors: Bahcall, John N.; Beichman, Charles A.; Canizares, Claude;
Cronin, James; Heeschen, David; Houck, James; Hunten, Donald; McKee,
Christopher F.; Noyes, Robert; Ostriker, Jeremiah P.
1991wpaa.book.....B Altcode:
This volume contains the working papers of the panels appointed by
the Astronomy and Astrophysics Survey Committee. These papers were
advisory to the survey committee and represent the opinions of the
members of each panel in the context of their individual charges. The
committee's full survey report is contained in a separately published
document, The decade of discovery in astronomy and astrophysics
(see 003.025). Contents: 1. Radio astronomy. 2. Infrared
astronomy. 3. Optical/IR from ground. 4. UV-optical from
space. 5. Interferometry. 6. High energy from space. 7. Particle
astrophysics. 8. Theory and laboratory astrophysics. 9. Solar
astronomy. 10. Planetary astronomy. 11. Computing and data
processing. 12. Policy opportunities. 13. Benefits to the nation from
astronomy and astrophysics. 14. Status of the profession. 15. Science
opportunities.
---------------------------------------------------------
Title: Solar astronomy
Authors: Rosner, Robert; Noyes, Robert; Antiochos, Spiro K.; Canfield,
Richard C.; Chupp, Edward L.; Deming, Drake; Doschek, George A.;
Dulk, George A.; Foukal, Peter V.; Gilliland, Ronald L.
1991aap..reptR....R Altcode:
An overview is given of modern solar physics. Topics covered include
the solar interior, the solar surface, the solar atmosphere, the Large
Earth-based Solar Telescope (LEST), the Orbiting Solar Laboratory, the
High Energy Solar Physics mission, the Space Exploration Initiative,
solar-terrestrial physics, and adaptive optics. Policy and related
programmatic recommendations are given for university research and
education, facilitating solar research, and integrated support for
solar research.
---------------------------------------------------------
Title: What can other stars tell us about the Sun?
Authors: Noyes, Robert W.; Baliunas, S. L.; Guinan, E. F.
1991sia..book.1161N Altcode:
The authors focus on those aspects of the solar-stellar connection where
observations of other stars give information about the Sun which could
not be obtained from study of the Sun alone. Solar-like phenomena
on other stars with a range of values for key parameters (e.g.,
rotation) yield the dependence on those parameters and hence better
physical insight into the governing mechanisms. A key presumption is
that the Sun is a normal star, so that the same mechanisms govern its
behavior. Also if the Sun is normal, then study of stars with similar
masses but different ages gives information on the evolution of solar
properties, such as structure, internal dynamics, activity, etc. First,
the authors discuss stellar observations which yield information on
the internal structure of solar-like stars, including central density,
and helium abundance. Such results support the standard value for
the solar helium abundance, as well as standard stellar structure
theory. The authors note how stellar seismology can, in principle,
determine the stellar radius, as well as the degree of mixing in stellar
cores, as a function of age. Next, the authors discuss information
on the internal dynamics of the Sun, and its evolution, as inferred
from the study of the time history of surface rotation in solar-type
stars. They use the rotation-activity-age connection to infer how the
Sun's rotation and activity level has changed with age. The authors
discuss what the dependence of activity on mass and rotation can
tell us about the nature and location of the solar dynamo. Finally,
they discuss the solar activity cycle and its likely change over the
lifetime of the Sun, inferred from observation of other stars.
---------------------------------------------------------
Title: Temporal Variations in Solar Chromospheric and Coronal
Extreme-Ultraviolet Lines and Implications for Heating Mechanisms
Authors: Matheson, T. D.; Noyes, R. W.
1990BAAS...22..852M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Leo Goldberg, 26 January 1913 - 1 November 1987.
Authors: Dalgarno, A.; Layzer, D.; Noyes, R.; Parkinson, W.
1990PhT....43b.144D Altcode:
No abstract at ADS
---------------------------------------------------------
Title: The Sun
Authors: Noyes, Robert W.
1990nssy.book...15N Altcode:
No abstract at ADS
---------------------------------------------------------
Title: High resolution optical imaging through the atmosphere
Authors: Noyes, R. W.; Nisenson, P.; Stachnik, R. V.; Papaliolios, C.
1989sao..rept.....N Altcode:
This program has concentrated on three major areas: the application
of high angular resolution image reconstruction techniques to the
reconstruction of solar surface features; speckle imaging of a wide
range of astronomical sources; and the implementation of adaptive
optics for faint object imaging. Substantial modifications were made
to a technique for reconstruction of high resolution images from single
short exposure solar frames, blind iterative deconvolution (IDC). These
improvements were tested using numerical simulation data. Analysis of
speckle data of the supernova SN1987A has detected a new bright source,
0.9 arcseconds south of the SN, as well as substantial structure in
the region surrounding the SN. New results were obtained on several
Young Stellar Objects and supergiants. In the area of adaptive
optics, an AOA wavefront sensor has been set up and tested using an
image intensifier which increases its sensitivity by three orders of
magnitude. Faint object image active tilt correction was also tested
with some important enhancements, including new highly linear and
sensitive CCD quad cells developed by Cal Tech and Tektronix, and
an off-the-shelf high speed 2-D tilting mirror with greatly improved
specifications. The effects of only partially correcting atmospheric
turbulence have been theoretically analyzed and numerically simulated.
---------------------------------------------------------
Title: Ca II H and K Flux Monitoring in Cool Stars: Rotation and
Activity Cycles
Authors: Robinson, C. R.; Baliunas, S. L.; Bennett, W.; Briggs, J.;
Frazer, J.; Noyes, R. W.; Shelton, C.; Woodard, L.; Vaughan, A. H.;
Wilson, O. C.
1989BAAS...21.1115R Altcode:
No abstract at ADS
---------------------------------------------------------
Title: The Mount Wilson Observatory HK Project: The Continuing
Analysis of Rotation and Stellar Magnetic Cycles
Authors: Baliunas, S. L.; Bennett, W.; Briggs, J.; Frazer, J.; Noyes,
R. W.; Robinson, C. R.; Shelton, C.; Woodard, L.; Vaughan, A. H.;
Wilson, O. C.
1988BAAS...20Q.994B Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Stellar Activity Cycles and Rotation in Cool Stars Observed
from Mt. Wilson Observatory
Authors: Baliunas, S. L.; Briggs, J.; Frazer, J.; Noyes, R. W.;
Robinson, C. R.; Carroll, S.; Donahue, R. A.; Shelton, C.; Woodard,
L.; Vaughan, A. H.; Wilson, O. C.
1988BAAS...20Q.697B Altcode: 1988BAAS...20Z.697B
No abstract at ADS
---------------------------------------------------------
Title: The Precision Calcium Photometer - a New Instrument for
Asteroseismology
Authors: Nisenson, P.; Dupree, A. K.; Noyes, R. W.
1988IAUS..123..521N Altcode:
The Precision Calcium Photometer has been built with characteristics
optimized for amplitude astroseismology. A description of the instrument
and of laboratory and on-telescope test runs are discussed here.
---------------------------------------------------------
Title: Time Variations of the Frequencies of Low-Degree Solar P-Modes
Authors: Woodard, M. F.; Noyes, R. W.
1988IAUS..123..197W Altcode:
A comparison of three separate years (1980, 1984, 1985) of SMM/ACRIM
solar total irradiance data reveals small but significant changes in
the frequencies of low-degree solar p-modes.
---------------------------------------------------------
Title: Detection of a Very Bright Source Close to the LMC Supernova
SN 1987A: Erratum
Authors: Nisenson, P.; Papaliolios, C.; Karovska, M.; Noyes, R.
1988ApJ...324L..35N Altcode:
In the Letter "Detection of a Very Bright Source Close to the LMC
Supernova SN 1987A" by P. Nisenson, C. Papaliolios, M. Karovska,
and R. Noyes (1987 Ap. J. [Letters], 320, L15), two of the figure
labels for Figure 1 were inadvertently transposed in the production
process. A corrected version of the figure appears as Plate L4. The
Journal regrets the error.
---------------------------------------------------------
Title: Space Observations of Solar and Stellar Oscillations
Authors: Noyes, R. W.
1988IAUS..123..527N Altcode:
A number of space investigations in helio- and asteroseismology
presently under definition or development are briefly discussed.
---------------------------------------------------------
Title: Detection of a Very Bright Source Close to the LMC Supernova
SN 1987A
Authors: Nisenson, P.; Papaliolios, C.; Karovska, M.; Noyes, R.
1987ApJ...320L..15N Altcode:
High angular resolution observations of the supernova in the Large
Magellanic Cloud, SN 1987A, have revealed a bright source separated
from the SN by approximately 60 mas with a magnitude difference of 2.7
at 656 nm (H-alpha). Speckle imaging techniques were applied to data
recorded with the CfA two-dimensional photon counting detector on the
CTIO 4 m telescope on March 25 and April 2 to allow measurements in
H-alpha on both nights and at 533 nm and 450 nm on the second night. The
nature of this object is as yet unknown, though it is almost certainly
a phenomenon related to the SN.
---------------------------------------------------------
Title: An investigation of short period oscillations of the solar
irradiance and their time variations
Authors: Noyes, Robert W.
1987sao..rept.....N Altcode:
Measurements of solar irradiance fluctuations by the Active Cavity
Radiometer (ACRIM) instrument onboard the Solar Maximum Mission
(SMM) show variations on a time scale of about 5 minutes due to
solar p-mode oscillations, as well as longer-term variations related
to solar magnetic activity. The question was studied whether the
p-mode frequencies change with time as a result of changing solar
structure associated with the activity cycle. The ACRIM data on SMM
are particularly well-suited for this purpose, because the instrument
operated continuously from February 1980 to December 1980 and again
from May 1984 to the present. The main activity entailed a detailed
study of the observational data to determine if a change in the p-mode
frequencies is evident from the time of solar maximum to that of solar
minimum. It was concluded that the measured eigenfrequencies were
significantly higher during the 1980 time frame than during the 1984
to 1986 time frame. The conclusion that there is significant change in
the eigenfrequencies with the activity cycle remains only tentative,
and needs confirmation from analysis of more data during the upcoming
solar maximum.
---------------------------------------------------------
Title: The Solar P-Mode Signal as a Function of Optical Wavelength;
3800 through 4400 A. and 6500 through 6900 A.
Authors: Ronan, R. S.; Harvey, J. W.; Duvall, T. L.; Noyes, R. W.
1987BAAS...19..936R Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Detection of a Very Bright Close Companion Source to SN1987A
Authors: Nisenson, P.; Karovska, M.; Noyes, R.; Papaliolios, C.
1987BAAS...19..950N Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Supernova 1987A in the Large Magellanic Cloud
Authors: Karovska, M.; Nisenson, P.; Noyes, R.; Papaliolios, C.;
McNaught, R.; Seargent, D. A. J.
1987IAUC.4382....2K Altcode: 1987IAUC.4382....1K; 1987IAUC.4382....0K
M. Karovska, P. Nisenson, R. Noyes, and C. Papaliolios, Center for
Astrophysics, write: "High-angular-resolution speckle observations of
SN 1987A on Mar. 25 and Apr. 2 using the Cerro Tololo Interamerican
Observatory 4-m telescope (with the CfA PAPA photon- counting detector)
show a bright feature with a separation of 0".057 +/- 0".014 at
p.a. 194 deg +/- 5 deg relative to the SN. This feature appears to
be 2.7 +/- 0.2 mag fainter than the SN in a 10-nm bandpass centered
on 656.3 nm (H-alpha). A corresponding feature was detected in a
10-nm bandpass centered at 533 nm, though it appears to be somewhat
fainter than in H-alpha. Preliminary analysis of data recorded in
a 10- nm bandpass centered at 450 nm shows no evidence of an object
within a 4-mag difference from the SN. Data from nearby comparison
stars, recorded close in time using the same filters, produced clean,
point-like images with no structure above the noise at the separation
and position angle of the observed feature." Corrigendum. On IAUC
4370, lines 7-15, for mm read microns Visual magnitude estimates:
Apr. 28.51 UT, 3.0 (R. McNaught, Siding Spring Observatory); 29.38,
3.0 (D. A. J. Seargent, The Entrance, N.S.W.); 30.43, 2.9 (McNaught).
---------------------------------------------------------
Title: High Angular Resolution Speckle Imaging of α Ori
Authors: Karovska, M.; Nisenson, P.; Noyes, R.
1987BAAS...19..755K Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Speckle Imaging at CfA
Authors: Nisenson, P.; Karovaka, M.; Noyes, R.; Papaliolios, C.;
Stachnik, R.; Strom, S.; Edwards, S.
1987BAAS...19Q.748N Altcode: 1987BAAS...19..748N
No abstract at ADS
---------------------------------------------------------
Title: The solar chromosphere
Authors: Noyes, R. W.; Avrett, E. H.
1987soap.conf..125N Altcode: 1987sap..book..125N
Observational data on the solar chromosphere (SC) are compiled in
tables and graphs and illustrated with sample spectra and H-alpha
filtergrams. The visible structure of the SC in active and quiet regions
is discussed; the mean SC structure determined from spectroscopic
observations is characterized; and particular attention is given to
plages and network, the role of magnetic fields, small-scale structure,
and the structure and dynamics of the high SC. From the similarity
in the thermal structures of magnetic and nonmagnetic SC regions it
is inferred that slow-mode MHD waves are the most likely mechanism
of energy transport, although high-angular-resolution observations
are required to verify this hypothesis. The implications of recent
stellar-chromosphere observations for SC models are briefly considered.
---------------------------------------------------------
Title: Rotation and magnetic activity in main-sequence stars.
Authors: Hartmann, Lee W.; Noyes, Robert W.
1987ARA&A..25..271H Altcode:
The authors discuss recent observational results on how rotation
interacts with convection to produce stellar magnetic fields. They
concentrate on the activity of main-sequence stars. They sketch the
evolution of stellar rotation from pre-main-sequence to main-sequence
phases. Some implications of this rotational evolution for internal
velocity fields, and therefore for the dynamo processes, are
noted. Surface manifestations of magnetic activity, thought to be
generated by the magnetic dynamo acting within rotating, convecting
stars, and how this activity depends on mass, rotation, and age are
discussed. The authors summarize the present state of our understanding
of rotation and magnetic activity in main-sequence stars and outline
some promising areas for future work.
---------------------------------------------------------
Title: On the Alpha Orionis Triple System
Authors: Karovska, M.; Nisenson, P.; Noyes, R.
1986ApJ...308..260K Altcode:
Detection of two close optical companions to the red supergiant α
Ori was accomplished in 1983 November on the Steward Observatory
2.25 m telescope. A new two-dimensional photon counting camera
was used for data recording, and speckle imaging was used for
image reconstruction. The closer of the two sources is located at
0arcsec.06±0arcsec.01 from α Ori (P.A. = 273°), the more distant at
0arcsec.51±0arcsec.01 (P.A. = 278°). An analysis of these results
and of earlier polarization data favors an interpretation in which
the two optical sources are stellar companions to α Ori.
---------------------------------------------------------
Title: Rotation and Long-term Activity in Evolved Stars
Authors: Baliunas, S. L.; Donahue, R. A.; Noyes, R. W.; Duncan, D. K.;
Frazer, J.; Misch, A.; Mueller, J.; Woodard, L.; Vaughan, A. H.
1986BAAS...18Q.983B Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Book-Review - Solar-Space Observations and Stellar Prospects
Authors: Harvey, J. W.; Stenflo, J. O.; Hudson, H. S.; Noyes, R. W.;
Kotrc, P.
1986BAICz..37..252H Altcode:
No abstract at ADS
---------------------------------------------------------
Title: High resolution astrophysical observations using speckle
imaging
Authors: Noyes, R. W.; Nisenson, P.; Papaliolios, C.; Stachnik, R. V.
1986sao..reptQ....N Altcode:
This report describes progress under a contract to develop a complete
astronomical speckle image reconstruction facility and to apply that
facility to the solution of astronomical problems. During the course
of the contract we have developed the procedures, algorithms, theory
and hardware required to perform that function and have made and
interpreted astronomical observations of substantial significance. A
principal result of the program was development of a photon-counting
camera of innovative design, the PAPA detector. Development of this
device was, in our view, essential to making the speckle process into
a useful astronomical tool, since the principal impediment to that
circumstance in the past was the necessity for application of photon
noise compensation procedures which were difficult if not impossible
to calibrate. The photon camera made this procedure unnecessary and
permitted precision image recovery. The result of this effort and the
associated algorithm development was an active program of astronomical
observation which included investigations into young stellar objects,
supergiant structure and measurements of the helium abundance of the
early universe. We have also continued research on recovery of high
angular resolution images of the solar surface working with scientists
at the Sacramento Peak Observatory in this area.
---------------------------------------------------------
Title: Development of a CCD based solar speckle imaging system
Authors: Nisenson, Peter; Stachnik, Robert V.; Noyes, Robert W.
1986sao..reptR....N Altcode:
A program to develop software and hardware for the purpose of obtaining
high angular resolution images of the solar surface is described. The
program included the procurement of a Charge Coupled Devices imaging
system; an extensive laboratory and remote site testing of the
camera system; the development of a software package for speckle
image reconstruction which was eventually installed and tested at
the Sacramento Peak Observatory; and experiments of the CCD system
(coupled to an image intensifier) for low light level, narrow spectral
band solar imaging.
---------------------------------------------------------
Title: Solar and stellar magnetic activity.
Authors: Noyes, R. W.
1986psun....3..125N Altcode:
Contents: Solar and stellar magnetic activity: a phenomenological
comparison (surface magnetic fields and their effects on stellar
radiative flux, direct detection of magnetic fields on stars like
the Sun, Ca II H and K emission as indicators of stellar magnetic
fields, coronal active regions, magnetic activity cycles). The
rotation/activity/age connection (the aging of magnetic activity and
rotation, rotation as the fundamental determinant of magnetic activity,
the influence of convection zone properties, the Vaughan-Preston gap,
the evolution of rotation and magnetic activity on the Sun). Avenues
for future research (observational studies of solar magnetic activity,
observational studies of stellar magnetic activity, theoretical
studies).
---------------------------------------------------------
Title: Change of solar oscillation eigenfrequencies with the solar
cycle
Authors: Woodard, M. F.; Noyes, R. W.
1986ASIC..169..303W Altcode: 1986ssds.proc..303W
No abstract at ADS
---------------------------------------------------------
Title: Companions to α Orionis
Authors: Karovska, M.; Nisenson, P.; Noyes, R. W.; Stachnik, R.
1986LNP...254..445K Altcode: 1986csss....4..445K
Detection of two close optical companions to the red supergiant a
Ori was accomplished using the PAPA detector for data recording,
and speckle imaging for image reconstruction. Our analysis favors an
interpretation in which the two optical sources are stellar companions
to a Ori.The observed time dependent variations of the polarization of
a Ori can be interpreted as being due to a systemic asymmetry created
by one of the companions.
---------------------------------------------------------
Title: Change of solar oscillation eigenfrequencies with the solar
cycle
Authors: Woodard, Martin F.; Noyes, Robert W.
1985Natur.318..449W Altcode:
Solar acoustic eigenfrequencies depend on the internal structure of the
Sun, which may change during the 11-yr cycle of magnetic activity as a
result of various effects associated with the solar dynamo. Observations
of low-degree acoustic frequencies were made, using the ACRIM instrument
on the Solar Maximum Mission (SMM) satellite, in 1980 (near solar
maximum) and 1984 (near solar minimum). The analysis of these data,
presented here, indicates that the frequencies of l = 0 and l = 1
acoustic modes in the 5-min band have decreased from 1980 to 1984,
by ~0.42 µHz or 1.3 parts in 10<SUP>4</SUP>. This finding may have
important implications for our understanding of the mechanism of the
solar activity cycle.
---------------------------------------------------------
Title: Book-Review - Solar / Space Observations and Stellar Prospects
Authors: Harvey, J. W.; Hudson, H. S.; Noyes, R. W.; Zirker, J. B.
1985Sci...230..660H Altcode:
No abstract at ADS
---------------------------------------------------------
Title: A new optical source associated with T Tauri.
Authors: Nisenson, P.; Stachnik, R. V.; Karovska, M.; Noyes, R.
1985ApJ...297L..17N Altcode:
A faint optical source close to T Tauri has been detected using speckle
imaging techniques in a photon-counting mode of operation. This second
optical source is located at position angle 358°±5° with a separation
of 0arcsec.27±0arcsec.04 from the optical astrometric position of T
Tauri. The visual magnitude difference with respect to the primary,
measured at 521 nm, is m<SUB>v</SUB> = 4.33±0.09. Since the new source
is located north of T Tauri, it is distinct from the radio/infrared
object recently reported to be located 0arcsec.61 south of T Tauri. If
the new source is a stellar object, it appears to have a mass of
between 0.2 and 0.35 M_sun; and has a surface temperature of 3000±200K.
---------------------------------------------------------
Title: Stellar Analogs of Solar Magnetic Activity
Authors: Noyes, R. W.
1985SoPh..100..385N Altcode:
The techniques and principal results of observational studies of stellar
activity are summarized. Both chromospheric and coronal emission clearly
track surface magnetic field properties, but it is not well known how
the detailed relation between the emission and surface magnetic fields
varies with spectral type. For lower Main-Sequence stars of the same
spectral type, there is clear evidence of a close relationship between
mean activity level and rotation period P<SUB>rot</SUB>. There is
also less definitive evidence for a similar dependence on convective
overturn time τ<SUB>c</SUB>, such that activity depends on the single
parameter Ro = P<SUB>rot</SUB>/τ<SUB>c</SUB>. For single stars, stellar
rotation, and magnetic activity both decline smoothly with age. This
implies a feedback between angular momentum loss rate and activity
level. Temporal variations in mean stellar activity level mimic the
solar cycle only for old stars like the Sun, being much more irregular
for younger stars. The characteristic timescale of the variations (the
`cycle period') appears to depend on Ro for old stars, but shows no
clear dependence on either rotation rate or spectral type for younger
stars. Further data on mean activity and its variation for a large
number of lower Main-Sequence stars should contribute significantly
to our understanding of the causes of stellar magnetic activity.
---------------------------------------------------------
Title: The extreme ultraviolet spectrum of sunspot plumes. I -
Observations
Authors: Noyes, R. W.; Raymond, J. C.; Doyle, J. G.; Kingston, A. E.
1985ApJ...297..805N Altcode:
A complete extreme ultraviolet spectrum of a sunspot plume by the Skylab
S-055 spectroheliometer is presented, and the relevant observational
details are discussed. Identifications and intensities are given for
emission lines and continua in the 303-1343 A range. The emission from
lines found between 100,000 and a million K are enhanced by up to a
factor of 40 compared with quiet and active region spectra. The emission
measure curve for the mean spectrum shows a high double peak at log T
= 5.7 and 6.0, reflecting the very inhomogeneous spatial structure of
the sunspot plumes. The extremely high signal to noise of the spectrum
is used to investigate the electron density and ionization stage of
the gas based on line ratio techniques. A model of line emission from
a gas cooling by radiation alone at constant density is presented,
and the observations are compared with various semiempirical and
theoretical models.
---------------------------------------------------------
Title: The Extreme Ultraviolet Spectrum of Sunspot Plumes - Part Two -
Spectral Diagnostics and Implications for Cooling
Authors: Doyle, J. G.; Raymond, J. C.; Noyes, R. W.; Kingston, A. E.
1985ApJ...297..816D Altcode:
The extreme ultraviolet emission-line spectrum of very intense sunspot
plumes is analyzed. Several of the standard density diagnostics
suggest a constant density, rather than constant pressure, emitting
region. Temperature diagnostic line ratios of several ions yield
temperatures below those expected in ionization equilibrium (and
observed in the quiet Sun). This provides strong evidence for the
suggestion that the internal energy of cooling, falling gas accounts for
the observed radiation. The lack of such departures from equilibrium in
the quiet Sun demonstrates that downflows are not the dominant source
of energy at transition region temperatures. We assess the accuracy
of several atomic rate coefficients.
---------------------------------------------------------
Title: Helioseismology
Authors: Leibacher, J. W.; Noyes, R. W.; Toomre, J.; Ulrich, R. K.
1985SciAm.253c..48L Altcode: 1985SciAm.253...48L
Oscillations of the sun's surface are due to sound waves resonating in
the solar interior. In actual observations, such surface displacements
are evidenced in the form of Doppler shifts in the wavelengths of
light that are absorbed by the moving gases, and as variations in
brightness. The spatial pattern and period of surface oscillation
allows investigators to deduce the three-dimensional structure of the
resonance, and to infer properties of the solar interior. Reflection
and refraction below the solar surface confine sound waves within
acoustic cavities. Such trapped waves interfere constructively with
themselves as they circle the sun, creating the resonances that are
detectable as solar surface oscillations.
---------------------------------------------------------
Title: Book-Review - Solar Space Observations and Stellar Prospects
Authors: Harvey, J. W.; Hudson, H. S.; Noyes, R. W.
1985Natur.317...91H Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Helioseismology.
Authors: Leibacher, J. W.; Noyes, R. W.; Toomre, J.; Ulrich, R. K.
1985SciAm.253c..34L Altcode: 1985SciAm.253...34L
Acoustic waves within the sun are visible as oscillations on the solar
surface. Their pattern and period hold clues to structure, composition
and dynamics in the sun's interior.
---------------------------------------------------------
Title: Book-Review - Solar / Space Observations and Stellar Prospects
Authors: Harvey, J. W.; Hudson, H. S.; Noyes, R. W.
1985Sci...229..787H Altcode:
No abstract at ADS
---------------------------------------------------------
Title: A study of ultraviolet and X-ray emissions of selected
solar regions
Authors: Schrijver, C. J.; Zwaan, C.; Maxson, C. W.; Noyes, R. W.
1985A&A...149..123S Altcode:
Apollo Telescope Mount-based Skylab observations of quiet regions,
coronal holes, and active regions of various sizes and in various stages
of evolution are studied. Total intensities in coronal emissions are
noted to increase more rapidly than linearly with total intensities in
chromospheric emissions, and areas of active regions determined from
chromospheric emissions are found to be systematically larger than
areas determined from transition region emissions. The coronal X-ray
temperature, as well as the average intensities of active regions,
depend on the area of the active region, on Ca II intensity, and on
relative coverage by sunspots.
---------------------------------------------------------
Title: Time-series measurements of chromospheric CA II H and K
emission in cool stars and the search for differential rotation.
Authors: Baliunas, S. L.; Horne, J. H.; Porter, A.; Duncan, D. K.;
Frazer, J.; Lanning, H.; Misch, A.; Mueller, J.; Noyes, R. W.; Soyumer,
D.; Vaughan, A. H.; Woodard, L.
1985ApJ...294..310B Altcode:
The relative strength of the chromospheric Ca II H and K emission cores
has been monitored on a near- nightly basis during several seasons
in a variety of cool stars, predominantly those lower-main-sequence
stars observed by Wilson for long-term chromospheric activity
fluctuations. From initial data obtained in 1980, rotation rates had
been inferred from the period of modulation of chromospheric flux. We
have analyzed the rotation periods determined from three seasons of
Ca II H and K emission strengths in these stars. In 12 stars we find
evidence for varying periodicities in different seasons or for multiple
periodicities in one season, or both. For about 10 stars, significant
peaks in the power spectrum are found at two different frequencies in
at least one season. Detailed analysis of the chromospheric emission
with time reveals two possibilities consistent with the appearance
of dual periodicities in the observed time series: two distinct
periods arising from active areas rotating differentially with
respect to each other because they are at different latitudes, or
the growth and decay of active areas with subsequent birth of active
areas occurring at a stellar longitude different from the original
site of the activity. Generally, the data from only one season cannot
discriminate between these two explanations of dual peaks in the power
spectra. In four stars, however, differential surface rotation is a
more likely explanation for the observed chromospheric fluctuations
with time during the first three seasons. The fractional differential
surface rotation would be at least 5% in HD 206860, 10% in HD 101501,
11% in HD 190406 and 21% in HD 114710. The analysis of the data for
the GO V star HD 206860, with a relatively rapid rotation period of
about 5 days, indicates an active area persisting for three years.
---------------------------------------------------------
Title: Speckle Image Reconstruction of a Northern Optical Companion
to T Tau
Authors: Nisenson, P.; Karovska, M.; Stachnik, R.; Noyes, R.
1985BAAS...17..556N Altcode:
No abstract at ADS
---------------------------------------------------------
Title: On a Possible Close Companion to αOri
Authors: Karovska, M.; Noyes, R. W.; Roddier, F.; Nisenson, P.;
Stachnik, R. V.
1985BAAS...17..598K Altcode:
No abstract at ADS
---------------------------------------------------------
Title: T Tauri
Authors: Karovska, M.; Nisenson, P.; Noyes, R.; Papaliolios, C.;
Stachnik, R.
1985IAUC.4039....2K Altcode: 1985IAUC.4039....0K
M. Karovska, P. Nisenson, R. Noyes, C. Papaliolios and R. Stachnik,
Center for Astrophysics, write: "Speckle image reconstructions
of T Tau show a second, unresolved source located ~ 0"35 from T
Tau at p.a. ~ 5 deg. The source was first detected at the Steward
Observatory's 2.3-m telescope in 1983 Nov., and it was detected again
using the 2.5-m telescope at Mt. Wilson Observatory in 1984 Nov.,
thus confirming its reality. Both sets of data were obtained through
broad-band filters centered near 660 nm (and including H=alpha), using
a two-dimensional photon-counting PAPA detector. The source appears
to be ~ 4 mag fainter than T Tau itself in this wavelength band. We
note that this appears to be a third component of the T Tau system;
it is not the object reported by infrared and radio observers as
being south of T Tau. Further optical or infrared observations of T
Tau during the remainder of this observing season would be most useful."
---------------------------------------------------------
Title: Report of IAU Commission 12: Radiation and structure of the
solar atmosphere (Radiation et structure de l'atmosphère solaire).
Authors: Noyes, R. W.
1985IAUTA..19...97N Altcode:
No abstract at ADS
---------------------------------------------------------
Title: A Search for Differential Rotation in Cool Stars Using Ca II
H and K Emission
Authors: Porter, A. C.; Baliunas, S. L.; Horne, J. H.; Noyes, R. W.;
Duncan, D. K.; Frazer, J.; Lanning, H.; Misch, A.; Mueller, J.;
Soyumer, D.; Vaughan, A. H.; Woodard, L.
1985BAAS...17..512P Altcode:
No abstract at ADS
---------------------------------------------------------
Title: The relation between stellar rotation rate and activity
cycle periods.
Authors: Noyes, R. W.; Weiss, N. O.; Vaughan, A. H.
1984ApJ...287..769N Altcode:
The empirical relation between rotation period, spectral type, and
cycle activity period in 13 slowly rotating main-sequence stars is
investigated, on the basis of available spectrometric data. It is
shown that for slowly rotating stars with similar spectral types, the
cycle period P(cyc), and rotation period P(rot) were related such that
P(cyc) varies as P(rot) to the nth, where n equals 1.25. In a group of
stars with individual spectral types from G2 to K7, the cycle periods
were consistent with the relation P(cyc) is approximately equal to (P
rot/tau<SUB>c)</SUB> exp n, where tau<SUB>c</SUB> is the convective
turnover time near the bottom of the convection zone. On the basis
of the above relations, it is suggested that an increase of P(cyc)
with increasing P(rot) does not agree with conventional estimates from
nonlinear dynamo models, and is limited by two factors: the quenching
of the alpha effect; and differential rotation.
---------------------------------------------------------
Title: Evidence for global oscillations in the K2 dwarf epsilon
Eridani.
Authors: Noyes, R. W.; Baliunas, S. L.; Belserene, E.; Duncan, D. K.;
Horne, J.; Widrow, L.
1984ApJ...285L..23N Altcode:
Evidence of global p-mode oscillations in the K2 V star Epsilon Eridani,
based on observed time variations in the Ca II H and K emission lines,
is presented. Power spectra of time series of Ca II intensity measures
reveal a number of peaks spaced at about 86 and 172 micro-Hz. The
172 micro-Hz spacing is significantly larger than the corresponding
spacing observed for solar p-mode oscillations but is in excellent
agreement with predictions for a star of the known radius of Epsilon
Eri. The amplitude of the oscillations seen in the H and K flux of this
chromospherically active star is much larger than in the sun. Peak
power in the H and K fluctuations occurs at periods near 10 minutes,
in contrast to predictions of peak oscillation amplitude near four
minutes for a K2 dwarf.
---------------------------------------------------------
Title: Activity Cycles of Lower Main-Sequence Stars: Eighteen Years
of Research
Authors: Baliunas, S. L.; Donahue, R. A.; Horne, J. H.; Noyes, R. W.;
Porter, A.; Gilliland, R.; Duncan, D. K.; Frazer, J.; Lanning, H.;
Misch, A.; Mueller, J.; Soyumer, D.; Vaughan, A. H.; Wilson, O. C.;
Woodard, L. A.
1984BAAS...16R.899B Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Is Mt. Wilson the Best Interferometric Site in the World?
Authors: Nisenson, P.; Noyes, R.; Shao, M.
1984BAAS...16..908N Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Chromospheric emission and rotation of the Hyades lower
main sequence.
Authors: Duncan, D. K.; Baliunas, S. L.; Noyes, R. W.; Vaughan, A. H.;
Frazer, J.; Lanning, H. H.
1984PASP...96..707D Altcode:
The identity of chromospheric Ca II H- and K-line emission has
been monitored for two seasons in a large sample of Hyades F and
G dwarfs. Mean emission levels vary smoothly with spectral type,
suggesting that the rotation rate at a given spectral type varies
relatively little, and that the rotation rate decreases smoothly
as a function of mass. In this case the mechanism which controls
pre-main-sequence angular momentum loss in late-type stars must be
self-regulating to a high degree.
---------------------------------------------------------
Title: Rotation, convection, and magnetic activity in lower
main-sequence stars.
Authors: Noyes, R. W.; Hartmann, L. W.; Baliunas, S. L.; Duncan,
D. K.; Vaughan, A. H.
1984ApJ...279..763N Altcode:
Rotation periods are reported for 14 main-sequence stars, bringing the
total number of such stars with well determined rotation periods to
41. It is found that the mean level of their Ca II H and K emission
(averaged over 15 years) is correlated with rotation period, as
expected. However, there is a further dependence of the emission
on spectral type. When expressed as the ratio of chromospheric flux
to total bolometric flux, the emission is well correlated with the
parameter P(obs)/tau(c), where P(obs) is the observed rotation period
and tau(c)(B - V) is a theoretically-derived convective overturn time,
calculated assuming a mixing length to scale height ratio alpha of about
2. This finding is consonant with general predictions of dynamo theory,
if the relation between chromospheric emission and dynamo-generated
magnetic fields is essentially independent of rotation rate and spectral
type for the stars considered. The dependence of mean chromospheric
emission on rotation and spectral type is essentially the same for
stars above and below the Vaughan-Preston (1980) 'gap', thus casting
doubt on explanations of the gap in terms of a discontinuity in dynamo
characteristics.
---------------------------------------------------------
Title: A study of the dependence of MG II emission on the rotational
periodsof main-sequence stars.
Authors: Hartmann, L.; Baliunas, S. L.; Duncan, D. K.; Noyes, R. W.
1984ApJ...279..778H Altcode:
International Ultraviolet Explorer satellite measurements of the
Mg II chromospheric emission from a sample of late-type dwarfs with
known rotational periods are presented. The ratio of chromospheric
to photospheric luminosity for the late-G and K type stars in this
sample can be fitted within the probable errors by a single function of
rotational period. The chromospheric emission of early-G and F dwarfs
appears to depend upon rotation in a qualitatively different way, which
suggests that the rapid variation of convective zone properties in this
spectral range affects the dissipation of energy in the chromosphere. Mg
II h and k emission correlates fairly well with Ca II emission. However,
the data sample is not large enough at present to show conclusively
that Mg II emission exhibits precisely the same dependence on rotation
and spectral type as the Ca II H and K line fluxes.
---------------------------------------------------------
Title: Chromospheric Activity and Rotation in the Giant Stars in
the Hyades and Praesepe Clusters
Authors: Baliunas, S. L.; Horne, J.; Noyes, R. W.; Duncan, D. K.;
Frazer, J.; Lanning, H.; Misch, A.; Soyumer, T.; Woodard, L.
1984BAAS...16..508B Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Book-Review - the Sun Our Star
Authors: Noyes, R. W.; Maunder, M.
1984JBAA...94...91N Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Book-Review - the Sun Our Star
Authors: Noyes, R. W.; Teske, R. G.
1984ApL....24..104N Altcode:
No abstract at ADS
---------------------------------------------------------
Title: An analysis of the Vaughan-Preston survey of chromospheric
emission.
Authors: Hartmann, L.; Soderblom, D. R.; Noyes, R. W.; Burnham, N.;
Vaughan, A. H.
1984ApJ...276..254H Altcode:
The survey of Ca II H and K emission conducted by Vaughan and Preston
(1980) represents a large homogeneous sample of the chromospheric
activity of late-type main-sequence stars. For stars in the neighborhood
of the sun, this survey is nearly complete, and it can, therefore, be
employed for statistical tests of stellar activity. It is shown that
the observed large-scale distribution of chromospheric emission in the
Vaughan-Preston diagram can be modeled using a smoothly varying decay
of chromospheric activity with age. A description is provided of the
observational data and its calibration in terms of a relative flux
scale. Monte Carlo techniques are employed to simulate the diagram
relating chromospheric emission and color.
---------------------------------------------------------
Title: Stellar magnetic activity, rotation and convection
Authors: Noyes, R. W.
1984AdSpR...4h.151N Altcode: 1984AdSpR...4..151N
The types of information that can be obtained on stellar activity
from synoptic observations are reviewed, and attention is given to
how such observations can be used together with oscillation data
to further the understanding of the physics of magnetic activity in
the sun and stars. Various aspects of stellar magnetic activity and
its measurement are considered, including chromospheric and coronal
emission as an activity indicator, starspots, and stellar rotation
and differential rotation. Stellar activity cycles are discussed with
emphasis on variations over evolutionary time-scales. Finally, the
principal advantages of space observations over ground observations
in the study of stellar magnetic activity are examined.
---------------------------------------------------------
Title: Preface
Authors: Harvey, J. W.; Hudson, H. S.; Noyes, R. W.
1984AdSpR...4d...1H Altcode: 1984AdSpR...4....1H
No abstract at ADS
---------------------------------------------------------
Title: Light Pollution Benefit
Authors: Noyes, R. W.
1984S&T....68..196N Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Solar-space observations and stellar prospects. Proceedings
of the Topical Meeting of the COSPAR Interdisciplinary Scientific
Commission E (Meetings E1, E2, and E6) of the COSPAR Twenty-fifth
Plenary Meeting held in Graz, Austria, 25th June - 7th July 1984.
Authors: Harvey, J. W.; Hudson, H. S.; Noyes, R. W.
1984AdSpR...4h....H Altcode: 1984AdSpR...4..180H; 1984AdSpR...4.....H
Selected topics pertaining to solar-space observations and stellar
prospects are discussed. Papers are presented on the fine-scale
structure of solar magnetic fields, increasing solar chromosphere
line intensities with solar activity, and ulraviolet spectroscopy
of the chromosphere and transition zone at high spatial and temporal
resolution. Consideration is also given to solar coronal studies using
normal-incidence X-ray optics, immediate and long-term prospects for
helioseismology, and a compact Dopplergraph/Magnetograph suitable for
space-based measurements of solar oscillations and magnetic fields.
---------------------------------------------------------
Title: The Relation Between Stellar Activity Rotation Convection
and Implications for the Combined Study of Stellar Activity and
Oscillations from Space
Authors: Noyes, R. W.
1984srps.conf..261N Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Time Series Measurements of Chromospheric Emission and Possible
Evidence for Differential Rotation
Authors: Horne, J. H.; Baliunas, S. L.; Noyes, R. W.; Duncan, D. K.;
Vaughan, A. H.
1984LNP...193..143H Altcode: 1984csss....3..143H
No abstract at ADS
---------------------------------------------------------
Title: The Study of Stellar Global Oscillations by CAII H and
K Variations
Authors: Noyes, R. W.
1984srps.conf..113N Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Stellar rotation in lower main-sequence stars measured from
time variations in H and K emission-line fluxes. II. Detailed analysis
of the 1980 observing season data.
Authors: Baliunas, S. L.; Hartmann, L.; Noyes, R. W.; Vaughan, H.;
Preston, G. W.; Frazer, J.; Lanning, H.; Middelkoop, F.; Mihalas, D.
1983ApJ...275..752B Altcode:
For a sample of 47 lower main-sequence stars, including the Sun,
and eight evolved stars, the relative strength of the Ca II H and
K emission cores has been measured daily over a nearly continuous
interval during 1980 July through October at Mount Wilson. From these
time series measurements of chromospheric emission, rotation rates
have been inferred with quantitative estimates of both the reality and
precision of the rotation periods. We find rotation rates easily for
the main-sequence stars with strong emission or those later than about
spectral type K0. With this technique, rotation rates can be measured
precisely for the first time for equatorial velocities as slow as 1 km
s<SUP>-1</SUP> and independently of the aspect of the rotation axis. In
a limited range of spectral type, a small sample of stars indicates that
chromospheric emission decreases smoothly as a function of rotation
period. No conclusion can be drawn on the question of the reality
of a discontinuity in chromospheric emission as a function of time
(the "Vaughan-Preston" gap for stars in the solar neighborhood). <P
/>In our sample of giant stars, the G2 III star HD 218658 shows a
persistent fluctuation of 4.6 days, a period that is inconsistent with
stellar rotation. The G0 III star HD 6903 is a previously unreported
FK Comae-type star. <P />For a few main-sequence stars, measurements
continued beyond 1980 October suggest the presence of active longitudes
(if not individual active regions) persisting through the observing
season 1981.
---------------------------------------------------------
Title: Identification of the solar emission lines near 12 microns
Authors: Chang, E. S.; Noyes, R. W.
1983ApJ...275L..11C Altcode:
The emission lines in the far-infrared solar spectrum discussed here
were reported by Murcray et al. (1981) and Brault and Noyes (1983). The
two strong emission lines, at 12.32 and 12.22 microns, appear at disk
center and brighten greatly toward the limb. More than 40 additional
limb-brightened lines appear near the limb, and most of these are too
weak to be seen at disk center. These lines are identified here as
transitions between Rydberg states of neutral magnesium and aluminum.
---------------------------------------------------------
Title: Combined ultraviolet studies of astronomical sources
Authors: Dupree, A. K.; Giampapa, M. S.; Huchra, J. P.; Noyes,
R. W.; Hartmann, L. W.; Raymond, J. C.; Blair, W. P.; Bothun, G. D.;
Patterson, J. O.; Baliunas, S. L.
1983sao..reptR....D Altcode:
Ultraviolet spectra of non-radiataive shock waves grain destruction and
elemental abundances in interstellar shocks, carbon abundance in M33
and M31 from supernova remnants, determination of the mass function
in the large Magellanic cloud, UV spectra of white dwarf pulsars,
stellar flares, availability of the double quasar Q 0957 + 56' AB,
spectra of late-F dwarfs and their relation to rotation, dynamics of
hot gas surrounding hybrid stars, high resolution study of epsilon
coronae Austriual, active regions on solar-type dwarfs as a function of
rotation rate and age, coordinated chromospheric synoptic observations
of selected late-type stars, the two-component atmosphere of Lambda
Andromedae, and activity in Hyades giants are discussed.
---------------------------------------------------------
Title: Speckle image reconstruction of solar features
Authors: Stachnik, R. V.; Nisenson, P.; Noyes, R. W.
1983ApJ...271L..37S Altcode:
Speckle image reconstruction procedures have been applied to 5 x 6
arcsec patches of the solar surface. Data were recorded with a CID
(charge-injection device) sensor. This detector has the wide dynamic
range and linearity required to record accurately the extremely
low contrast speckle that occurs for extended objects such as the
sun. Reconstructed images of spot penumbrae and of pores show evidence
for detail at scales as fine as 0.11 arcsec, despite prevailing seeing
conditions of 1 - 2 arcsec. The finest structures appear to be embedded
in penumbral filaments. Coarser sub-arcsecond detail appears in some,
but not all, of the pores studied. The presence of such fine, presumably
magnetically controlled detail suggests that much can be learned from
high-resolution solar surface imaging from space.
---------------------------------------------------------
Title: Solar emission lines near 12 microns
Authors: Brault, J.; Noyes, R.
1983ApJ...269L..61B Altcode:
The newly discovered 12 micron emission lines in the solar spectrum
are found to vary strongly with position on the solar disk. The two
strongest lines strengthen greatly toward the limb and disappear in spot
umbrae. They show pronounced splitting in spot penumbrae and plages,
characteristic of simple Zeeman triplets with g approximately equal
to 1. Their narrow line profiles suggest a chromospheric rather than
coronal origin, but the lines remain unidentified. Forty-one additional
unidentified far-infrared solar emission lines are reported. Potential
uses of the lines for astrophysical investigations are noted.
---------------------------------------------------------
Title: The Sun Our Star
Authors: Noyes, R. W.; Mitton, S.
1983Natur.302..768N Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Magnetically-Sensitive Solar Emission Lines Near 12 Microns
Authors: Brault, J. W.; Noyes, R. W.
1983BAAS...15..702B Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Rotation, Convection, and Solar-Stellar Dynamos
Authors: Noyes, R. W.; Baliunas, S. L.; Duncan, D. K.; Hartmann,
L. W.; Vaughan, A. H.
1983BAAS...15Q.698N Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Solar Speckle Imaging with a CCD Camera
Authors: Nisenson, P.; Stachnik, R.; Noyes, R.; Ebstein, S.
1983BAAS...15..718N Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Book-Review - the Sun Our Star
Authors: Noyes, R. W.; Stickland, D.
1983Obs...103R.270N Altcode:
No abstract at ADS
---------------------------------------------------------
Title: The interpretation of EUV spectra of sunspots
Authors: Doyle, J. G.; Raymond, J. C.; Noyes, R. W.; Kingston, A. E.
1983ASSL..102..325D Altcode: 1983ards.proc..325D; 1983IAUCo..71..325D
EUV observations of a sunspot made on Skylab are discussed. For the
60,000-300,000 K temperature range, a constant electron density of
10 billion/cu cm fits the data, while for the million K plasma the
density decreases by an order of magnitude and a constant pressure
approximation. Temperature diagnostic line ratios show temperatures
lower than the equilibrium temperature and lower than the temperatures
observed in the averaged quiet sun. The observed departure from
ionization equilibrium is consistent with those expected for a
radiatively cooling gas. A model which assumes a constant density
and a constant velocity flow of 7 km/s beginning in ionization
equilibrium at log T = 5.8 matches the overall energetic needs for
the transition region and accounts for the observed shift away from
ionization equilibrium.
---------------------------------------------------------
Title: The relation between rotation and magnetic activity on lower
main sequence stars as derived from chromospheric indicators
Authors: Noyes, R. W.
1983IAUS..102..133N Altcode:
The nature of the relationship between magnetic-field-induced
chromospheric emission of lower-main-sequence stars in the H and K
lines of Ca II and stellar rotation is investigated in a survey of
observational data, which are plotted against each other in a series
of graphs. Parameters such as spectral type, rotation period, H+K flux,
and stellar age are considered, and particular attention is devoted to
the gap in the plot of chromospheric emission versus (B-V) constructed
by Vaughan and Preston (1980).
---------------------------------------------------------
Title: Book-Review - the Sun Our Star
Authors: Noyes, R. W.; Morrison, P.
1983SciAm.248...32N Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Book-Review - the Sun - Our Star
Authors: Noyes, R. W.
1983S&T....66..128N Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Observational Needs for Progress in Solar / Stellar Magnetic
Activity - Overview
Authors: Noyes, R. W.
1983IAUS..102..501N Altcode:
No abstract at ADS
---------------------------------------------------------
Title: The Evolution of Chromospheric Emission Among Solar-Type Stars
Authors: Hartmann, L. W.; Soderblom, D. R.; Noyes, R. W.; Burnham,
N.; Vaughan, A. H.
1982BAAS...14R.918H Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Speckle Image Reconstruction of Solar Features
Authors: Stachnik, R. V.; Nisenson, P.; Noyes, R. W.
1982BAAS...14R.624S Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Combined ultraviolet studies of astronomical sources
Authors: Dupree, A. K.; Giampapa, M. S.; Huchra, J. P.; Noyes, R. W.;
Hartmann, L. W.; Raymond, J. C.
1982sao..reptQ....D Altcode:
Ultraviolet studies of astronomical sources are discussed. Some studies
utilized IVE data. Non-radiative shock at the edge of the Cygnses Loop,
stellar flares, local interestellar medium, hot galaxies, stellar mass
ejection, contact binaries, double quasars, and stellar chromosphere
and coronae are discussed.
---------------------------------------------------------
Title: The growth and decay of magnetic activity in lower main
sequence stars.
Authors: Noyes, R. W.
1982SAOSR.392B..41N Altcode: 1982csss....2...41N
No abstract at ADS
---------------------------------------------------------
Title: The Sun, our star
Authors: Noyes, R. W.
1982sust.book.....N Altcode: 1982QB521.N68......
Observational data, analytical models, and instrumentation used to
study the sun and its evolution are detailed, and attention is given
to techniques for converting solar energy to useful power on earth. The
star ignited when the mutual gravitational attractions of dust and vapor
in a primordial cloud in the Galaxy caused an in-rush of accelerating
particles which eventually became dense enough to ignite. The heat grew
until inward rushing matter was balanced by outward moving radiative
forces. The planets formed from similar debris, and solar radiation is
suggested to have triggered the chemical reactions giving rise to life
on earth. Visual, spectroscopic, coronagraphic, and UV observations
of the sun from the ground and from spacecraft, particularly Skylab,
are described, together with features of the solar surface, magnetic
field, sunspots, and coronal loops. Models for the processes that
occur in the solar interior are explored, as are the causes of solar
flares. Attention is given to solar cells, heliostat arrays, wind
turbines, and water turbines as means to convert, either directly or
indirectly, the earth-bound solar energy to electrical and thermal
power. Finally, the life cycle of the sun, about 9 billion yr in
duration, is summarized, noting the current status of midlife.
---------------------------------------------------------
Title: Book-Review - the Sun Our Star
Authors: Noyes, R. W.
1982SciN..122..378N Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Active Regions on Solar-Type Dwarfs
Authors: Noyes, Robert W.
1982iue..prop.1151N Altcode:
We propose to obtain ultraviolet spectra of late-type dwarfs with known
rotation rates to Investigate the emission level of chromospheres
and coronae as a function of rotation and age, and to determine the
physical structure of active regions or other Inhomogeneities within
the atmospheres. The investigation will be carried out jointly and
In a coordinated manner with the Mt. Wilson HK photometer program,
which will provide continuous monitoring of the program stars before,
during, and after the times of IUE observation.
---------------------------------------------------------
Title: A matter of degrees
Authors: Noyes, R. W.
1982rupp.book...85N Altcode:
The development and interaction between theory and predictions
of features, composition, and behavior of the solar corona are
examined. Spectrography has revealed that the corona is composed of
the same elements present in the sun, and is actually an atmosphere
and held aloft by intense heating, which causes expansion. Mechanisms
which heat the coronal material are discussed, and the advent of MHD
theory in the 1940s furnished material for present day observations
in terms of the directions of investigations. It is still uncertain
why the solar wind emerges from coronal holes, which are magnetically
open while the remaining coronal is magnetically bottled and composed
of 3,000,000 C iron plasma.
---------------------------------------------------------
Title: Stellar rotation in lower main-sequence stars measured from
time variations in H and K emission-line fluxes. I. Initial results.
Authors: Vaughan, A. H.; Baliunas, S. L.; Middelkoop, F.; Hartmann,
L. W.; Mihalas, D.; Noyes, R. W.; Preston, G. W.
1981ApJ...250..276V Altcode:
Fluxes at 1 Å bands at the centers of the H and K lines in 46 lower
main sequence field stars, and in eight selected subgiants and giant
stars, have been measured at nightly intervals in the course of a
nearly continuous 14-week observing run. In 19 stars we have found
clear evidence of rotational modulation, from which values of the
rotational periods can be assigned by inspection. In nine others,
periods have been found by an autocorrelation analysis of the flux
records. The periods obtained imply rotation velocities that are in
good accord with spectroscopically determined values of V sin i in
the literature for 13 of the stars we have observed. <P />Much of
the short term scatter in H-K flux observed by Wilson appears to be
caused by rotational modulation, although variations on other time
scales are also present. <P />As many as 80% of the chromospherically
active (i.e., young) stars display prominent rotational modulation,
and in some cases the phase of the modulation remained unchanged for
the entire observing period, suggesting that markedly asymmetric and
long-lived distributions of active regions are common in such stars. <P
/>At a given (B - V) < 1.0, the strength of H-K emission is shown
to vary as a function of rate of rotation, suggesting that rotation,
rather than initial conditions or age per se, is the chief parameter
influencing chromospheric output. <P />From data on stellar activity
cycles available at present, it is suggested that periodic cycles
resembling the Sun's are almost exclusively found in stars with
rotation periods in excess of about 20 days; and, except for this
threshold effect, the cycle periods are uncorrelated with rotation rate.
---------------------------------------------------------
Title: Analysis of Extreme Ultraviolet Spectroheliograms of Solar
Prominences
Authors: Kanno, M.; Withbroe, G. L.; Noyes, R. W.
1981SoPh...69..313K Altcode:
The optical depth at the head of the Lyman continuum, τ<SUB>H</SUB>,
is determined at a number of positions in three hedgerow prominences
using spectroheliograms (5″ × 5″ resolution) of C IIIλ 977,
LC λ896, and O IV λ554 observed with the Harvard experiment
on Skylab. At heights greater than 10″ above the limb the
maximum value of τ<SUB>H</SUB> is 30 to 50, which occurs at the
central part of the prominences. For one of the prominences the
determination of τ<SUB>H</SUB> is found to be consistent with data from
spectroheliograms of Mg X λ625. The degree of ionization of hydrogen is
estimated from the intensity of LC λ896 at τ<SUB>H</SUB> ≫ 1. In the
central part of a model prominence N<SUB>P</SUB>/N<SUB>HI</SUB>≤1.9
for a reasonable range of the electron densities, where N<SUB>P</SUB>
and N<SUB>HI</SUB> are the proton density and the neutral hydrogen
density, respectively.
---------------------------------------------------------
Title: Particle acceleration in solar flares
Authors: Noyes, R. W.
1981sfmh.book..429N Altcode: 1981sfmh.book..429H
Energetic particles at 1 AU are considered along with hard X-ray
emission in flares, implications of X-ray observations, and microwave
impulsive bursts. Attention is also given to gamma-ray emission,
elemental and isotopic abundances of solar cosmic rays, fast particle
impact on the chromosphere and photosphere from EUV and H-alpha bursts,
the directed flow of fast particles to the chromosphere or hot fireball,
the first-phase acceleration process, runaways through turbulence,
current-driven microinstabilities, the production of a Langmuir
wave spectrum suitable for acceleration, strong-turbulence effects,
proposed microturbulent acceleration models, double layers, tearing
modes and fast particles, second-phase acceleration, the compatibility
of second-phase Fermi acceleration with observational data, Fermi
mechanism and resonant MHD processes, first-order Fermi mechanism near
shocks, nuclei preheating, and acceleration in and near shocks fronts.
---------------------------------------------------------
Title: The sun as a star: solar phenomena and stellar applications.
Authors: Noyes, R. W.
1981ASIC...68....1N Altcode: 1981spss.conf....1N
The properties of the sun as a star are discussed in light of the
possibilities offered by studies of the sun for the understanding of
other stars, and the potential implications of studies of solar-type
stars with different fundamental properties for the understanding of
solar physics. Particular attention is given to the relation between
rotation rates, activities, magnetic fields and ages in the sun and
other main-sequence stars, which is explained in terms of processes in
stellar convection zones, the phenomenology of the solar activity cycle
and its relation to stellar cycles, and to closed and open magnetic
structures in the solar corona and the possible mainfestations of such
structures on other stars. Areas of stellar and solar physics which
are likely to be clarified in the future by further solar observations,
related stellar observations and theoretical studies are indicated.
---------------------------------------------------------
Title: Study of Active Regions on Solar-Type Dwarfs as a Function
of Rotation and Age
Authors: Noyes, Robert
1981iue..prop..804N Altcode:
We propose to obtain ultraviolet spectra of late-type dwarfs with
known rotation rates to investigate the presence and emission level
of chromospheres and coronae as a function of rotation and age,
and to determine the physical structure of active regions or other
inhomogeniety within the atmospheres.
---------------------------------------------------------
Title: A study of coronal magnetic structures and solar output
Authors: Noyes, Robert W.; Levine, R. H.
1981scms.book.....N Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Semiempirical models of chromospheric flare regions
Authors: Machado, M. E.; Avrett, E. H.; Vernazza, J. E.; Noyes, R. W.
1980ApJ...242..336M Altcode:
Homogeneous plane-parallel semiempirical flare model atmospheres
which reproduce observations in lines and continua of H I, Si I,
C I, Ca II, and Mg II have a thin transition zone at the top of the
enhanced chromosphere, indicating a significant amount of heating from
the zone to the temperature minimum level. The minimum temperature is
located deeper and is higher than in the quiet-sun and active-region
models. The results do not agree with the particle-heated theoretical
models, and it is suggested that the models of Brown (1973) and Henoux
and Nakagawa (1977, 1978) do not include an essential term for heat
conduction in their energy balance equations. It is concluded that
substantial Ly-alpha radiative heating occurs in the upper chromosphere
resulting from the conductive energy flux in the transition zone where
the Ly-alpha line cools the gas.
---------------------------------------------------------
Title: Measurements of coronal kinetic temperatures from 1.5 to 3
solar radii
Authors: Kohl, J. L.; Weiser, H.; Withbroe, G. L.; Noyes, R. W.;
Parkinson, W. H.; Reeves, E. M.; Munro, R. H.; MacQueen, R. M.
1980ApJ...241L.117K Altcode:
A rocket-borne Lyman-alpha coronagraph has been used to make the first
measurements of the spectral line profile of resonantly scattered
hydrogen Lyman-alpha coronal radiation between 1.5 and 3 solar
radii. These data provide, for the first time, direct measurements of
coronal temperatures above 1.5 solar radii. Data were obtained in a
coronal hole, quiet region, and streamer. The widths of the profiles
from the quiet region decrease with height and correspond to a steady
decrease in hydrogen kinetic temperature, with increasing radius, from
about 2.5 million K at r = 2 solar radii to about 1 million K at r =
9 solar radii. In the coronal hole the measured line widths indicate
a kinetic temperature of 1.8 million K at r = 2.5 solar radii.
---------------------------------------------------------
Title: Mission Options for SCADM in the 1980's
Authors: Noyes, R. W.
1980NASCP2098...31N Altcode: 1980sscs.nasa...31N
Recent insights into the workings of the solar system are reviewed as
factors to be considered when formulating key questions to be answered
during a large scale program to study the solar cycle. The main
objectives of the Solar Cycle and Dynamics Mission are to determine
the causes (physical origins and mechanisms) of the solar cycle and
the effects of these mechanisms on the heliosphere, the vast region
that includes the corona, interplanetary medium, and the terrestrial
environment. The mission should be able to obtain synoptic data on
solar variability associated with the cycle, and over at least a
fraction of a single 11-year cycle.
---------------------------------------------------------
Title: The Sun as a Star
Authors: Noyes, R. W.
1980SAOSR.389....3N Altcode: 1980csss....1....3N
No abstract at ADS
---------------------------------------------------------
Title: Optical observations of SS 433.
Authors: Noyes, R.; Liller, W.; Davis, M.; Baliunas, S.; Sternberg,
A.; Tokarz, S.
1979BAAS...11..732N Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Optical Observations of SS 433
Authors: Liller, W.; Noyes, R.; Davis, M.; Baliunas, S.; Sternberg,
A.; Tokarz, S.
1979BAAS...11..732L Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Optical Observations of SS 433.
Authors: Noyes, R.; Liller, W.; Davis, M.; Baliunas, S.; Sternberg,
A.; Tokarz, S.
1979BAAS...11..786N Altcode:
No abstract at ADS
---------------------------------------------------------
Title: SS 433
Authors: Baliunas, S.; Noyes, R.; Liller, W.; Tokarz, S.
1979IAUC.3410....1B Altcode:
S. Baliunas, R. Noyes, W. Liller and S. Tokarz, Harvard-Smithsonian
Center for Astrophysics, report that the central intensity of H-alpha
relative to the continuum in SS 433 showed factor-of-two increases
on Apr. 29 and June 20, each lasting about two days. Observations
over five nights during these times, plus additional observations on
14 other nights throughout the interval Apr. 28 to June 24, showed
all the data to be commensurate with the 13.1-day period reported by
Crampton et al. (IAUC 3388). Comparison with other photometric data
indicates that the ratio increases represent increases of absolute
H-alpha-emission-line intensity. The data were obtained with the
digital spectrograph at the Mount Hopkins 1.5-m telescope.
---------------------------------------------------------
Title: Lyman-α and White Light Observations of the Outer Solar
Corona.
Authors: Munro, R. H.; Kohl, J. L.; MacQueen, R. M.; Noyes, R. W.;
Parkinson, W. H.; Weiser, H.; Withbroe, G. L.
1979BAAS...11..398M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: The Balmer 9 and Balmer 11 lines of He II in the sun.
Authors: Raymond, J. C.; Noyes, R. W.; Stopa, M. P.
1979SoPh...61..271R Altcode:
We identify the Balmer 9 and 11 lines of He II at 959 Å and 942 Å
in solar spectra. These lines are produced mainly by recombination
following photoionization of He II by coronal XUV radiation. From
analysis of the line intensities, we confirm the theoretical model
of Avrett et al. (1976), who found that an appreciable amount of
He<SUP>++</SUP> is present at temperatures of 1-2 × 10<SUP>4</SUP> K
and that the anomalously strong He II λ304 line is produced primarily
by collisional excitation. We also confirm the suggestion of Kohl (1977)
that the photoionization-recombination process is more important in
active regions than in the quiet Sun, and we find that the λ304 line
is produced largely by recombination in solar flares.
---------------------------------------------------------
Title: A broad look at solar physics adapted from the solar physics
study of August 1975
Authors: Parker, E.; Timothy, A.; Beckers, J.; Hundhausen, A.; Kundu,
M. R.; Leith, C. E.; Lin, R.; Linsky, J.; MacDonald, F. B.; Noyes, R.
1979sswp.book....3P Altcode: 1979sswp.book....3B
The current status of our knowledge of the basic mechanisms involved
in fundamental solar phenomena is reviewed. These include mechanisms
responsible for heating the corona, the generation of the solar
wind, the particle acceleration in flares, and the dissipation of
magnetic energy in field reversal regions, known as current sheets. The
discussion covers solar flares and high-energy phenomena, solar active
regions; solar interior, convection, and activity; the structure and
energetics of the quiet solar atmosphere; the structure of the corona;
the solar composition; and solar terrestrial interactions. It also
covers a program of solar research, including the special observational
requirements for spectral and angular resolution, sensitivity, time
resolution, and duration of the techniques employed.
---------------------------------------------------------
Title: Lyman continuum observations of solar flares.
Authors: Machado, M. E.; Noyes, R. W.
1978SoPh...59..129M Altcode:
A study is made of Lyman continuum observations of solar flares, using
data obtained by the Harvard College Observatory EUV spectroheliometer
on the Apollo Telescope Mount. We find that there are two main types of
flare regions: an overall `mean' flare coincident with the Hα flare
region, and transient Lyman continuum kernels which can be identified
with the Hα and X-ray kernels observed by other authors. It is
found that the ground level hydrogen population in flares is closer
to LTE than in the quiet Sun and active regions, and that the level
of Lyman continuum formation is lowered in the atmosphere from a
mass column density m ≈ 5/sx 10<SUP>−6</SUP> g cm<SUP>−2</SUP>
in the quiet Sun to m ≈ 3/sx 10<SUP>−4</SUP> g cm<SUP>−2</SUP>
in the mean flare, and to m ∼ 10<SUP>−3</SUP>g cm<SUP>−2</SUP>
in kernels. From these results we derive the amount of chromospheric
material `evaporated' into the high temperature region, which is found
to be ∼- 10<SUP>15</SUP>g, in agreement with observations of X-ray
emission measures. A comparison is made between kernel observations
and the theoretical predictions made by model heating calculations,
available in the literature; significant discrepancies are found
between observation and current particle-heating models.
---------------------------------------------------------
Title: The characteristics of impulsive solar EUV bursts
Authors: Gordon Emslie, A.; Noyes, Robert W.
1978SoPh...57..373G Altcode:
We examine a number of high time resolution intensity-time profiles of
EUV impulsive bursts as observed by the Harvard College Observatory
EUV Spectroheliometer carried aboard the Skylab Apollo Telescope
Mount. These bursts are found to be synchronous (to within the
instrumental time resolution of 5.5 s) in all wavelengths observed,
corresponding to emissions from temperatures ranging from upper
chromospheric to coronal. The distribution with temperature of a
suitably defined emission measure parameter is also examined as a
function of time throughout the bursts and a marked similarity in
the shape of this distribution, both between different events and
throughout the time history of any particular event, is noted. The
significance of these observations for physical processes associated
with EUV bursts is briefly discussed.
---------------------------------------------------------
Title: The characteristics of impulsive solar EUV bursts.
Authors: Emslie, A. G.; Noyes, R. W.
1978SoPh...57..373E Altcode:
This paper examines a number of high-time-resolution
intensity-time profiles of EUV impulsive bursts as observed
by the EUV spectroheliometer carried aboard the Skylab Apollo
Telescope Mount. These bursts are found to be synchronous (to
within the instrumental time resolution of 5.5 s) in all wavelengths
observed, corresponding to emissions from temperatures ranging from
upper-chromospheric to coronal. The distribution with temperature of
a suitably defined emission-measure parameter is also examined as a
function of time throughout the bursts, and a marked similarity in
the shape of this distribution, both between different events and
throughout the time history of any particular event, is noted. The
significance of these observations for physical processes associated
with EUV bursts is briefly discussed.
---------------------------------------------------------
Title: Secular Changes in Solar Rotation, 1888-1964.
Authors: Eddy, J. A.; Noyes, R. W.; Wolbach, J. G.; Boornazian, A. A.
1978BAAS...10..400E Altcode:
No abstract at ADS
---------------------------------------------------------
Title: The Faint Object Spectrograph for Space Telescope
Authors: Noyes, R. W.
1978nisa.symp...71N Altcode: 1978nisa.conf...71N
The design concept and scientific goals for the space-telescope
faint-object spectrograph (FOS) are reviewed. The primary operating
mode of the FOS can obtain spectra of faint objects with a resolution
of the order of 1000 through the UV and well into the visual; stigmatic
imagery is maintained to 0.1 arcsec. A spectral resolution as low as
100 is contemplated, allowing the observation of objects as faint as a
visual magnitude of about 25. Operation of the FOS is described, and
the detection system is discussed. Scientific opportunities listed
for the FOS include UV observations of quasars, active and normal
galaxies, stars, the interstellar medium, and solar-system objects,
particularly the outer planets, their satellites, and comets.
---------------------------------------------------------
Title: Mass and energy flow in the solar chromosphere and corona.
Authors: Withbroe, G. L.; Noyes, R. W.
1977ARA&A..15..363W Altcode:
The work reviews some investigations into the mass and energy
flow in the solar chromosphere and corona; the objective of these
investigations is the development of a physical model that will not
only account for the physical conditions in the outer atmosphere of
the sun, but can also be applied to the study of the outer atmospheres
of other stars. Particular attention is given to mass and energy flow
in regions with weak and strong magnetic fields, to observational
evidence for wave heating and systematic mass flows, and to heating
mechanisms. Consideration is given throughout to mechanisms of energy
input and energy loss.
---------------------------------------------------------
Title: Out-of-Ecliptic Studies of Coronal Holes and Their Relation
to the Solar Wind
Authors: Noyes, R. W.
1976ssim.conf...48N Altcode: 1975ssim.conf...48N; 1976sipm.symp...48N
The advantages of observing coronal holes of the sun above the solar
ecliptic plane by a solar probe are discussed. Also discussed are the
size of coronal holes, their temperature, and magnetic fields associated
with the holes. The role of coronal holes in contributing to the solar
wind is examined. Data and observations on coronal holes from Skylab
and OSO are treated. It is concluded that an out-of-the-ecliptic solar
probe mission would greatly add to the understanding of coronal holes
(at high latitudes) thus adding a new perspective to the observation
of these phenomena. (Photographs of the sun taken by Skylab are shown).
---------------------------------------------------------
Title: Extreme Ultraviolet Observations of Solar Flares
Authors: Wood, A. T., Jr.; Noyes, R. W.; Reeves, E. M.
1976saop.book..117W Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Extreme-ultraviolet transients observed at the solar pole.
Authors: Withbroe, G. L.; Jaffe, D. T.; Foukal, P. V.; Huber, M. C. E.;
Noyes, R. W.; Reeves, E. M.; Schmahl, E. J.; Timothy, J. G.; Vernazza,
J. E.
1976ApJ...203..528W Altcode:
Extreme-ultraviolet (EUV) observations of two polar transient features
('macrospicules') are described. These features appear to be caused
by jets of chromospheric material that shoot upward to a height of
35,000 km above the limb and then fall back into the chromosphere,
reaching terminal velocities of about 140 km/s. On the basis of a
model developed from the EUV measurements, it is found that the energy
required to produce each event is about 3 by 10 to the 26th power ergs,
about two orders of magnitude more than that required to produce an
ordinary spicule. This indicates that macrospicules may be an important
factor in the energy balance of the chromosphere and corona.
---------------------------------------------------------
Title: Initial results from the EUV spectroheliometer on ATM
Authors: Reeves, E. M.; Timothy, J. G.; Foukal, P. V.; Huber, M. C. E.;
Noyes, R. W.; Vernazza, J. E.; Withbroe, G. L.; Schmahl, E. J.
1976skls.conf...73R Altcode:
The Harvard College Observatory photoelectric spectroheliometer on
the Apollo Telescope Mount operated correctly in orbit from May 29,
1973 to February 7, 1974. During this period, many thousands of
spatial and spectral scans at extreme ultraviolet wavelengths were
recorded during observations of a variety of solar features. The
construction and modes of operation of the instrument are outlined,
and the principal scientific results from a preliminary analysis of
the data are described.
---------------------------------------------------------
Title: New development in solar research.
Authors: Noyes, R. W.
1976fras.conf...41N Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Extreme ultraviolet observations of solar flares.
Authors: Wood, A. T.; Noyes, R. W.; Reeves, E. M.
1976npsa.conf...87W Altcode:
No abstract at ADS
---------------------------------------------------------
Title: A high-resolution map of the W3 region at far-infrared
wavelengths.
Authors: Fazio, G. G.; Kleinmann, D. E.; Noyes, R. W.; Wright, E. L.;
Zeilik, M., II; Low, F. J.
1975ApJ...199L.177F Altcode:
The area in the vicinity of the H II region W3 is mapped at an effective
wavelength of 69 microns with high angular resolution (1 min) using
the 102-cm balloon-borne telescope. The main continuum source, W3,
shows a partially resolved complex structure with a FWHM size of 1.8
min. The radio sources W3(OH) and G133.8 + 1.4 are also observed as
well as three faint sources not associated with known radio emission.
---------------------------------------------------------
Title: Time variations in extreme-ultraviolet emission lines and
the problem of coronal heating.
Authors: Vernazza, J. E.; Foukal, P. V.; Huber, M. C. E.; Noyes,
R. W.; Reeves, E. M.; Schmahl, E. J.; Timothy, J. G.; Withbroe, G. L.
1975ApJ...199L.123V Altcode:
We have analyzed the time structure of the intensity of solar
chromospheric and coronal extreme-ultraviolet lines, obtained by
the Harvard College Observatory spectrometer aboard Skylab. We find
changes in the intensity of up to 50 percent in times as short as
1 minute, but not periodic oscillations. Some evidence is found for
the presence of shock waves in the chromosphere and the transition
region. It is suggested that the solar chromosphere and corona are
heated by nonperiodic waves.
---------------------------------------------------------
Title: Book reviews
Authors: van de Stadt, Herman; Rawer, Karl; Schadee, A.; Noyes, R. W.;
Bleeker, J. A. M.; Wittenberg, H.; de Graaff, W.; Akasofu, S. -I.;
Hooykaas, R.; Bappu, M. K. V.; Atanasijević, I.; Icke, Vincent;
van der Valk, F.; Kresàk, L.; Müller, Edith A.
1975SSRv...17..159V Altcode:
No abstract at ADS
---------------------------------------------------------
Title: EUV Observations of the Active Sun from the Harvard Experiment
on ATM
Authors: Noyes, R. W.; Foukal, P. V.; Huber, M. C. E.; Reeves, E. M.;
Schmahl, E. J.; Timothy, J. G.; Vernazza, J. E.; Withbroe, G. L.
1975IAUS...68....3N Altcode:
Some extreme UV observations of solar active regions made with a
scanning spectroheliometer are described. Spectroheliograms constructed
from digital data using a computer-driven cathode-ray tube display show
clearly how the appearance of an active region changes as a function
of temperature. Flare studies indicate that the impulsive rise in
EUV emission occurs essentially simultaneously at all levels from the
transition zone to the corona. Observations of sunspots reveal a very
intense emission in transition zone lines. A matrix of Mg x rasters
covering the entire sun reveals several hundred bright points having
dimensions of 30 arc seconds or less. Other observations include
coronal holes and prominences.
---------------------------------------------------------
Title: Extreme-Ultraviolet Observations of Coronal Holes: Initial
Results from SKYLAB
Authors: Huber, M. C. E.; Foukal, P. V.; Noyes, R. W.; Reeves, E. M.;
Schmahl, E. J.; Timothy, J. G.; Vernazza, J. E.; Withbroe, G. L.
1974ApJ...194L.115H Altcode:
We compare the appearance and physical parameters of the solar
chromosphere, transition zone, and corona in areas of coronal holes
with that of quiet areas outside the hole. Measurements of the height
of emission of various ions in a coronal hole appearing at the polar
limb give a quantitative indication of the increased thickness of the
transition zone underlying coronal holes.
---------------------------------------------------------
Title: Observed Heights of EUV Lines Formed in the Transition Zone
and Corona. II: NRL Rocket Observations
Authors: Simon, G. W.; Seagraves, P. H.; Tousey, R.; Purcell, J. D.;
Noyes, R. W.
1974SoPh...39..121S Altcode:
Using high resolution (3-5″) rocket spectroheliograms obtained by
NRL, we have analyzed hundreds of small, bright, quiet Sun features
to determine the heights of formation of five transition zone lines:
He I 584, He II 304, O V 630, Ne VII 465, and Mg IX 368. The results
are in excellent agreement with theoretical model calculations.
---------------------------------------------------------
Title: Extreme-Ultraviolet Observations of Sunspots with the Harvard
Spectrometer on the Apollo Telescope Mount
Authors: Foukal, P. V.; Noyes, R. W.; Reeves, E. M.; Schmahl, E. J.;
Timothy, J. G.; Vernazza, J. E.; Wilhbroe, G. L.; Huber, M. C. E.
1974ApJ...193L.143F Altcode:
EUV spectroheliograms show that the areas directly above sunspot
umbrae are the brightest features in an active region by an order of
magnitude in the chromospherecorona transition region (1 K < T <
108 K.) Rarios of density-sensitive lines in the transition region
show a significant decrease in gas density over the umbra relative
to surrounding plage. We deduce that the temperature gradient in the
transition region over the spot is decreased by an order of magnitude
or more, relative to the plage. S#ject headings: chromosphere, solar -
corona, solar - spectroheliograms - sunspots
---------------------------------------------------------
Title: A balloon-borne 1 meter telescope for far-infrared astronomy
Authors: Fazio, G. G.; Kleinmann, D. E.; Noyes, R. W.; Wright, E. L.;
Low, F. J.
1974tsbb.nasa...38F Altcode:
The flight of a balloon-borne one-meter telescope for infrared astronomy
in the wavelength interval of 40 to 240 microns is discussed. The
gyro-stabilized telescope mapped the intensity of the far infrared
radiation from NGC 7538, Mars, the Orion Nebula, and W3 with a
resolution of one minute and from selected regions of these sources
with a resolution of 30 seconds. The infrared detection is described
and its capabilities are analyzed. The instrumentation, orientation
system, and modes of observation of the telescope are defined.
---------------------------------------------------------
Title: High-resolution maps of H II regions at far-infrared
wavelengths.
Authors: Fazio, G. G.; Kleinmann, D. E.; Noyes, R. W.; Wright, E. L.;
Zeilik, M., II; Low, F. J.
1974hrgc.conf...79F Altcode: 1974hrgc.rept...79F
The first successful flight of a balloon-borne 1-m telescope for
far-infrared (40 micron) astronomy occurred on 4 February 1974 (UT),
from Palestine, Texas. During 6 h at float altitude, the gyrostabilized
telescope mapped the intensity of far-infrared radiation from the H
2 regions Ori A and W3 with a resolution of 1 prime. Partial maps of
these regions were made with a resolution of 0.5 prime. These sources
were resolved into several components, some of which were previously
unknown. Observations of Mars were used for calibration.
---------------------------------------------------------
Title: Initial results from the EUV spectroheliometer on ATM.
Authors: Reeves, E. M.; Timothy, J. G.; Foukal, P. V.; Huber, M. C. E.;
Noyes, R. W.; Schmahl, E. J.; Vernazza, J. E.; Withbroe, G. L.
1974aiaa.conf.....R Altcode:
The Harvard College Observatory photoelectric spectroheliometer on
the Apollo Telescope Mount operated correctly in orbit from May 29,
1973 to Feb. 7, 1974. During this period many thousands of spatial and
spectral scans at extreme ultraviolet wavelengths were recorded during
observations of a variety of solar features. The construction and modes
of operation of the instrument are outlined and the principal scientific
results from a preliminary analysis of the data are described.
---------------------------------------------------------
Title: The Extreme Ultraviolet Spectrum of Sunspots.
Authors: Noyes, R. W.
1974BAAS....6..428N Altcode:
No abstract at ADS
---------------------------------------------------------
Title: A High-Resolution Map of the Orion Nebula Region at
Far-Infrared Wave-Lengths
Authors: Fazio, G. G.; Kleinmann, D. E.; Noyes, R. W.; Wright, E. L.;
Zeilik, M., II; Low, F. J.
1974ApJ...192L..23F Altcode:
A high angnlar resolution (1') map of Ori A (M42) at an effective
wavelength of 69 shows two components: a small (< 1') intense source
at the position of the Kleinmann-Low infrared nebula and an extended
emission similar to the 11-cm aperture-synthesis map of Webster and
Altenhoff. Nearby sources also detected include the nebula M43 and the
molecular cloud OMC-2. Subject headings: infrared sources - Orion Nebula
---------------------------------------------------------
Title: High Resolution Maps of the Orion Nebula Region and W3 at
Far Infrared Wavelengths.
Authors: Fazio, G. G.; Kleinman, D. E.; Noyes, R. W.; Wright, E. L.;
Zeilik, M., II; Low, F. J.
1974BAAS....6..329F Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Extreme Ultraviolet Solar Spectra from Skylab-Apollo Telescope
Mount.
Authors: Dupree, A. K.; Foukal, P. V.; Huber, M. C. E.; Noyes, R. W.;
Reeves, E. M.; Schmahl, E. J.; Timothy, J. G.; Vernazza, J. E.;
Withbroe, G. L.
1974BAAS....6..349D Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Extreme Ultraviolet Solar Observations from the Harvard
ATM Experiment
Authors: Withbroe, G. L.; Foukal, P. K.; Huber, M. C. E.; Noyes,
R. W.; Reeves, E. M.; Schmahl, E. J.; Timothy, J. G.; Vernazza, J. E.
1974BAAS....6V.297W Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Rocket Spectroheliogram Observations of the Heights of
Formation and Sizes of Bright Features in the Transition Zone
Authors: Simon, George W.; Seagraves, Paul H.; Tousey, R.; Noyes,
Robert W.
1974BAAS....6U.294S Altcode:
No abstract at ADS
---------------------------------------------------------
Title: ATM Observations of the Time Dependent Intensity Fluctuations
in the Extreme Ultraviolet
Authors: Vernazza, J. E.; Foukal, P. K.; Huber, M. C. E.; Noyes,
R. W.; Reeves, E. M.; Schmahl, E. J.; Timothy, J. G.; Withbroe, G. L.
1974BAAS....6R.296V Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Solar Prominences in the Extreme Ultraviolet as Observed from
the Apollo Telescope Mount
Authors: Schmahl, E. J.; Foukal, P. V.; Huber, M. C. E.; Noyes, R. W.;
Reeves, E. M.; Timothy, J. G.; Vernazza, J. E.; Withbroe, G. L.
1974SoPh...39..337S Altcode:
Observations of quiescent solar prominences with the Harvard College
Observatory spectrometer abroad Skylab show that prominence material is
optically thick in the Lyman alpha line and the Lyman continuum. The
color temperature of the Lyman continuum has a mean of 6600 K and
an upward gradient toward the top of the prominence. The departure
coefficient of the ground state of hydrogen is found to be of the
order of unity as expected from theory.
---------------------------------------------------------
Title: Observations of the Chromospheric Network: Initial Results
from the Apollo Telescope Mount
Authors: Reeves, E. M.; Foukal, P. V.; Huber, M. C. E.; Noyes, R. W.;
Schmahl, E. J.; Timothy, J. G.; Vernazza, J. E.; Withbroe, G. L.
1974ApJ...188L..27R Altcode:
A preliminary analysis of early data taken by the HCO spectrometer on
Skylab shows that the solar chromospheric network can be clearly seen
with varying contrast in the extreme-ultraviolet emission characteristic
of temperatures between 10 v K (the Lyman continuum) and 3 X 10 K (0
vi). In the emission of Mg x, a coronal line formed at about 1.5 X 108
K, the network is generally unrecognizable. This is interpreted as being
due to a spreading of the magnetic field lines of the network boundary
in the height interval corresponding to the temperature difference
between 3 X 10 and 1.5 X 108 K. We note that in certain anomalous cases,
bright points of the network are seen to extend with high contrast and
essentially unchanged in their cross-section through the full range of
temperatures characteristic of the chromosphere, transition region,
and low corona. Subject headings: granules and supergranules, solar-
spectra, ultraviolet
---------------------------------------------------------
Title: Solar EUV Photoelectric Observations from SKYLAB
Authors: Reeves, E. M.; Foukal, P. V.; Huber, M. C. E.; Noyes, R. W.;
Schmahl, E. J.; Timothy, J. G.; Vernazza, J. E.; Withbroe, G. L.
1974IAUS...57..497R Altcode:
No abstract at ADS
---------------------------------------------------------
Title: A Study of the Active Region McMath 12417 with the Harvard
ATM EUV Spectrometer.
Authors: Foukal, P. V.; Huber, M. C. E.; Noyes, R. W.; Reeves, E. M.;
Schmahl, E. J.; Timothy, J. G.; Vernazza, J. E.; Withbroe, G. L.
1973BAAS....5..432F Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Preliminary Solar Extreme Ultraviolet Observations from the
ATM with the Harvard Instrument.
Authors: Reeves, E. M.; Foukal, P. K.; Huber, M. C. E.; Noyes, R. W.;
Schmahl, E. J.; Timothy, J. G.; Vernazza, J. E.; Withbroe, G. L.
1973BAAS....5..419R Altcode:
No abstract at ADS
---------------------------------------------------------
Title: ATM Observations of Solar Flares in the Extreme Ultraviolet.
Authors: Noyes, R. W.; Foukal, P. V.; Huber, M. C. E.; Reeves, E. M.;
Schmahl, E. J.; Timothy, J. G.; Vernazza, J. E.; Withbroe, G. L.
1973BAAS....5..433N Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Solar Prominences-in the EUV as Observed from ATM.
Authors: Schmahl, E. J.; Foukal, P. V.; Huber, M. C. E.; Noyes, R. W.;
Reeves, E. M.; Timothy, J. G.; Vernazza, J. E.; Withbroe, G. L.
1973BAAS....5..432S Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Observations of a Coronal Hole Boundary in the Extreme
Ultraviolet.
Authors: Huber, M. C. E.; Foukal, P. V.; Noyes, R. W.; Reeves, E. M.;
Schmahl, E. J.; Timothy, J. G.; Vernazza, J. E.; Withbroe, G. L.
1973BAAS....5..446H Altcode:
No abstract at ADS
---------------------------------------------------------
Title: The Harvard Experiment on OSO-6: Instrumentation, Calibration,
Operation, and Description of Observations
Authors: Huber, Martin C. E.; Dupree, A. K.; Goldberg, Leo; Noyes,
R. W.; Parkinson, W. H.; Reeves, E. M.; Withbroe, George L.
1973ApJ...183..291H Altcode:
The Harvard experiment carried by OS 0-6 was an extreme-ultraviolet
(EUV) spectrometerspectroheliometer with wavelength range 285-1385 A,
spatial and spectral bandwidth 35 x 35 (arc sec)2 and 3 A, respectively;
the instrumeflt acquired data that have been deposited with the National
Space Science Data Center and World Data Center A at the Goddard Space
Flight Center in Greenbelt, Maryland, and are now available in their
entirety to the scientific community. This paper describes aspects
of the experiment that are relevant to potential users of the data:
instrument configuration and parameters, laboratory and inflight
calibrations, as well as operational capabilities and procedures. We
also report the observations obtained and, where relevant, list
the nature, number, and dates of observations. Subject headings:
atmospheres, solar - instruments - solar activity - spectra, solar -
spectra, ultraviolet
---------------------------------------------------------
Title: The Extreme-Ultraviolet Spectrum of a Solar Active Region
Authors: Dupree, A. K.; Huher, M. C. E.; Noyes, R. W.; Parkinson,
W. H.; Reeves, E. M.; Withbroe, G. L.
1973ApJ...182..321D Altcode:
Extreme-ultraviolet spectra ( 370 A) of the brightest point in McMath
Region 10266 and of the quiet solar atmosphere are presented as measured
by the Harvard scanning spectrometer on 0S0-6. Line identifications
and physical parameters of the active region are discussed. Subject
headings: line identifications - spectra, solar - spectra, ultraviolet
---------------------------------------------------------
Title: The Extreme Ultraviolet Emissions of Solar Flares: A Comparison
between OSO-6 Spectroheliograph Observations and SFD's
Authors: Donnelly, R. F.; Wood, A. T.; Noyes, R. W., Jr.
1973SoPh...29..107D Altcode:
The time structure and intensity of OSO-6 observations of EUV bursts
were studied in relation to the corresponding 10-1030 Å enhancements
deduced from SFD data. Impulsive EUV emissions from lines normally
emitted from either the chromosphere or from the chromosphere-corona
transition region rise simultaneously with the 10-1030 Å flash,
to within the time resolution of the OSO-6 observations. Mg × 625
Å also showed concurrent impulsive emissions and a close intensity
relation to the 10-1030 Å enhancement. The observational results
are consistent with the hypothesis that most of the EUV radiation is
being produced thermally in a region of chromospheric density, which
is being heated by collisional losses of nonthermal electrons.
---------------------------------------------------------
Title: Equator-Pole Temperature Difference and the Solar Oblateness
Authors: Noyes, R. W.; Ayres, T. R.; Hall, D. N. B.
1973SoPh...28..343N Altcode:
No abstract at ADS
---------------------------------------------------------
Title: The Extreme Ultraviolet Spectrum of Solar Flares
Authors: Noyes, Robert W.
1973NASSP.342..231N Altcode: 1973heps.conf..231N
No abstract at ADS
---------------------------------------------------------
Title: Extreme-Ultraviolet Emission from Solar Prominences
Authors: Noyes, R. W.; Dupree, A. K.; Huber, M. C. E.; Parkinson,
W. H.; Reeves, E. M.; Withbroe, G. L.
1972ApJ...178..515N Altcode:
Spectra and spectroheliograms of prominences have been obtained at
wavelengths 300 A < A < 1400 A from instruments aboard the OSO 4
and OSO 6 spacecraft. Quiescent prominences appear in emission above
the limb for all strong lines formed at temperatures below 3 x 10 K,
but not at higher temperatures. The gas pressure in the 10 K transition
zone around prominences is approximately equal to that in the cooler
(6300 K) central regions. The temperature and the hydrogen ground-state
departure coefficient in the central regions are determined from
the Lymancontinuum spectrum. Prominences on the disk (filaments) are
visible in absorption in many lines, especially those at wavelengths
below the hydrogen Lyman limit at 912 A. The fractional absorption,
averaged over the spectrometer aperture, decreases regularly with
increasing temperature of line formation. The hydrogen La and Lfl lines
show only slight absorption relative to chromospheric lines lying on
top of the Lyman continuum.
---------------------------------------------------------
Title: Observing Programs in Solar Physics during the 1973 ATM
Skylab Program
Authors: Reeves, E. M.; Noyes, R. W.; Withbroe, G. L.
1972SoPh...27..251R Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Equator-Pole Differences in the Solar Chromosphere from
Lyman-Continuum Data
Authors: Vernazza, J. E.; Noyes, R. W.
1972SoPh...26..335V Altcode:
From the analysis of OSO-4 Lyman-continuum spectroheliograms,
differences in the brightness and the color temperature between the
poles and the equator have been found. These differences are interpreted
as resulting from a lower chromospheric density at the poles than at
the equator. Two models, one for the poles and one for the equator,
giving temperature and density as a function of height, explain the
observations. The poles have a lower density and a smaller temperature
gradient than the equator does. The differences begin in the middle
chromosphere and increase toward the transition zone.
---------------------------------------------------------
Title: Thermal Oscillations in the High Solar Photosphere
Authors: Noyes, Robert W.; Hall, Donald N. B.
1972ApJ...176L..89N Altcode:
Prominent 5-minute oscillations have been detected in the intensity of
the fundamental vibrationrotation lines of CO at 4.67 IL. These lines
are formed near the temperature minimum in the high photosphere, where
the thermal response to density fluctuations is nearly adiabatic. The
intensity amplitude corresponds to a temperature oscillation with
peak-to-peak amplitude of 225 K.
---------------------------------------------------------
Title: Solar Rotation as Measured in EUV Chromospheric and Coronal
Lines
Authors: Simon, George W.; Noyes, Robert W.
1972SoPh...26....8S Altcode:
Active regions were followed across the disk on OSO 4 spectroheliograms
in the Lyman continuum (LC) and in Mg X λ625. These observations
indicate differential rotation with latitude, but not with height in
the atmosphere. The measured equatorial sidereal rotation velocity
is 14.7° ±0.2° per day in both chromospheric LC and coronal Mg X,
where the quoted error is the standard deviation of a least-squares
fit to the data.
---------------------------------------------------------
Title: The Solar Euv-Emitting Plasma (invited Paper)
Authors: Noyes, R. W.; Withbroe, G. L.
1972SSRv...13..612N Altcode: 1972IAUCo..14..612N
No abstract at ADS
---------------------------------------------------------
Title: The Identification of the 1-0 and 2-1 Bands of HCI in the
Infrared Sunspot Spectrum
Authors: Hall, Donald N. B.; Noyes, Robert W.
1972ApJ...175L..95H Altcode:
Observations of the infrared umbral spectrum between 2400 and 3000
have permitted positive identification of 14 lines of the fundamental
vibration-rotation bands of HCl. A preliminary solar 35C1 abundance of
log10N(35Cl) = 5.4 + 0.3 [on a scale where log10N(H) = 12] has been
obtained. Several weak features are consistent with the presence of
87Cl with a terrestrial abundance ratio.
---------------------------------------------------------
Title: Spectra of CO Fundamental Lines and the Structure of the
High Photosphere
Authors: Noyes, R. W.; Hall, D. N. B.
1972BAAS....4..389N Altcode:
No abstract at ADS
---------------------------------------------------------
Title: An Umbral Model Atmosphere Derived from Infrared Observations
Authors: Hall, D. N. B.; Noyes, R. W.
1972BAAS....4R.383H Altcode:
No abstract at ADS
---------------------------------------------------------
Title: EUV Spectra of Prominences and Filaments
Authors: Noyes, R. W.
1972BAAS....4S.388N Altcode:
No abstract at ADS
---------------------------------------------------------
Title: On the Difference between the Poles and Equator in the Region
of Formation of the Lyman Continuum
Authors: Vernazza, J. E.; Noyes, R. W.
1972BAAS....4Q.394V Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Solar Flares in the Extreme Ultraviolet. I. The Observations
Authors: Wood, A. T., Jr.; Noyes, R. W.; Dupree, A. K.; Huber,
M. C. E.; Parkinson, W. H.; Reeves, E. M.; Withbroe, G. L.
1972SoPh...24..169W Altcode:
Solar-flare observations in the extreme ultraviolet (300-1350 Å) are
reported. Some 269 flares observed by the Harvard College Observatory
(HCO) experiment on OSO 4 and 211 flares observed by the HCO experiment
on OSO 6 have been analyzed. The flares were observed in spectral
lines and continua emitted by many ionic species over a temperature
range from 10<SUP>4</SUP> to 3.5 × 10<SUP>6</SUP> K. The EUV data
have been correlated with X-ray, Hα, and radio observations, and a
significant number of EUV bursts not associated with reported Hα,
X-ray, or radio bursts have been iden tified and investigated. The
results indicate that these latter EUV events are less energetic by
about a factor of 2 than EUV bursts associated with — F subflares.
---------------------------------------------------------
Title: Solar Flares in the Extreme Ultraviolet. II. Comparisons with
Other Observations
Authors: Wood, A. T., Jr.; Noyes, R. W.
1972SoPh...24..180W Altcode:
Extreme-ultraviolet (300-1350 Å) observations of nearly 500 solar
flares from the satellites OSO 4 and OSO 6 have been compared with data
in X-ray and radio wavelengths. It is found that EUV flares are closely
associated with nonthermal X-ray and microwave bursts. The EUV maximum
intensity generally precedes the maximum intensity in Hα or soft
X-rays by up to several minutes. The EUV e-folding rise time and peak
intensity both depend on the X-ray burst characteristics. Nonthermal
X-ray flares tend to be accompanied by strong, rapidly rising EUV
bursts, while thermal X-ray events are usually associated with weaker,
more slowly rising EUV flares. These relations are consistent with a
picture of the flare in which the EUV radiation is produced thermally
in a region of high (chromospheric) density, which is being heated
by collisional losses of the nonthermal electrons responsible for the
impulsive X-ray and microwave burst.
---------------------------------------------------------
Title: Observed Heights of EUV Lines Formed in the Transition Zone
and Corona
Authors: Simon, George W.; Noyes, Robert W.
1972SoPh...22..450S Altcode:
The heights of formation of a number of extreme ultraviolet lines in
active regions have been measured from OSO-IV spectroheliograms. Using
the Lyman continuum at 2000 km above the white light limb as
a reference, we find heights for HeI, HeII, CIII, NIII, OIV, OVI,
NeVIII, MgX, SiXII, FeXV and FeXVI that are in approximate agreement
with models based on analysis of EUV emission intensities. The height of
CII is anomalously high. The accuracy of measurement is typically about
2000 km. The data suggest that the transition zone is less steep than
calculated from EUV emission intensities; however, higher resolution
observations are necessary to resolve the discrepancy.
---------------------------------------------------------
Title: Inhomogeneous Structure of the Solar Chromosphere from
Lyman-Continuum Data
Authors: Vernazza, J. E.; Noyes, R. W.
1972SoPh...22..358V Altcode:
We describe a new model of the chromosphere based on Lyman-continuum
observations by Harvard spectrometers aboard the satellites OSO 4 and
OSO 6. The model assumes (a) that a random distribution of optically
thick inhomogeneities overlies a plane-parallel homogeneous atmosphere,
and (b) that the Lyman continuum in the chromosphere is optically
thick and the only significant opacity source between 600 and 912 Å.
---------------------------------------------------------
Title: The Identification of ^{13}C^{16}O in the Infrared Sunspot
Spectrum and the Determination of the Solar ^{12}C/^{13}C Abundance
Ratio
Authors: Hall, Donald N. B.; Noyes, Robert W.; Ayres, Thomas R.
1972ApJ...171..615H Altcode:
The presence of the first-overtone vibration-rotation bands of 13C16O
in the infrared sunspot spectrum has been established on the basis of
wavenumber and relative intensity consistency of 30 weak lines. Nine
particularly clean lines have been used to obtain a solar 12C/13C
abundance ratio of 90 with a probable error of 15 percent.
---------------------------------------------------------
Title: Extreme Ultraviolet Observations of Solar Flares
Authors: Wood, A. T., Jr.; Noyes, R. W.; Reeves, E. M.
1972PrAA...30..117W Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Coronal Electron Density Maps for 7 March, 1970, Derived from
Mgx λ625 Spectroheliograms (Papers presented at the Proceedings
of the International Symposium on the 1970 Solar Eclipse, held in
Seattle, U. S. A. , 18-21 June, 1971.)
Authors: Withbroe, G. L.; Dupree, A. K.; Goldberg, L.; Huber,
M. C. E. .; Noyes, R. W.; Parkinson, W. H.; Reeves, E. M.
1971SoPh...21..272W Altcode:
We have analyzed daily Mgx λ 625 spectroheliograms acquired by the
Harvard College Observatory experiment on OSO-6 for a 28-day period
centered on 7 March, 1970, the date of a well-observed total solar
eclipse. These data are used to construct maps of the variation across
the solar disk of the electron density at the base of the corona. The
correspondence of high and low density regions with regions of enhanced
and reduced emission in white light and Mgx pictures made during or
near the time of the eclipse are described.
---------------------------------------------------------
Title: Extreme-Ultraviolet Observations of a Surge
Authors: Kirshner, Robert P.; Noyes, Robert W.
1971SoPh...20..428K Altcode:
A flare surge at the limb was observed in CIII 977 Å by the Harvard OSO
6 spectroheliometer. The kinematic behavior of the surge is the same
in CIII and in Hα. The amount of CIII emission is consistent with a
model in which the CIII ions occupy sheaths with thickness ∼ 100 km
surrounding the cooler Hα-emitting threads. The mass of the material
containing CIII ions is about 10<SUP>−2</SUP> times that emitting Hα.
---------------------------------------------------------
Title: The Harvard-Smithsonian reference atmosphere
Authors: Gingerich, O.; Noyes, R. W.; Kalkofen, W.; Cuny, Y.
1971SoPh...18..347G Altcode:
We present a model of the solar atmosphere in the optical depth
range from τ<SUB>5000</SUB> = 10<SUP>−8</SUP> to 25. It combines
an improved model of the photosphere that incorporates recent EUV
observations with a new model of the quiet lower chromosphere. The
latter is based on OSO 4 observations of the Lyman continuum, on
infrared observations, and on eclipse electron densities.
---------------------------------------------------------
Title: EUV observations of solar flares.
Authors: Wood, A. T., Jr.; Noyes, R. W.; Reeves, E. M.
1971BAAS....3..266W Altcode:
No abstract at ADS
---------------------------------------------------------
Title: EUV emission lines: Density sensitive multiplet ratios.
Authors: Dupree, A. K.; Munro, R. H.; Noyes, R. W.; Withbroe, G. L.
1971BAAS....3Q.260D Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Solar rotation as measured in EUV chromospheric and coronal
lines.
Authors: Noyes, R. W.; Simon, G. W.
1971BAAS....3R.263N Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Observed heights of EUV lines formed in the transition zone
and corona.
Authors: Simon, G. W.; Noyes, R. W.
1971BAAS....3R.264S Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Observation of the Coronal Network
Authors: Simon, G. W.; Noyes, R. W.
1971IAUS...43..663S Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Ultraviolet Studies of the Solar Atmosphere
Authors: Noyes, Robert W.
1971ARA&A...9..209N Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Real Time Control of the Observing Program of an Orbiting
Solar Observatory
Authors: Reeves, E. M.; Huber, M. C. E.; Withbroe, G. L.; Noyes, R. W.
1971IAUS...41..336R Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Solar EUV observations: Lines of lithium-like ions.
Authors: Withbroe, G. L.; Noyes, R. W.
1971BAAS....3S.265W Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Models of the Quiet and Active Solar Atmosphere from Harvard
OSO Data
Authors: Noyes, R. W.
1971ASSL...27..192N Altcode: 1971psc..conf..192N
No abstract at ADS
---------------------------------------------------------
Title: The Solar Lyman Continuum and the Structure of the Solar
Chromosphere
Authors: Noyes, Robert W.; Kalkofen, Wolfgang
1970SoPh...15..120N Altcode:
Data on the spectrum and center-to-limb variation of the solar Lyman
continuum have been analyzed. They show: (a) The brightness temperature
of the Lyman continuum is about 6500 K, but the kinetic temperature,
as deduced from the slope of the continuum, lies between 8000 and
9000 K. The difference between the kinetic temperature and the
brightness temperature requires that the source function be smaller
than the Planck function by a factor of several hundred. (b) The
Lyman continuum exhibits slight limb darkening longward of 825 Å,
and slight limb brightening shortward of 750 Å. The crossover point
varies from equator to pole and with solar activity. (c) The slope d ln
I(λ)/dλ of the Lyman continuum decreases toward the limb, implying
that the kinetic temperature increases outward in the region of Lyman
continuum formation.
---------------------------------------------------------
Title: OSO-VI: Surges, Flares, and the Development of Active Regions
Authors: Reeves, E. M.; Dupree, A. K.; Goldberg, L.; Huber, M. C. E.;
Noyes, R. W.; Parkinson, W. H.; Withbroe, G. L.
1970BAAS....2R.215R Altcode:
No abstract at ADS
---------------------------------------------------------
Title: OSO-VI: The EUV Spectrum of Solar-Active Regions
Authors: Dupree, A. K.; Goldberg, L.; Huber, M. C. E.; Noyes, R. W.;
Parkinson, W. H.; Reeves, E. M.; Withbroe, G. L.
1970BAAS....2..191D Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Extreme Ultraviolet Observations of Active Regions in the
Chromosphere and the Corona
Authors: Noyes, Robert W.; Withbroe, George L.; Kirshner, Robert P.
1970SoPh...11..388N Altcode:
New observations of solar active regions have been obtained by
the Harvard College Observatory EUV spectroheliometer aboard the
OSO-IV spacecraft. From the observations we have determined the
enhancement in active regions of the emission from ions formed at
various temperatures in the chromosphere and corona. The results are
in accord with a simple model of active regions, for which the active
region pressure is about 5 times the quiet sun pressure; the temperature
gradient in the transition zone is about 5 times the quiet sun value;
and the coronal temperature above active regions is slightly increased.
---------------------------------------------------------
Title: OSO-VI: The Harvard Experiment
Authors: Huber, M. C. E.; Dupree, A. K.; Goldberg, L.; Noyes, R. W.;
Parkinson, W. H.; Reeves, E. M.; Withbroe, G. L.
1970BAAS....2S.200H Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Extreme Ultraviolet Observations of Active Regions in the
Chromosphere and the Corona
Authors: Noyes, R. W.; Withbroe, G. L.; Kirshner, R. P.
1969cctr.conf..125N Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Observations and Interpretation of the Solar Lyman Continuum
Authors: Noyes, Robert W.; Kalkofen, Wolfgang
1969BAAS....1R.288N Altcode:
No abstract at ADS
---------------------------------------------------------
Title: The Solar Continuum in the Far-Infrared and Millimetre Regions
Authors: Noyes, R. W.
1969RSPTA.264..205N Altcode:
No abstract at ADS
---------------------------------------------------------
Title: The differences between quiet and active regions measured by
spectroheliograms in the neutral helium resonance lines
Authors: Hearn, A. G.; Noyes, R. W.; Withbroe, G. L.
1969MNRAS.144..351H Altcode:
Spectroheliograms of the 537 and 584 A lines of neutral helium
were obtained in November 1967 by the Harvard spectroheliometer on
OSO-IV. The increased intensities of these lines in active regions
cannot be explained by an increased electron temperature. Calculations
show that the variation of the ratio of the intensity of the 537 A line
to the 584 A line as a function of the intensity of the 584 A line
is consistent with the layers emitting these lines having a higher
electron density in the active regions. The calculations require the
layer emitting the neutral helium lines in a quiet region to have an
electron temperature of 32000 K and an electron density of 4.5 X 1010
cm-3. The error in this electron density may be a factor of 3. The
active regions that have been observed require an increase in the
electron density of up to times that of a quiet region.
---------------------------------------------------------
Title: Observation of Hydrogen Fluoride in Sunspots and the
Determination of the Solar Fluorine Abundance
Authors: Hall, D. N. B.; Noyes, R. W.
1969ApL.....4..143H Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Spectral Observations of Spicules at Two Heights in the
Solar Chromosphere
Authors: Pasachoff, Jay M.; Noyes, Robert W.; Beckers, Jacques M.
1968SoPh....5..131P Altcode:
An observational program at the Sacramento Peak Observatory in
1965 provided high-dispersion spectra of the solar chromosphere in
several spectral regions simultaneously. These regions included
various combinations of the spectral lines Hα, Hβ and Hɛ, the
D<SUB>3</SUB>-line of HeI, the infrared triplet of OI, and the H-
and K-lines and the infrared triplet of CaII. With the use of an image
slicer the observations were made simultaneously at two heights in the
solar chromosphere separated by several thousand kilometers. From these
data we draw the following conclusions: Emission of different lines
arises in the same chromospheric features. The intensity ratio of lines
of different elements varies significantly from spicule to spicule. For
the H- and K-lines of ionized calcium, this ratio remains constant,
independent of wavelength throughout the line, overall intensity,
and height in the chromosphere. Two rare-earth lines in the wing of
the H-line show no spicular structure at all.
---------------------------------------------------------
Title: Ultraviolet Solar Images from Space
Authors: Goldberg, Leo; Noyes, Robert W.; Parkinson, William H.;
Reeves, Edmond M.; Withbroe, George L.
1968Sci...162...95G Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Preliminary EUV Spectroheliograms from OSO-IV
Authors: Noyes, R. W.; Goldberg, L.; Parkinson, W. H.; Reeves, E. M.;
Withbroe, G. L.
1968AJS....73R..73N Altcode:
The Harvard OSO-I V spectrometer-spectroheliometer has provided pictures
of the sun over a wide range of wavelengths originating from different
heights in the solar atmosphere, from the low chromosphere through the
corona. Lines from H I through Si XII have been observed against the
solar disk showing structure on the disk both in active regions and, in
certain cases, well above the limb. The data allow a close comparison
with simultaneous ground-based coronal observations. Representative
spectroheliograms in lines of increasing ionization potentials are
used to illustrate the size, structure, and development of active
regions on the limb and on the disk at different heights in the solar
atmosphere. Preliminary observations of limb brightening, instensity
of active regions, and flare activity are presented.
---------------------------------------------------------
Title: Observational Studies of the Solar Intensity Profile in the
Far Infrared and Millimeter Regions
Authors: Noyes, R. W.; Beckers, J. M.; Low, F. J.
1968SoPh....3...36N Altcode:
Observations of the intensity distribution near the solar limb at 2.43
and 22.5 μ, show the absence of limb brightening to within 1 or 2 arc
sec of the limb. Observations at 1.2 mm indicate limb brightening at
this wavelength. These results are compared with the Utrecht Reference
Photosphere and with existing data on the solar flux in the millimeter
range, and suggest that the temperature minimum is broad and extends
above τ<SUB>5000</SUB> = 2 × 10<SUP>−3</SUP>. A sharp rise of
temperature is required above τ<SUB>5000</SUB> = 10<SUP>−5</SUP>.
---------------------------------------------------------
Title: Infrared Intensity Distribution at the Solar Limb in the
20-MICRON Region
Authors: Noyes, R. W.
1968inas.book...77N Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Observational Studies of Velocity Fields in the Solar
Photosphere and Chromosphere
Authors: Noyes, R. W.
1967IAUS...28..293N Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Center-to-limb variations of the solar continuum in the far
infrared and millimeter wavelength regions
Authors: Noyes, R. W.; Beckers, J. M.; Low, F. J.; Davidson, A. W.
1966AJ.....71..866N Altcode:
No abstract at ADS
---------------------------------------------------------
Title: On the Infrared Continuum of the Sun and Stars
Authors: Noyes, Robert W.; Gingerich, Owen; Goldberg, Leo
1966ApJ...145..344N Altcode:
No abstract at ADS
---------------------------------------------------------
Title: New Observations of Solar Chromospheric Spicules.
Authors: Beckers, Jaques M.; Noyes, Robert W.; Pasachoff, Jay M.
1966AJ.....71T.155B Altcode:
We observed the spectra of spicules on the solar limb simultaneously at
two heights in the quiescent ebromosphere with the 16-in. coronagraph
and the 12-m Littrow spectrograph at the Sacramento Peak Observatory
during the summer of 1965. Time sequences of simultaneous observations
were obtained, using the following combinations of lines: K, H, HE,
and D3 H, HE, D3, and the 0 1 infrared triplet; H, HE, D3, and the Ca
II infrared triplet; and Hp and HCL. Time intervals between exposures
ranged from 5 to 30 sec, and the height separation was 2000 km. Our
preliminary conclusions follow. (a) A strong correlation exists between
the intensities of the spectra of spicules in HE and D3, while spectra
in H and HE show less correlation. The rare earth line between H and
HE shows no brightness or velocity structure. This suggests that it is
nonspicular in Origin. (b) We see the line-of-sight velocities of some
spicules reverse in direction. This suggests tbat the apparent rising
and subsequent falling seen in HCL on the limb may represent actual
mass motions. Further, most of il~e spicules with large line-of-sight
velocities seem to be moving faster at the higher than at the lower
levels. (c) The profiles of the H and K lines are indeed very broad with
respect to the HCL line, in agreement with Athay. It is unlikely that
these large widths are caused by overlapping spicules. (d) Many spicular
spectra are tilted with respect to the direction of the dispersion. We
believe this to be a real effect, caused by differential motions across
the spicule. (e) The H and K lines are strongly self-reversed at low
levels. We believe the self-reversal to be nonspicular in origin because
it does not share the Doppler shifts of spicules. Microphotometry and
detailed reduction of the data are underway.
---------------------------------------------------------
Title: Dielectronic Recombination and the Solar H and K Lines
Authors: Noyes, R. W.
1965SAOSR.174..405N Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Origin of Emission Cores in Lines of Ionized Calcium and
Magnesium.
Authors: Goldberg, Leo; Noyes, Robert W.
1964AJ.....69R.542G Altcode:
Transitions between doubly excited 4pnl levels and singly excited 4snl
levels of the Ca I atom are shown to be probable contributors to the
emission cores of the Ca II H and K lines in the solar spectrum. The
contribution to the source function from this process is calculated
and found to reach a maximum at a height of approximately 300 km
above the photosphere. Preliminary calculations of line profiles and
center-to-limb variations for the H and K lines of both Ca II and Mg
ii are presented and discussed.
---------------------------------------------------------
Title: Preliminary Results from a Rocket Flight of the Harvard
OSO-B Spectrometer.
Authors: Goldberg, Leo; Parkinson, W. H.; Reeves, E. M.; Noyes, R. W.
1964AJ.....69Q.140G Altcode:
A model of the Harvard OSO-B spectrometer was flown in an Aerobee-Hi
rocket from White Sands, New Mexico on 6 September 1963. During the
course of the rocket flight, which attained a peak altitude of 221 km,
three full scans and part of a fourth were obtained in the spectral
region 1350-500 A. The dimensions of the entrance slit were 1.8 arc
minutes wide by 9.0 arc minutes long. Examination of Ha and Ca K
spectroheliograms shows that the entrance aperture was free of plage
regions. The purpose of the flight was primarily to check the absolute
calibration prior to launch of a similar instrument in OSO-B and also
to obtain data on spectral intensities for the center of the quiet
sun. Essentially all emission lines found by other experimenters were
observed and good records were also obtained of the Lyman continuum. In
general, the observed numbers of counts recorded for the emission lines
are in satisfactory agreement with those predicted on the basis of
published data on photon fluxes and the absolute laboratory calibration,
but there are interesting differences which can be attributed at least
in part to the fact that the present observations refer to the center of
the quiet sun, whereas H interegger `s observations, for example, apply
to the integrated flux from the whole sun, including active regions.
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Title: Velocity Fields in the Solar Atmosphere. II. The Oscillatory
Field.
Authors: Noyes, Robert W.; Leighton, Robert B.
1963ApJ...138..631N Altcode:
From a systematic visual study of sets of "Doppler plates" obtained
at the 13-foot spectroheliograph of the Mount Wilson Observatory
during 1960 and 1961, the following results were derived: a) Vertical
oscillatory motions were found in all medium-strong lines observed. The
average period of the motions, about 290 sec, is a well-determined
quantity for each spectral line. Slight, but apparently real,
variations between the weaker and stronger lines observed suggest that
the average period gradually decreases with increasing altitude in
the line-forming regions of the upper photosphere. b) An oscillatory
fluctuation of residual intensity was found in the cores of the stronger
lines observed. The average period is somewhat shorter than that of
the velocity oscillations and also exhibits an apparent decrease with
increasing altitude. The two oscillations bear a definite phase relation
to each other, indicating that they are physically connected. Intensity
oscillations were not found in the weaker lines observed or in the core
of Ha. These observations are discussed and compared with expectations
for a plane wave propagating vertically through an isothermal atmosphere
with an altitude-dependent radiative relaxation time.
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Title: Observations of oscillatory motions in the solar atmosphere
Authors: Noyes, Robert W.
1963PhDT........26N Altcode:
This thesis presents observations of the macroscopic line-of-sight
velocity field in the solar atmosphere. The observations were made at
Mt. Wilson Observatory, primarily in 1960 and 1961. A quasi-periodic
vertical oscillatory motion has been detected in the upper photosphere
and low chromosphere. The "average period" of this oscillation has been
determined with some accuracy to be about 300 sec.; there appears to
be a slight decrease of period with increasing altitude. The mean life
of a single oscillation is about 400 sec. The “velocity elements"
which partake of the oscillation have an appearance very similar to the
photospheric granulation of low levels, and are probably identical to
it. The vertical velocity amplitude is about 1/2 km/sec at these levels,
and increases with altitude. The horizontal component of velocity is
nearly as large as the vertical at low levels, but decreases with
altitude, until at higher levels the velocities are substantially
vertical only. The mean diameter of the velocity elements is only
slightly larger than the photospheric granulation at low levels,
but increases to many times that size at higher levels. <P />We also
report in this thesis on observations of macroscopic intensity fields,
made concurrently with the velocity observations. A correlation
coefficient between intensity and velocity has been found which
appears to decrease monotonically with altitude, from about +0.5 at
the lowest elevations observed to about -0.2 at the highest observed
elevations. An oscillatory behavior of the intensity field is found
in the chromosphere, with roughly the same period as the velocity
oscillation, and evidently coupled to it. This oscillation may be
followed to considerable altitudes in the chromosphere. It is apparently
absent in the upper photosphere, however, even though the velocity
oscillation is quite strong there. <P />Also discussed are some possible
interpretations of the observations and what they might imply about
the structure of the solar atmosphere. We find that the observed period
is close to the "critical period" separating propagating and standing
acoustic waves in a gravitating atmosphere with the solar values for
temperature and gravitational field. Several possible explanations for
the decrease of period with altitude are suggested. The amplitude and
phase of the temperature fluctuations accompanying a wave propagating
in an atmosphere with radiative leakage are discussed; this leads to
a possible explanation of the presence of an intensity oscillation at
high levels and its absence at low levels, and of the reversal with
altitude of the sign of the correlation coefficient between intensity
and velocity. <P />Some observational problems are also discussed,
both in the body of the thesis (Parts I and II) and in appendices.
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Title: Velocity Fields in the Solar Atmosphere. I. Preliminary Report.
Authors: Leighton, Robert B.; Noyes, Robert W.; Simon, George W.
1962ApJ...135..474L Altcode:
Velocity fields in the solar atmosphere have been detected and measured
by an adaptation of a technique previously used for measuring magnetic
fields Data obtained during the summers of 1960 and 1961 have been
partially analyzed and yield the following principal results: 1. Large
"cells" of horizontally moving material are distributed roughly
uniformly over the entire solar surface. The motions within each
cell suggest a (horizontal) outward flow from a source inside the
cell. Typical diameters are 1.6 X 10 km; spacings between centers,
3 X 10 km ( 5 X 10 cells over the solar surface); r.m S. velocities
of outflow, 0.5 km sec-1 lifetimes, sec. There is a similarity
in appearance to the Ca+ network. The appearance and properties
of these cells suggest that they are a surface manifestation of a
"supergranulation" pattern of convective currents which come from
relatively great depths inside the sun. 2. A distinct correlation
is observed between local brightness fluctuations and vertical
velocities: bright elements tend to move upward, at the levels at
which the lines Fe X 6102 and Ca X 6103 are formed. In the line Ca
X 6103, the correlation coefficient is 0.5. This correlation appears
to reverse in sign in the height range spanned by the Doppler wings
of the Na D1 line and remains reversed at levels up to that of Ca+ X
8542. At the level of Ca X 6103, an estimate of the mechanical energy
transport yields the rather large value 2 W cm . 3. The characteristic
"cell size" of the vertical velocities appears to increase with
height from 1700 km at the level of Fe X 6102 to 3500 km at that
of Na X 5896. The r.m s. vertical velocity of 0 4 km appears nearly
constant over this height range. 4. The vertical velocities exhibit
a striking repetitive time correlation, with a period T = 296 * 3
sec. This quasi-sinusoidal motion has been followed for three full
periods in the line Ca 6103, and is also clearly present in Fe X 6102,
Na X 5896, and other lines. The energy contained in this oscillatory
motion is about 160 J cm the "losses" can apparently be compensated for
by the energy transport (2). 5. A similar repetitive time correlation,
with nearly the same period, seems to be present in the brightness {
observed on ordinary spectroheliograms taken at the center of the Na D1
line. We believe that we are observing the transformation of potential
energy into wave energy through the brightness-velocity correlation
in the photosphere, the upward propagation of this energy by waves
of rather well-defined frequency, and its dissipation into heat in
the lower chromosphere. 6. Doppler velocities have been observed at
various heights in the upper chromosphere by means of the Ha line. At
great heights one finds a granular structure with a mean size of about
3600 km, but at lower levels one finds predominantly downward motions,
which are concentrated in "tunnels" which presumably follow magnetic
lines of force and are geometrically related to the Ca+ network. The
Doppler field changes its appearance very y at higher levels, typical
lifetimes being about 30 seconds.
