explanation blue bibcodes open ADS page with paths to full text
Author name code: deming
ADS astronomy entries on 2022-09-14
author:"Deming, L. Drake"
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Title: Terrestrial Planet Optical Phase Curves. I. Direct Measurements
of the Earth
Authors: De Cock, Roderick; Livengood, Timothy A.; Stam, Daphne M.;
Lisse, Carey M.; Hewagama, Tilak; Deming, L. Drake
2022AJ....163....5D Altcode:
NASA's EPOXI mission used the Deep Impact spacecraft to observe
the disk-integrated Earth as an analog to terrestial exoplanets'
appearance. The mission took five 24 hr observations in 2008-2009 at
various phase angles (57.°7-86.°4) and ranges (0.11-0.34 au), of
which three equatorial (E1, E4, E5) and two polar (P1, North and P2,
South). The visible data taken by the HRIV instrument ranges from 0.3
to 1.0 μm, taken trough seven spectral filters that have spectral
widths of about 100 nm, and which are centered about 100 nm apart,
from 350 to 950 nm. The disk-integrated, 24 hr averaged signal is used
in a phase angle analysis. A Lambertian-reflecting, spherical planet
model is used to estimate geometric albedo for every observation
and wavelength. The geometric albedos range from 0.143 (E1, 950 nm)
to 0.353 (P2, 350 nm) and show wavelength dependence. The equatorial
observations have similar values, while the polar observations have
higher values due to the ice in view. Therefore, equatorial observations
can be predicted for other phase angles, but (Earth-like) polar views
(with ice) would be underestimated.
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Title: Characterizing Terrestrial Exoplanets
Authors: Meadows, V. S.; Lustig-Yaeger, J.; Lincowski, A.; Arney,
G. N.; Robinson, T. D.; Schwieterman, E. W.; Deming, L. D.; Tovar, G.
2017LPICo2042.4114M Altcode:
We will provide an overview of the measurements, techniques,
and upcoming missions required to characterize terrestrial planet
environments and evolution, and search for signs of habitability
and life.
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Title: Illusion and reality in the atmospheres of exoplanets
Authors: Deming, L. Drake; Seager, Sara
2017JGRE..122...53D Altcode:
The atmospheres of exoplanets reveal all their properties beyond mass,
radius, and orbit. Based on bulk densities, we know that exoplanets
larger than 1.5 Earth radii must have gaseous envelopes and, hence,
atmospheres. We discuss contemporary techniques for characterization of
exoplanetary atmospheres. The measurements are difficult, because—even
in current favorable cases—the signals can be as small as 0.001%
of the host star's flux. Consequently, some early results have been
illusory and not confirmed by subsequent investigations. Prominent
illusions to date include polarized scattered light, temperature
inversions, and the existence of carbon planets. The field moves from
the first tentative and often incorrect conclusions, converging to
the reality of exoplanetary atmospheres. That reality is revealed
using transits for close-in exoplanets and direct imaging for young
or massive exoplanets in distant orbits. Several atomic and molecular
constituents have now been robustly detected in exoplanets as small
as Neptune. In our current observations, the effects of clouds and
haze appear ubiquitous. Topics at the current frontier include the
measurement of heavy element abundances in giant planets, detection
of carbon-based molecules, measurement of atmospheric temperature
profiles, definition of heat circulation efficiencies for tidally
locked planets, and the push to detect and characterize the atmospheres
of super-Earths. Future observatories for this quest include the
James Webb Space Telescope and the new generation of extremely large
telescopes on the ground. On a more distant horizon, NASA's study
concepts for the Habitable Exoplanet Imaging Mission (HabEx) and the
Large UV/Optical/Infrared Surveyor (LUVOIR) missions could extend the
study of exoplanetary atmospheres to true twins of Earth.
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Title: A Uniform and Improved Analysis of Spitzer's Exoplanet
Eclipse Data
Authors: Deming, L.
2015adap.prop..122D Altcode:
Thermal emission measurements of exoplanets - dominated by data from
the Spitzer Space Telescope - are our only window into the temperature
structure of exoplanetary atmospheres. Our current understanding of the
temperatures and molecular abundances in giant exoplanets is built on
the foundation of Spitzer's eclipse measurements. Exoplanet eclipses
are an order of magnitude smaller than the instrument signatures in
Spitzer data. Corrections for Spitzer's instrumental signatures depend
on data analyses techniques that have evolved considerably since
the first eclipse detections a decade ago. However, several of the
key conclusions from Spitzer's eclipses have recently been questioned
based on new analyses. Resolving those questions requires improved data
analysis techniques. Fortunately, we have recently developed a new and
powerful data analysis method that can significantly strengthen and
improve the Spitzer analyses. Nearly simultaneously, powerful Bayesian
temperature and abundance retrieval techniques have emerged, that can
robustly define the range of temperature structure and molecular mixing
ratios that are consistent with the Spitzer data. Those retrievals are
especially valuable when applied to a group of planets that have been
measured using uniformly consistent analysis techniques. We propose to
re-analyze all of Spitzer's secondary eclipse data using a uniform and
improved method. Our results will address the temperature structure
and abundances in hot Jupiter to hot Neptune atmospheres, and will
define and focus the future questions to be answered via spectroscopy
from JWST.
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Title: A Statistical Characterization of the Atmospheres of Kepler's
Small Planets
Authors: Deming, L.
2014adap.prop...46D Altcode:
We propose a two year program to characterize the atmospheres of
super-Earths, mini-Neptunes, and Neptunes in the Kepler data, using
a novel statistical method. The Kepler mission is the most productive
exoplanet mission ever launched, and our program mines the Kepler data
to extract the maximum amount of information concerning the atmospheres
of Kepler's planets. We group the planets by similar physical
characteristics, then we apply a piecewise-linear transformation to
their orbital phases near transit and secondary eclipse. We thereby
scale, bin and average all of the planets in each physical grouping,
greatly increasing the signal to noise. We will detect reflected light
(and/or thermal emission) for groups of planets at secondary eclipse,
as well as refractive shoulders on their average transit curve just
before ingress and just after egress. The combination of refracted and
reflected light provides a powerful probe of the atmospheric scale
height and cloud cover on each group of planets. We demonstrate
our method on a group of small planets (sub-Saturns) observed at
secondary eclipse using Kepler's short cadence data. Our two-year
program will utilize both the short- and long cadence data for many
more planets. We will validate our eclipse analyses by applying our
method to the average secondary eclipse for a group of well-observed
Kepler hot Jupiters. Our refraction analysis will use a new numerical
code that we will validate by reproducing the amplitude of refraction
during the transit of Venus (archival data from the TRACE mission). We
also analyze control groups of planets wherein no signal is reasonably
expected, to prove the reality of the signals we detect.
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Title: NIMBUS: the Near-infrared Multi-Band Ultraprecise Spectroimager
for SOFIA
Authors: McElwain, Michael W.; Mandell, Avi; Woodgate, Bruce;
Spiegel, David S.; Madhusudhan, Nikku; Amatucci, Edward; Blake, Cullen;
Budinoff, Jason; Burgasser, Adam; Burrows, Adam; Clampin, Mark; Conroy,
Charlie; Deming, L. Drake; Dunham, Edward; Foltz, Roger; Gong, Qian;
Knutson, Heather; Muench, Theodore; Murray-Clay, Ruth; Peabody, Hume;
Rauscher, Bernard; Rinehart, Stephen; Villanueva, Geronimo
2012SPIE.8446E..7BM Altcode: 2012arXiv1208.0832M
We present a new and innovative near-infrared multi-band ultraprecise
spectroimager (NIMBUS) for SOFIA. This design is capable of
characterizing a large sample of extrasolar planet atmospheres
by measuring elemental and molecular abundances during primary
transit and occultation. This wide-field spectroimager would also
provide new insights into Trans-Neptunian Objects (TNO), Solar System
occultations, brown dwarf atmospheres, carbon chemistry in globular
clusters, chemical gradients in nearby galaxies, and galaxy photometric
redshifts. NIMBUS would be the premier ultraprecise spectroimager by
taking advantage of the SOFIA observatory and state of the art infrared
technologies. This optical design splits the beam into eight separate
spectral bandpasses, centered around key molecular bands from 1 to
4μm. Each spectral channel has a wide field of view for simultaneous
observations of a reference star that can decorrelate time-variable
atmospheric and optical assembly effects, allowing the instrument
to achieve ultraprecise calibration for imaging and photometry for a
wide variety of astrophysical sources. NIMBUS produces the same data
products as a low-resolution integral field spectrograph over a large
spectral bandpass, but this design obviates many of the problems that
preclude high-precision measurements with traditional slit and integral
field spectrographs. This instrument concept is currently not funded
for development.
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Title: Properties of an Earth-Like Planet Orbiting a Sun-Like Star:
Earth Observed by the EPOXI Mission
Authors: Livengood, Timothy A.; Deming, L. Drake; A'Hearn, Michael
F.; Charbonneau, David; Hewagama, Tilak; Lisse, Carey M.; McFadden,
Lucy A.; Meadows, Victoria S.; Robinson, Tyler D.; Seager, Sara;
Wellnitz, Dennis D.
2011AsBio..11..907L Altcode:
No abstract at ADS
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Title: A NIR spectrum of a hot Jupiter from the ground: Preliminary
results
Authors: Mandell, Avi M.; Deming, L. Drake; Blake, Geoffrey A.;
Knutson, Heather A.; Mumma, Michael J.; Villanueva, Geronimo L.;
Salyk, Colette
2011IAUS..276..158M Altcode:
High resolution NIR spectroscopy offers an excellent complement to
the expanding dataset of transit and secondary eclipse observations
of exo-planets with Spitzer that have provided the bulk of our
understanding of the atmospheres and internal structure of these
objects. High-resolution data can quantify the vertical temperature
structure by isolating specific spectral lines formed at various
depths. The presence of an opaque absorbing layer can also be inferred -
and its pressure level determined quantitatively - via its effect on
spectral line intensities. <P />We have analyzed data for a single
secondary eclipse of the bright transiting exo-planet host star
HD189733 at L-band wavelengths (3-4 μm) using the NIRSPEC instrument
on Keck-II. We utilize a sophisticated first-order telluric absorption
modeling technique that, combined with a calibration star, has already
been proven to remove the effects of varying atmospheric transmittance
and allow us to reach unprecedented S/N. We are conducting validation
of the final data reduction products and developing high-resolution
atmospheric models for comparison, but we have already been able to
rule out emission from methane as reported by Swain et al. (2010). We
present preliminary results and discuss future plans for analysis
and observations.
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Title: Alien Earth: Glint observations of a remote planet
Authors: Barry, Richard K.; Deming, L. Drake
2011IAUS..276..471B Altcode:
We give a preliminary report on a multi-wavelength study of specular
reflections from the oceans and clouds of Earth. We use space-borne
observations from a distance sufficient to ensure that light rays
reflected from all parts of Earth are closely parallel, as they will be
when studying exoplanets. We find that the glint properties of Earth in
this far-field vantage point are surprising - in the sense that some
of the brightest reflections are not from conventional ocean-glints,
but appear to arise from cirrus cloud crystals. The Earth observations
discussed here were acquired with the High Resolution Instrument
(HRI) - a 0.3 m f/35 telescope on the Deep Impact (DI) spacecraft
during the Extrasolar Planet Observation and Characterization (EPOCh)
investigation.
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Title: Views from EPOXI: Colors in Our Solar System as an Analog
for Extrasolar Planets
Authors: Crow, Carolyn A.; McFadden, L. A.; Robinson, T.; Meadows,
V. S.; Livengood, T. A.; Hewagama, T.; Barry, R. K.; Deming, L. D.;
Lisse, C. M.; Wellnitz, Dennis
2011ApJ...729..130C Altcode:
The first visible-light studies of Earth-sized extrasolar planets will
employ photometry or low-resolution spectroscopy. This work uses EPOCh
medium-band filter photometry between 350 and 950 nm obtained with
the Deep Impact (DI) High Resolution Instrument (HRI) of Earth, the
Moon, and Mars in addition to previous full-disk observations of the
other six solar system planets and Titan to analyze the limitations
of using photometric colors to characterize extrasolar planets. We
determined that the HRI 350, 550, and 850 nm filters are optimal for
distinguishing Earth from the other planets and separating planets to
first order based on their atmospheric and surface properties. Detailed
conclusions that can be drawn about exoplanet atmospheres simply from
a color-color plot are limited due to potentially competing physical
processes in the atmosphere. The presence of a Rayleigh scattering
atmosphere can be detected by an increase in the 350-550 nm brightness
ratio, but the absence of Rayleigh scattering cannot be confirmed due
to the existence of atmospheric and surface absorbing species in the
UV. Methane and ammonia are the only species responsible for strong
absorption in the 850 nm filter in our solar system. The combination
of physical processes present on extrasolar planets may differ from
those we see locally. Nevertheless, a generation of telescopes capable
of collecting such photometric observations can serve a critical role
in first-order characterization and constraining the population of
Earth-like extrasolar planets.
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Title: Views from EPOXI: Colors in our Solar System as an Analog
for Extrasolar Planets
Authors: Crow, Carolyn; McFadden, L. A.; Robinson, T.; Meadows, V.;
Livengood, T. A.; Hewagama, T.; Barry, R. K.; Deming, L. D.; Lisse,
C. M.
2010DPS....42.5206C Altcode: 2010BAAS...42Q1071C
The first visible light studies of Earth-sized extrasolar planets
will employ photometry or low-resolution spectroscopy. We analyzed
the limitations of using photometric colors to characterize extrasolar
planets using EPOCh medium-band filter photometry between 350 and 950 nm
obtained with the Deep Impact (DI) High Resolution Instrument (HRI) of
the Earth, Moon, and Mars in addition to previous full-disk observations
of the other six solar system planets and Titan. We determined the
HRI 350, 550, and 850 nm filters are optimal for distinguishing Earth
from the other planets and separating planets to first order based on
their atmospheric and surface properties. As in this study, detailed
conclusions that can be drawn about exoplanet atmospheres simply from
a color-color plot are limited due to potentially competing physical
processes in the atmosphere. For example, the presence of a Rayleigh
scattering atmosphere can be detected by an increase between 350 to
550 nm, but the absence or Rayleigh scattering cannot be confirmed
due to the existence of atmospheric and surface absorbing species
in the UV. We also observed that methane and ammonia are the only
species responsible for absorption in the 850 nm filter in our Solar
System. The combination of physical processes present on extrasolar
planets may differ from those we see locally. Nevertheless, a generation
of telescopes capable of collecting such photometric observations can
serve a critical role in first order characterization and constraining
the population of Earth-like extrasolar planets.
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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
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Title: Development and utilization of a point spread function for
the Extrasolar Planet Observation and Characterization/Deep Impact
Extended Investigation (EPOXI) Mission
Authors: Barry, R. K.; Lindler, D.; Deming, L. D.; A'Hearn, M. F.;
Ballard, S.; Carcich, B.; Charbonneau, D.; Christiansen, J.; Hewagama,
T.; McFadden, L.; Wellnitz, D.
2010SPIE.7731E..3DB Altcode: 2010SPIE.7731E.107B
The Extrasolar Planet Observation Characterization and the Deep Impact
Extended Investigation missions (EPOXI) are currently observing the
transits of exoplanets, a comet nucleus at short range, and Earth
using the High Resolution Instrument (HRI) - a 0.3 m f/35 telescope
- on the Deep Impact flyby spacecraft. The HRI is in a permanently
defocused state with the instrument point of focus about 0.6 cm
before the focal plane due to the use of a reference flat mirror
that became a powered optic due to thermal warping during ground
thermal-vacuum testing. Consequently, the point spread function (PSF)
covers approximately nine pixels FWHM and is characterized by a patch
with three-fold symmetry due to the three-point support structures
of the primary and secondary mirrors. The PSF is also strongly color
dependent varying in shape and size with change in filtration and
target color. While defocus is highly desirable for exoplanet transit
observations to limit sensitivity to intra-pixel variation, it is
suboptimal for observations of spatially resolved targets. Consequently,
all images used in our analysis of such objects were deconvolved with
an instrument PSF. The instrument PSF is also being used to optimize
transit analysis. We discuss development and usage of an instrument
PSF for these observations.
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Title: Earth as an Extrasolar Planet: Comparing Polar and Equatorial
Views
Authors: Shields, A. L.; Meadows, V. S.; Robinson, T. D.; Deming,
L. D.; A'Hearn, M. F.; Charbonneau, D.; Hewagama, T.; Lisse, C.;
Livengood, T.; McFadden, L.; Seager, S.; Welnitz, D. D.; Epoxi
Earthling Team
2010LPICo1538.5408S Altcode:
We present data-model comparisons for EPOXI observations of the
distant Earth's equator and poles modelled with the NAI's VPL 3D
Earth Model. These are being used to determine the detectability of
habitability for different planetary inclinations.
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Title: A Time-Dependent Radiative Model for the Atmosphere of the
Eccentric Exoplanets
Authors: Iro, N.; Deming, L. D.
2010ApJ...712..218I Altcode:
We present a time-dependent radiative model for the atmosphere
of extrasolar planets that takes into account the eccentricity of
their orbit. In addition to the modulation of stellar irradiation by
the varying planet-star distance, the pseudo-synchronous rotation
of the planets may play a significant role. We include both of
these time-dependent effects when modeling the planetary thermal
structure. We investigate the thermal structure and spectral
characteristics for time-dependent stellar heating for two highly
eccentric planets. Finally, we discuss observational aspects for those
planets suitable for Spitzer measurements and investigate the role of
the rotation rate.
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Title: Transiting Exoplanet Survey Satellite (TESS)
Authors: Ricker, George R.; Latham, D. W.; Vanderspek, R. K.; Ennico,
K. A.; Bakos, G.; Brown, T. M.; Burgasser, A. J.; Charbonneau,
D.; Clampin, M.; Deming, L. D.; Doty, J. P.; Dunham, E. W.; Elliot,
J. L.; Holman, M. J.; Ida, S.; Jenkins, J. M.; Jernigan, J. G.; Kawai,
N.; Laughlin, G. P.; Lissauer, J. J.; Martel, F.; Sasselov, D. D.;
Schingler, R. H.; Seager, S.; Torres, G.; Udry, S.; Villasenor, J. N.;
Winn, J. N.; Worden, S. P.
2010AAS...21545006R Altcode: 2010BAAS...42..459R
TESS is a low-cost SMEX-class satellite mission. In a two-year all-sky
survey, TESS will observe more than 2,000,000 nearby stars, searching
for temporary drops in brightness caused by planetary transits. <P
/>TESS is expected to identify more than 1000 transiting exoplanet
candidates, including a sample of about 100 Super Earths---small
rock-and-ice planets in the range 1 to 10 Earth masses---orbiting F,
G, K, and M dwarfs. TESS's "wide-shallow” survey complements the
"narrow-deep” CoRoT and Kepler surveys. TESS-discovered transiting
systems will be nearby (< 50 pc), and typically 10-20 x brighter than
those discovered by CoRoT and Kepler. Thus, the resulting TESS Transit
Catalog will comprise all of the best transiting systems for follow-up
observations. TESS will identify Super Earths orbiting IR-bright stars,
within reach of JWST spectroscopic searches for planetary water and
carbon dioxide. <P />TESS is a collaborative effort led by researchers
at the Massachusetts Institute of Technology, the Harvard-Smithsonian
Center for Astrophysics, and the NASA Ames Research Center. Additional
TESS scientific partners include Las Cumbres Observatory Global
Telescope, Lowell Observatory, the NASA Goddard Space Flight Center,
the Infrared Processing and Analysis Center at the California Institute
of Technology, the Geneva Observatory (Switzerland), the Tokyo Institute
of Technology (Japan), and Institut Supérieur de l'Aéronautique et
de l'Espace (France). <P />TESS was funded by NASA for a Phase A study
from May 2008 - June 2009, but was not selected for flight. Additional
funding leading to a flight opportunity is being sought. Support has
also been provided by the Kavli Foundation, Google, and the Smithsonian
Institution. TESS could launch as early as 2013-2014.
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Title: Estimates of the Population of Exoplanets Discoverable by
the Transiting Exoplanet Survey Satellite (TESS)
Authors: Seager, Sara; Winn, J. N.; Ricker, G. R.; Latham, D. W.;
Vanderspek, R. K.; Ennico, K. A.; Bakos, G.; Brown, T. M.; Burgasser,
A. J.; Charbonneau, D.; Clampin, M.; Deming, L. D.; Doty, J. P.;
Dunham, E. W.; Elliot, J. L.; Holman, M. J.; Ida, S.; Jenkins,
J. M.; Jernigan, J. G.; Kawai, N.; Laughlin, G. P.; Lissauer, J. J.;
Martel, F.; Sasselov, D. D.; Schingler, R. H.; Torres, G.; Udry, S.;
Villasenor, J. N.; Worden, S. P.
2010AAS...21545004S Altcode: 2010BAAS...42R.458S
In a two year survey, the Transiting Exoplanet Survey Satellite
(TESS) will search the entire sky for planets orbiting nearby,
bright stars. In this paper, we calculate the number of transiting
planets that TESS will detect, as a function of the properties of the
planet and the properties of the host star. The ingredients in this
calculation are divided into five groups: <P />The properties of the
planet: its radius r and orbital distance a. <P />The properties of
the star: its luminosity L, mass M, radius R, and number density n in
our Galactic neighborhood. <P />The TESS instrumental parameters: its
effective area, bandpass, and limiting photometric precision. <P />The
TESS survey parameters: the characteristics of the input catalog (2.5
million V < 13.5 dwarfs over the whole sky), observing duty cycle
(observing a given star 10.3% of the time), and duration of observations
for a given star (72 days). <P />The abundance of planets around stars,
which may depend on r, a, and L <P />The calculation is performed for
a three-dimensional grid of planet/star/orbit combinations, in which
the three parameters are the planet radius r, the stellar luminosity L,
and the orbital distance a. For the range of instrument and population
parameters and assumptions considered, we estimate that TESS will detect
1600-2700 planets in total, of which 100-300 should be small planets:
SuperEarths or Earths. <P />Support for this work has been provided
by NASA, the Kavli Foundation, Google, and the Smithsonian Institution.
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Title: Monte Carlo Simulations of Transit Light Curves for the
Transiting Exoplanet Survey Satellite (TESS)
Authors: Jernigan, J. G.; Villasenor, J. N.; Ricker, G. R.; Latham,
D. W.; Vanderspek, R. K.; Ennico, K. A.; Bakos, G.; Brown, T. M.;
Burgasser, A. J.; Charbonneau, D.; Clampin, M.; Deming, L. D.;
Doty, J. P.; Dunham, E. W.; Elliot, J. L.; Holman, M. J.; Ida, S.;
Jenkins, J. M.; Kawai, N.; Laughlin, G. P.; Lissauer, J. J.; Martel,
F.; Sasselov, D. D.; Schingler, R. H.; Seager, S.; Torres, G.; Udry,
S.; Winn, J. N.; Worden, S. P.
2010AAS...21545003J Altcode: 2010BAAS...42..458J
During the Phase A for TESS, simulations of planetary transits were
performed to confirm the instrument's ability to detect transits. The
simulations cover the full TESS discovery space in the planet
period-transit duration plane. Examples included a 36-day period planet,
two previously known systems (HAT-P-11 and CoRoT 7B), and one Earth
and one SuperEarth. In addition, a broad matrix of planetary periods
and transit depths were also simulated. We present simulated light
curves of transiting planets that are typical of those that TESS will
detect. Each light curve is computed via a Monte Carlo algorithm. The
timing of the optical emission includes the parameters of orbital
motion for the planet-star system. All simulations include estimates
of the noise from the following effects: spacecraft pointing jitter,
vignetting, optical PSF wings, background effects, CCD gain and bias
instability, sky background, and intrinsic stellar variability. The
stellar variability includes a scaled, full temporal power spectrum
of the Sun. Typical light curves of planet-star systems are simulated
for a 72 day duration with a 10 minute time resolution of each TESS
sample. These simulated light curves are analyzed to determine estimates
of the S/N for detection for each simulated system. Support for this
work has been provided by NASA, the Kavli Foundation, Google, and the
Smithsonian Institution.
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Title: High-Precision Imaging Photometers for the Transient Exoplanet
Survey Satellite
Authors: Kraft Vanderspek, Roland; Ricker, G. R.; Latham, D. W.;
Ennico, K.; Bakos, G.; Brown, T. M.; Burgasser, A. J.; Charbonneau,
D.; Clampin, M.; Deming, L.; Doty, J. P.; Dunham, E. W.; Elliot,
J. L.; Holman, M. J.; Ida, S.; Jenkins, J. M.; Jernigan, J. G.;
Kawai, N.; Laughlin, G. P.; Lissauer, J. J.; Martel, F.; Sasselov,
D. D.; Schingler, R. H.; Seager, S.; Szentgyorgyi, A.; Torres, G.;
Udry, S.; Villasenor, J. N.; Winn, J. N.; Worden, S. P.
2010AAS...21545007K Altcode: 2010BAAS...42..459K
The Transient Exoplanet Survey Satellite (TESS) is designed to
search for transiting exoplanet systems around all stars with V <
12. The TESS payload consists of a bank of six identical, wide-field,
high-precision imaging photometers. When deployed on the highly-stable
TESS satellite platform, these photometers can perform <200 ppm
photometry for V=8 stars (∼100 ppm for V=6 stars) in a 10-minute
observation. We describe the components of the TESS imaging photometers:
the custom, wide-field optics; the large-area CCD arrays; and the
low-power, high precision CCD electronics. Support for TESS has been
provided by NASA, the Kavli Foundation, Google, and the Smithsonian
Institution.
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Title: Data Network for the TESS Mission
Authors: Martel, Francois; Villasenor, J. N.; Ricker, G. R.; Latham,
D. W.; Vanderspek, R. K.; Ennico, K. A.; Bakos, G.; Brown, T. M.;
Burgasser, A. J.; Charbonneau, D.; Clampin, M.; Deming, L. D.; Doty,
J. P.; Dunham, E. W.; Elliot, J. L.; Holman, M. J.; Ida, S.; Jenkins,
J. M.; Jernigan, J. G.; Kawai, N.; Laughlin, G. P.; Lissauer, J. J.;
Sasselov, D. D.; Schingler, R. H.; Seager, S.; Torres, G.; Udry, S.;
Winn, J. N.; Worden, S. P.
2010AAS...21545002M Altcode: 2010BAAS...42..458M
The Transiting Exoplanet Survey Satellite (TESS) is designed for an
all-sky photometric survey of bright stars, extending&nbspover the
entire celestial sphere.&nbspTESS will catalog planetary transits
of nearby stars that can be followed-up with ground observatories. The
satellite cameras will perform measurements of 2,500,000 stars with
brightness ranging from V=4.5 to V=13.5 within two years, and download
typically 4.7 G Bytes of data per day.&nbspWe describe the TESS
operation plan and the communication and ground system designed to
download and process the TESS data. The dedicated ground system uses
a network of S-band ground stations spaced around the equator which
allows three communications passes per orbit, at data rates of 3.5
Mbit/sec, for up to 45 data downloads per day. Satellite operations
and data download are controlled remotely through the internet by
the TESS Mission Operation Center at NASA Ames Research Center, which
transfers the TESS observation data for processing and distribution to
the Science Operation Center managed by &nbspMIT and Harvard-SAO
in Cambridge. Support for this work has been provided by NASA, the
Kavli Foundation, Google, and the Smithsonian Institution.
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Title: Transiting Exoplanet Survey Satellite (TESS) Community Observer
Program including the Science Enhancement Option Box (SEO Box) -
12 TB On-board Flash Memory for Serendipitous Science
Authors: Schingler, Robert; Villasenor, J. N.; Ricker, G. R.; Latham,
D. W.; Vanderspek, R. K.; Ennico, K. A.; Lewis, B. S.; Bakos, G.;
Brown, T. M.; Burgasser, A. J.; Charbonneau, D.; Clampin, M.; Deming,
L. D.; Doty, J. P.; Dunham, E. W.; Elliot, J. L.; Holman, M. J.; Ida,
S.; Jenkins, J. M.; Jernigan, J. G.; Kawai, N.; Laughlin, G. P.;
Lissauer, J. J.; Martel, F.; Sasselov, D. D.; Seager, S.; Torres,
G.; Udry, S.; Winn, J. N.; Worden, S. P.
2010AAS...21545001S Altcode: 2010BAAS...42Q.458S
The Transiting Exoplanet Survey Satellite (TESS) will perform an
all-sky survey in a low-inclination, low-Earth orbit. TESS's 144
GB of raw data collected each orbit will be stacked, cleaned, cut,
compressed and downloaded. The Community Observer Program is a Science
Enhancement Option (SEO) that takes advantage of the low-radiation
environment, technology advances in flash memory, and the vast amount
of astronomical data collected by TESS. The Community Observer Program
requires the addition of a 12 TB "SEO Box” inside the TESS Bus. The
hardware can be built using low-cost Commercial Off-The-Shelf (COTS)
components and fits within TESS's margins while accommodating GSFC
gold rules. <P />The SEO Box collects and stores a duplicate of the
TESS camera data at a "raw” stage ( 4.3 GB/orbit, after stacking and
cleaning) and makes them available for on-board processing. The sheer
amount of onboard storage provided by the SEO Box allows the stacking
and storing of several months of data, allowing the investigator
to probe deeper in time prior to a given event. Additionally, with
computation power and data in standard formats, investigators can
utilize data-mining techniques to investigate serendipitous phenomenon,
including pulsating stars, eclipsing binaries, supernovae or other
transient phenomena. <P />The Community Observer Program enables ad-hoc
teams of citizen scientists to propose, test, refine and rank algorithms
for on-board analysis to support serendipitous science. Combining
"best practices” of online collaboration, with careful moderation
and community management, enables this `crowd sourced’ participatory
exploration with a minimal risk and impact on the core TESS Team. This
system provides a powerful and independent tool opening a wide range of
opportunity for science enhancement and secondary science. <P />Support
for this work has been provided by NASA, the Kavli Foundation, Google,
and the Smithsonian Institution.
---------------------------------------------------------
Title: Our Solar System at Low Spectral Resolution: A Starting Point
for Characterizing Colors of Other Systems
Authors: Crow, Carolyn A.; McFadden, L. A.; Livengood, T. A.; Hewagama,
T.; Barry, R.; Deming, L. D.
2009DPS....41.0808C Altcode:
One of the next frontiers in extrasolar planet exploration is color
characterization. We have analyzed images of the Earth and Moon acquired
during the EPOXI mission with the High Resolution Instrument (HRI)
and seven color filters, and compiled disk-integrated spectra for a
range of Solar System planets from previous studies. These data form a
basis for characterizing exoplanetary systems in the future. The images
used for this study were taken on January 16, 2005 and May 29, 2008 by
the Deep Impact spacecraft's HRI at distances of 1.64x10<SUP>6</SUP>
km and 0.33 AU, phase angles of 97.6° and 75.1°, resolutions of 3.3
and 99.0 km/pix, respectively. We derived disk-integrated spectra
of the Earth and far side of the Moon in addition to regionally
integrated spectra of the Sahara Desert, African savanna, northern
and southern hemispheres of the lunar far side, and various regions of
the lunar near side. Ground based low-resolution spectra of lunar near
side regions from McCord et al. 1972 were compared with our data for
verification. We also convolved disk-integrated spectra of Jupiter,
Saturn, Uranus, Neptune, and Titan (Karkoschka 1994, 1998) with the
HRI filter transmission curves to compare the low-resolution spectral
features of gaseous planets with those of terrestrial bodies. The
resulting spectra of the Moon and Earth are similar to what is expected
for rocky bodies with and without an atmosphere, and the spectra of the
Sahara and savanna are also what is expected of dry desert and vegetated
regions. We observe that the low-resolution spectral signatures of the
Giant Planets, the Moon and Earth are unique. A solar system like our
own would have these characteristic spectral features at low resolution
and visible wavelengths.
---------------------------------------------------------
Title: Transiting Exoplanet Survey Satellite (TESS)
Authors: Ricker, George R.; Latham, D. W.; Vanderspek, R. K.; Ennico,
K. A.; Bakos, G.; Brown, T. M.; Burgasser, A. J.; Charbonneau,
D.; Clampin, M.; Deming, L. D.; Doty, J. P.; Dunham, E. W.; Elliot,
J. L.; Holman, M. J.; Ida, S.; Jenkins, J. M.; Jernigan, J. G.; Kawai,
N.; Laughlin, G. P.; Lissauer, J. J.; Martel, F.; Sasselov, D. D.;
Schingler, R. H.; Seager, S.; Torres, G.; Udry, S.; Villasenor, J. S.;
Winn, J. N.; Worden, S. P.
2009AAS...21430605R Altcode:
The Transiting Exoplanet Survey Satellite (TESS) is a low
cost, SMEX-class planet finder. In a two year all-sky survey,
TESS will observe more than two million bright, nearby stars,
searching for temporary drops in brightness that are caused by
planetary transits. Such transits not only provide the means of
identifying the planet, but also provide knowledge of the planet's
diameter, mass density, surface gravity, temperature, and other key
properties. TESS is expected to detect more than 1000 transiting
exoplanet candidates. These detections will include a sample of
100 Super Earths -- small rock-and-ice planets with masses in the
range 1 to 10 Earth masses -- orbiting nearby stars with spectral
types spanning a broad range, including F, G, K, and M dwarfs. No
ground-based survey can achieve this feat. TESS's "wide-shallow" survey
complements the "narrow-deep" Corot and Kepler mission surveys. The
resulting TESS Transit Catalog of the nearest and brightest stars
in the sky will constitute a unique scientific legacy for followup
observations. TESS will identify Super Earths orbiting IR-bright stars,
ideal for JWST searches for planetary water and carbon dioxide. <P
/>The TESS mission is a collaborative effort led by researchers at
the Massachusetts Institute of Technology, the Harvard-Smithsonian
Center for Astrophysics, and the NASA Ames Research Center. Additional
TESS partners include ATK Space Systems, the Las Cumbres Observatory
Global Telescope Network, Lowell Observatory, the NASA Goddard Space
Flight Center, the Infrared Processing and Analysis Center at the
California Institute of Technology, the University of California
(Berkeley and Santa Cruz), the SETI Institute, Espace Incorporated,
the Geneva Observatory (Switzerland), the Tokyo Institute of Technology
(Japan), and Institut Supérieur de l'Aéronautique et de l'Espace
(France). <P />TESS is currently completing a NASA-funded Phase A study,
and is proposed for launch in December 2012.
---------------------------------------------------------
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: The Transiting Exoplanet Survey Satellite (TESS)
Authors: Ricker, George R.; Latham, D. W.; Vanderspek, R. K.; Ennico,
K. A.; Bakos, G.; Brown, T. M.; Burgasser, A. J.; Charbonneau, D.;
Deming, L. D.; Doty, J. P.; Dunham, E. W.; Elliot, J. L.; Holman,
M. J.; Ida, S.; Jenkins, J. M.; Jernigan, J. G.; Kawai, N.; Laughlin,
G. P.; Lissauer, J. J.; Martel, F.; Sasselov, D. D.; Schingler,
R. H.; Seager, S.; Torres, G.; Udry, S.; Villasenor, J. S.; Winn,
J. N.; Worden, S. P.
2009AAS...21340301R Altcode: 2009BAAS...41..193R
The Transiting Exoplanet Survey Satellite (TESS) is a low cost,
SMEX-class planet finder. In a two year all-sky survey, TESS will
observe more than two million bright, nearby stars, searching for
temporary drops in brightness that are caused by planetary transits,
which occur when a planet's orbit carries it directly in front of its
parent star. Such transits not only provide the means of identifying
the planet, but also provide knowledge of the planet's diameter, mass
density, surface gravity, temperature, and other key properties. <P
/>TESS is expected to catalog more than 1000 transiting exoplanet
candidates--20 times as many as are presently known, including a
sample of 'super Earths'. The TESS "wide-shallow" survey will be
complementary to the "narrow-deep" ones of the Corot and Kepler
missions: its sky coverage will exceed that of Corot by 1000 times,
and that of Kepler by 400 times. Because the TESS all-sky survey will
systematically examine every interesting bright star likely to harbor an
exoplanet, the resulting TESS Transit Catalog will constitute a unique
scientific legacy. High resolution, follow-up ground-based optical and
space-based IR spectroscopy of exoplanets demands bright targets. Thus,
TESS should identify those new exoplanets that are ideal for study
with the world's largest ground-based telescopes, as well as with
NASA's upcoming James Webb Space Telescope. <P />The TESS mission is a
collaborative effort led by researchers at MIT, the Harvard-Smithsonian
Center for Astrophysics, and the NASA Ames Research Center. Additional
TESS partners include the NASA Goddard Space Flight Center, the Harvard
Origins of Life Initiative, Lowell Observatory, Caltech's IPAC, the
SETI Institute, Geneva Observatory in Switzerland, Tokyo Institute
of Technology, SUPAERO in France, ATK Space, Espace Inc, and the Las
Cumbres Observatory Global Telescope Network. TESS has been accepted
for Phase A study by NASA, and is proposed for launch in late 2012.
---------------------------------------------------------
Title: The Fourier Kelvin Stellar Interferometer (FKSI): A Probe-class
Infrared Space Mission for the Spectroscopic Characterization of
Exoplanets, Exozodi Levels, Debris Disks, and High Angular Resolution
Astrophysics
Authors: Barry, Richard K.; Danchi, W. C.; Deming, L. D.; Lawsen,
P.; Traub, W.; Unwin, S.
2009AAS...21333601B Altcode: 2009BAAS...41..397B
The Fourier-Kelvin Stellar Interferometer (FKSI) mission is
a two-telescope infrared space interferometer with a 12.5 meter
baseline on a boom, operating in the spectral range 3 to 8 (or 10)
microns, and passively cooled to about 60 K. The main goals for the
mission are the measurement and characterization of the exozodiacal
emission around nearby stars, debris disks, and the atmospheres of
known exoplanets, and the search for Super Earths around nearby
stars. We discuss progress on this mission in the context of the
upcoming Decadal Survey, in particular how FKSI is ideally suited to
be an Exoplanet Probe mission in terms of crucial observations which
should be done before a flagship mission can be undertaken, as well
as technical readiness, cost, and risk.
---------------------------------------------------------
Title: Chromospheric Lines as Diagnostics of Stellar Oscillations
Authors: Paulson, Diane B.; Pesnell, W. Dean; Deming, L. Drake; Snow,
Martin; Metcalfe, Travis S.; Woods, Tom; Hesman, Brigette
2008psa..conf..311P Altcode:
Gravitational waves in the chromosphere, theorized as early as
1963 [10], are thoroughly explored in the more recent papers by
[7, 8]. Theory predicts that the convective overshoot in the upper
photosphere and low chromosphere will readily excite gravity waves. [9]
note that these waves are not easily detected because of the long
periods, short wavelengths required and slanted propagation angles of
the waves themselves (causing small velocity shifts and short duration
on individual detector pixels). Recently, [9] find evidence for gravity
waves manifested in the f 700Å chromospheric line with frequencies
<1 mHz.
---------------------------------------------------------
Title: Solar Magnetograms at 12 μm Using the Celeste Spectrograph
Authors: Moran, Thomas G.; Jennings, Donald E.; Deming, L. Drake;
McCabe, George H.; Sada, Pedro V.; Boyle, Robert J.
2007SoPh..241..213M Altcode:
We present the first solar vector magnetogram constructed from
measurements of infra-red Mg I 12.32-μm line spectra. Observations
were made at the McMath-Pierce Telescope using the Celeste
spectrometer/polarimeter. Zeeman-split Stokes line spectra were fitted
with Seares profiles to obtain the magnetic field parameters. Maps
of absolute field strength, line-of-sight angle, and azimuth are
presented. Analysis shows that the variation in field strength
within a spatial resolution element, 2 arcseconds, is greatest in the
sunspot penumbra and that this is most likely caused by vertical field
strength gradients, rather than horizontal image smearing. Widths of
the Zeeman-split σ components, assuming a formation layer thickness
of 200 km, indicate that vertical field strength gradients can be as
large as 6.5 G/km in a penumbra.
---------------------------------------------------------
Title: The Fourier-Kelvin Stellar Interferometer: a low-complexity
low-cost space mission for high-resolution astronomy and direct
exoplanet detection
Authors: Barry, R. K.; Danchi, W. C.; Deming, L. D.; Richardson, L. J.;
Kuchner, M. J.; Seager, S.; Frey, B. J.; Martino, A. J.; Lee, K. A.;
Zuray, M.; Rajagopal, J.; Hyde, T. T.; Millan-Gabete, R.; Monnier,
J. D.; Allen, R. J.; Traub, W. A.
2006SPIE.6265E..1LB Altcode: 2006SPIE.6265E..46B
The Fourier-Kelvin Stellar Interferometer (FKSI) is a mission concept
for a spacecraft-borne nulling interferometer for high-resolution
astronomy and the direct detection of exoplanets and assay of their
environments and atmospheres. FKSI is a high angular resolution
system operating in the near to mid-infrared spectral region and is a
scientific and technological pathfinder to the Darwin and Terrestrial
Planet Finder (TPF) missions. The instrument is configured with an
optical system consisting, depending on configuration, of two 0.5 -
1.0 m telescopes on a 12.5 - 20 m boom feeding a symmetric, dual Mach-
Zehnder beam combiner. We report on progress on our nulling testbed
including the design of an optical pathlength null-tracking control
system and development of a testing regime for hollow-core fiber
waveguides proposed for use in wavefront cleanup. We also report results
of integrated simulation studies of the planet detection performance of
FKSI and results from an in-depth control system and residual optical
pathlength jitter analysis.
---------------------------------------------------------
Title: The Fourier-Kelvin Stellar Interferometer: an achievable,
space-borne interferometer for the direct detection and study of
extrasolar giant planets
Authors: Barry, R. K.; Danchi, W. C.; Deming, L. D.; Richardson,
L. J.; Kuchner, M. J.; Chambers, V. J.; Frey, B. J.; Martino, A. J.;
Rajagopal, J.; Allen, R. J.; Harrington, J. A.; Hyde, T. T.; Johnson,
V. S.; Linfield, R.; Millan-Gabet, R.; Monnier, J. D.; Mundy, L. G.;
Noecker, C.; Seager, S.; Traub, W. A.
2006dies.conf..221B Altcode: 2006IAUCo.200..221B
The Fourier-Kelvin Stellar Interferometer (FKSI) is a mission concept
for a spacecraft-borne imaging and nulling interferometer for the near
to mid-infrared spectral region. FKSI is a scientific and technological
pathfinder to the Darwin and Terrestrial Planet Finder (TPF) missions
and will be a high angular resolution system complementary to the James
Webb Space Telescope (JWST). There are four key scientific issues the
FKSI mission is designed to address. These are: 1.) characterization
of the atmospheres of the known extra-solar giant planets, 2.) assay
of the morphology of debris disks to look for resonant structures
characteristic of the presence of extrasolar planets, 3.) study of
circumstellar material around a variety of stellar types to better
understand their evolutionary state, and in the case of young stellar
systems, their planet forming potential, and 4.) measurement of
detailed structures inside active galactic nuclei. We report results of
simulation studies of the imaging capabilities of the FKSI, current
progress on our nulling testbed, results from control system and
residual jitter analysis, and selection of hollow waveguide fibers
for wavefront cleanup.
---------------------------------------------------------
Title: HD209458b Transit Spectroscopy
Authors: Harrington, J.; Deming, L. D.; Matthews, K.; Richardson,
L. J.; Rojo, P.; Steyert, D.; Wiedemann, G.; Zeehandelaar, D.
2002DPS....34.3005H Altcode: 2002BAAS...34Q.893H
We search for the spectral signature of H<SUB>2</SUB>O, CH<SUB>4</SUB>,
and CO on the extrasolar planet HD 209458b using transit
spectroscopy. The planet will modulate the stellar spectrum during
transit. The extinction altitude of tangent rays of a given wavelength
depends on the abundance and distribution of molecular species that
absorb at that wavelength. The depth of the occultation at a given
wavelength depends on the cross-sectional area of the planet, which is
determined by the extinction altitude. For deep lines of H<SUB>2</SUB>O,
CH<SUB>4</SUB>, and CO, the effect is about 0.07%, due to the ~750
km scale height. Our S/N calculations show that well-calibrated,
ground-based spectra, integrated over time and wavelength, can measure
or place useful limits on the atmospheric abundances of H<SUB>2</SUB>O,
CH<SUB>4</SUB>, and CO. Carbon forms predominantly CH<SUB>4</SUB>
below 1400 K and CO if hotter. Since the effective temperature is
around 1400 K, detecting CH<SUB>4</SUB> and/or CO would provide a tight
constraint on atmospheric temperatures. Observations began in August
2001 at Palomar and we have 12 additional nights granted in 2002 at
Keck, VLT, and IRTF. The expected modulation of the stellar spectrum
is model-dependent: high-altitude hazes, photochemical effects, and
different thermal profiles would substantially modify the effect
for the same planetary elemental abundances. Since the effect is
subtle compared to the noise in the data, we correlate model spectra
against thousands of observed spectra and average the correlations
to test whether the data support a given model. We are developing a
radiative-transfer model to predict the spectrum of a given planetary
model, and we are measuring H<SUB>2</SUB>O, CH<SUB>4</SUB>, and CO in
the laboratory at 1300 K, with pressure-broadening by H<SUB>2</SUB>,
to make our model spectra realistic at these elevated temperatures
(crucial for detecting H<SUB>2</SUB>O). Analysis of the 2001 data and
acquisition of 2002 data are in progress. We solicit participation by
those who wish to test their planetary models.
---------------------------------------------------------
Title: Simple Models of SL-9 Impact Plumes
Authors: Harrington, J.; Deming, L. D.
1996DPS....28.2249H Altcode: 1996BAAS...28.1150H
The impacts of the larger fragments of Comet Shomaker-Levy 9 on Jupiter
left debris patterns of consistent appearance, likely caused by the
landing of the observed impact plumes. Realistic fluid simulations of
impact plume evolution may take months to years for even single computer
runs. To provide guidance for these models and to elucidate the most
basic aspects of the plumes, debris patterns, and their ultimate effect
on the atmosphere, we have developed simple models that reproduce many
of the key features. These Monte-Carlo models divide the plume into
discrete mass elements, assign to them a velocity distribution based
on numerical impact models, and follow their ballistic trajectories
until they hit the planet. If particles go no higher than the observed ~
3,000 km plume heights, they cannot reach the observed crescent pattern
located ~ 10,000 km from the impact sites unless they slide horizontally
after ballistic flight. By introducing parameterized sliding or higher
trajectories, we can reproduce most of the observed impact features,
including the central streak, the crescent, and the ephemeral ring
located ~ 30,000 km from the impact sites. We also keep track of
the amounts of energy and momentum delivered to the atmosphere as a
function of time and location, for use in atmospheric models (D. Deming
and J. Harrington, this meeting).
---------------------------------------------------------
Title: The Bounce of SL-9 Impact Ejecta Plumes on Re-Entry
Authors: Deming, L. D.; Harrington, J.
1996DPS....28.2250D Altcode: 1996BAAS...28.1151D
We have generated synthetic light curves of the re-entry of
SL-9 ejecta plumes into Jupiter's atmosphere and have modeled
the periodic oscillation of the observed R plume light curves
(P. D. Nicholson et al. 1995, Geophys. Res. Lett. 22, 1613--1616) as a
hydrodynamic bounce. Our model is separated into plume and atmospheric
components. The plume portion of the model is a ballistic Monte Carlo
calculation (Harrington and Deming, this meeting). In this paper we
describe the atmospheric portion of the model. The infalling plume
is divided over a spatial grid (in latitude/longitude). The plume is
layered, and joined to a 1-D Lagrangian radiative-hydrodynamic model
of the atmosphere, at each grid point. The radiative-hydrodynamic
code solves the momentum, energy, and radiative transfer equations
for both the infalling plume layers and the underlying atmosphere
using an explicit finite difference scheme. It currently uses gray
opacities for both the plume and the atmosphere, and the calculations
indicate that a much greater opacity is needed for the plume than for
the atmosphere. We compute the emergent infrared intensity at each grid
point, and integrate spatially to yield a synthetic light curve. These
curves exhibit many features in common with observed light curves,
including a rapid rise to maximum light followed by a gradual decline
due to radiative damping. Oscillatory behavior (the “bounce”) is a
persistent feature of the light curves, and is caused by the elastic
nature of the plume impact. In addition to synthetic light curves, the
model also calculates temperature profiles for the jovian atmosphere
as heated by the plume infall.
---------------------------------------------------------
Title: Location of Hydrocarbon Emission Near Jupiter's South Pole
Authors: Livengood, T. A.; Buhl, D.; Deming, L. D.; Espenak, F.;
Kostiuk, T.; Reuter, D.; Fast, K. E.
1993DPS....25.0902L Altcode: 1993BAAS...25.1051L
No abstract at ADS
---------------------------------------------------------
Title: Photometric observations of visual binaries and inferences
concerning mixing in red giants
Authors: Deming, Leo Drake
1976PhDT.......168D Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Photometric Observations of Visual Binaries and Inferences
Concerning Mixing in Red Giants.
Authors: Deming, L. D.
1976PhDT.........2D Altcode:
The DDO and uvby beta methods photometry were used to study a sample
of visual binaries. Inferences were made concerning the amount and
kind of mixing which occurs in population I red giants before and
during the stage of core helium burning. The binaries consist of G
and K giants in association with main sequence stars of nearly solar
type. The DDO photometry of the giant components of the binaries
yields absolute magnitudes which are in generally good accord with
the absolute magnitudes derived for the secondary components from
uvby beta photometry. The spectral types indicated by DDO photometry
are in generally good agreement with spectral types given by visual
classification. However there exists a small group of stars for which
DDO photometry gives widely discrepant spectral types and absolute
magnitudes. These stars can often be noticed to have peculiar spectra
at the time of visual classification; they may be spectroscopic binaries
but this is not certain.
---------------------------------------------------------
Title: a Comparison of Spectrographic and DDO Photoelectric
Luminosities and Composition Indices
Authors: Yoss, Kenneth M.; Deming, L. Drake
1975mpth.conf..359Y Altcode: 1975mpth.proc..359Y
No abstract at ADS
