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Author name code: schneeberger
ADS astronomy entries on 2022-09-14
author:"Schneeberger, Timothy J."
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Title: Limits on line-of-site jitter derived from image resolution
requirements
Authors: Schneeberger, Timothy J.
1994SPIE.2221..704S Altcode:
Requirements for image resolution can be used to set upper limits on
the allowable line-of-site (LOS) motion of an acquisition, tracking,
and pointing (ATP) system. Image resolution is important for image-based
tracking algorithms and for typical ancillary requirements for target
phenomenology data gathering. During the system design phase of an
ATP platform, base-motion- disturbance details such as total rms
power and spectral distribution of this power may not be known for
primary disturbance sources such a gimbals, cooling systems, and
steering mirrors. In this case, setting upper limits to allowable
LOS jitter is an important criteria in the trade study analyses for
these components. The effect of jitter is frequency dependent and
can be partitioned into regimes based on the image sample rate of the
system. The application of image-resolution requirements for the High
Altitude Balloon Experiment are used to set allowable LOS motion for
random, sinusoidal, and linear disturbances. Three frequency regimes are
identified with different allowable-motion amplitudes. This top-level
systems methodology can be applied to many imaging applications such as
estimating the blur induced by wind loading of ground based telescopes.
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Title: Image Recovery and Pattern Recognition Applications in a
Visual Language Environment
Authors: Schneeberger, Timothy; Pierson, Robert; Dayton, Dave;
Gonglewski, John D.
1992ASPC...25..140S Altcode: 1992adass...1..140S
Khoros is a software system which implements a visual programming
language. It uses graphical icons and pipeline data flow to simplify
the development and testing of new signal and image processing
algorithms. We briefly describe two different applications developed
under Khoros: one in pattern recognition, the other in astronomical
imaging.
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Title: Integrated image processing and tracker performance prediction
workstation
Authors: Schneeberger, Timothy J.; McIntire, Harold D.
1991SPIE.1567....2S Altcode:
Extensive research has shown that including target aspect angle
measurements from an optical sensor can significantly improve the
performance of radar tracking systems. Integrating sequences of
target imagery with the kinematic information involves sets of
image processing and sensor data fusion algorithms. A workstation
has been developed to expedite the analysis of the algorithms and to
integrate the image processing with selectable extended-state tracker
modules. This workstation can access analog video imagery from a video
optical disk controlled by a PC, segment the target in the image,
and perform target identification and aspect angle estimation using a
database of target models which span the range of possible aspects. The
angle information is then `fused' with kinematic data to augment the
tracker state estimator. The workstation is implemented with a powerful
visual user interface in a UNIX/X- Windows environment, and includes
a wide array of image and signal processing algorithms. Interactive
modifications of processing sequences and `what if' analyses are easily
conducted. The workstation provides a consistent user interface across
a variety of applications. This system has also been used to implement
phase retrieval and related image recovery algorithms.
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Title: Spatial frequency selective error sensing for space-based,
wide field-of-view, multiple-aperture imaging systems
Authors: Erteza, Ahmed; Schneeberger, Timothy J.
1991SPIE.1527..182E Altcode:
High-resolution space-based imaging applications are limited by
the difficulty of placing large monolithic mirrors in space and
by technology limitations on the diameter achievable in monolithic
mirrors. Multiple-mirror imaging systems can overcome these limitations
but require precise alignment-error sensing and correcting schemes to
maintain all elements in phase. When a wide field of view is desired,
the complexity increases substantially since significant error terms
will be a function of field angle. Approaches which can reduce the
complexity of the error sensing/correcting schemes are thus of great
interest. By sampling selected spatial frequencies, representative
of both the individual subapertures and errors between subapertures,
measurement of all error terms except absolute piston can be achieved. A
technique which places a nonredundant mask in the compacted pupil plane
of a phased-array imager and senses the selected spatial-frequency
magnitude and phase in the focal plane has been analyzed. This technique
can reduce complexity in the local error-sensing system while accounting
for all tilt, geometry, magnification, and relative piston errors.
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Title: The response of chromospheric emission lines to flares on YZ
Canis Minoris.
Authors: Worden, S. P.; Schneeberger, T. J.; Giampapa, M. S.; Deluca,
E. E.; Cram, L. E.
1984ApJ...276..270W Altcode:
Six flares of the dMe star YZ CMi have been observed with simultaneous
photometry and high-dispersion, time-resolved spectroscopy.The spectra
have temporal resolutions of 3 minutes with spectral resolutions
of 0.24 Å. The largest observed flare had a U band amplitude of
1.5 mag. Hα and Hβ line profiles did not broaden during any of the
observed flares, although the line center intensity increased by over a
factor of 2 during some flares. After the initial increase in intensity,
the emission line strength decreases but remains at enhanced levels
for hours following U band flares. The Hα flare luminosity and total
energy are compared to corresponding properties of solar flares.
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Title: Using small aperture interferometry to detect planets in
nearby binary star systems
Authors: Currie, D. G.; McAlister, H. A.; Schneeberger, T. J.; Worden,
S. P.
1983STIN...8331551C Altcode:
If suitably accurate binary star orbits can be observed, the effects of
planets in the binary star system may be detectable in the reflex motion
of the component binary stars. We show that interferometric measurements
of binary star systems will provide this information. We discuss the
effects of the atmosphere on degrading images and how interferometry
will remove these effects to provide very accurate binary star positions
relative to the other components in the binary system. Two systems,
amplitude interferometry and speckle interferometry, can accomplish
this using existing telescopes and techniques. With these methods,
nearly accuracies of 0.00002 arc second are possible for binaries of 1
arc second separation and 10000 arc second for a 5 arc binary. These
accuracies are more than enough to detect planets in orbits like
Jupiter's out to over 20 pc. There are 188 observable systems within
20 pc, in most of which it is possible to have stable planetary orbits
similar to solar system orbits. With advanced data recording systems it
is possible to observe binary systems where the components are as faint
as +16 stellar magnitudes. A dedicated 2-meter interferometric telescope
to monitor binary stars could be built for about 1.4 million dollars.
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Title: Cloudcroft occultation summary .I. December 1978-March 1980.
Authors: Radick, R. R.; Africano, J. L.; Rogers, W. F.; Schneeberger,
T. J.; Tyson, E. T.
1982AJ.....87..885R Altcode:
Results are presented from the first 16 months of a program undertaken
to record lunar occultations at Cloudcroft Observatory. The 85 events
summarized include 38 observations of stars brighter than seventh
magnitude, 26 reappearances, nine angular diameter measurements,
and 11 observations of binary stars or stars which may be double.
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Title: Coordinated X-ray, optical and radio observations of flaring
activityon YZ Canis Minoris.
Authors: Kahler, S.; Golub, L.; Harnden, F. R.; Liller, W.; Seward,
F.; Vaiana, G.; Lovell, B.; Davis, R. J.; Spencer, R. E.; Whitehouse,
D. R.; Feldman, P. A.; Viner, M. R.; Leslie, B.; Kahn, S. M.; Mason,
K. O.; Davis, M. M.; Crannell, C. J.; Hobbs, R. W.; Schneeberger,
T. J.; Worden, S. P.; Schommer, R. A.; Vogt, S. S.; Pettersen, B. R.;
Coleman, G. D.; Karpen, J. T.; Giampapa, M. S.; Hege, E. K.; Pazzani,
V.; Rodono, M.; Romeo, G.; Chugainov, P. F.
1982ApJ...252..239K Altcode:
The YZ Canis Minoris (Gliese 285), a late-type dwarf star with
Balmer emission (dM4.5e), is a member of the UV Ceti class of flare
stars. Obtaining good X-ray observations of a dMe star flare is
important not only for understanding the physics of flares but also for
testing current ideas regarding the similarity between stellar and solar
flares. The Einstein X-ray Observatory has made it possible to conduct
X-ray observations of dMe stars with unprecedented sensitivity. A
description is presented of the results of a program of ground-based
optical and radio observations of YZ CMi coordinated with those of
the Einstein Observatory. The observations were carried out as part
of a coordinated program on October 25, 26, and 27, 1979, when YZ CMi
was on the dawn side of the earth. Comprehensive observational data
were obtained of an event detected in all three wavelength regions on
October 25, 1979.
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Title: High-resolution profiles of chromospheric lines in M dwarf
stars.
Authors: Worden, S. P.; Schneeberger, T. J.; Giampapa, M. S.
1981ApJS...46..159W Altcode:
Forty-six hydrogen and sodium line profiles are presented for 17
selected dwarf M and dwarf M emission line stars. These profiles,
derived from echelle spectrograms, typically have 0.25 A spectral
resolution. Most of the dMe stars show hydrogen emission lines with
central reversals. Central emission features in the cores of the Na D
lines are often observed, and the presence of these emission features
is strongly correlated with hydrogen line emission.
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Title: Stellar model chromospheres. XII. High-resolution, absolute
flux profiles of the CaII H and K lines in dMe and non-dMe stars.
Authors: Giampapa, M. S.; Worden, S. P.; Schneeberger, T. J.; Cram,
L. E.
1981ApJ...246..502G Altcode:
We present 142 mÅ resolution spectra of the cores and wings of the
Ca II H and K lines in three dMe and four comparison dwarf M stars,
obtained with the KPNO 4 m echelle spectrograph and blue image
tube. The narrow-band photometry of Willstrop and the Barnes and
Evans relations for stellar angular diameters convert the observed
relative flux to absolute surface flux units with an estimated
uncertainty of ± 15 %. We derive chromospheric radiative loss rates
in the H and K lines and discuss trends in these loss rates with
effective temperature. Monochromatic surface fluxes are tabulated for
different features in the H and K lines, and radiation temperatures
are derived from the mean surface fluxes at K<SUB>1</SUB> and
H<SUB>1</SUB>, respectively. We find T<SUB>R</SUB>(H<SUB>1</SUB>) >
T<SUB>R</SUB>(K<SUB>1</SUB>), consistent with partial redistribution
theory. The T<SUB>R</SUB>(K<SUB>1</SUB>)/T<SUB>eff</SUB> ratio
is higher in these M dwarfs than the giants studied in Paper X,
and it is anomalously high for the dMe flare star YZ CMi. If
T<SUB>R</SUB>(K<SUB>1</SUB>)/T<SUB>eff</SUB> is an empirical age
indicator, then the result for YZ CMi implies that flare activity
and youth are directly correlated, as has been suggested by other
investigators. Moreover, the result implies that a high degree of
nonradiative heating is present in the upper photospheres of dMe
stars. Measurements of line widths at H<SUB>1</SUB> and K<SUB>1</SUB>
are presented together with FWHM data for the H and K lines. We find
that the scaling law proposed by Ayres generally agrees with the
observed trend exhibited by the K<SUB>1</SUB> widths. We also discuss
chromospheric radiative loss rates in the Hɛ line compared with loss
rates in the H and K lines, and present corrected FWHM(K) widths and
compare them to the widths predicted by the Wilson-Bappu relation as
calibrated by Lutz.
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Title: Flare activity on T Tau stars.
Authors: Worden, S. P.; Schneeberger, T. J.; Kuhn, J. R.; Africano,
J. L.
1981ApJ...244..520W Altcode:
Observations of short-period photometric fluctuations in T Tauri
stars show flarelike events. These events are consistent with the
superposition of many solar-like flare events and have a power-spectrum
frequency dependence of ∼f<SUP>-2</SUP>. This dependence is the same
as that observed on UV Ceti stars. The flare events are very powerful,
and the expected proton flux from these events may explain early solar
system abundance anomalies without recourse to nearby supernovae. The
flare events are consistent with the observations of mass loss in
these stars.
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Title: Observational Astronomy at the Cloudcroft Observatory
Authors: Schneeberger, Timothy J.; Worden, S. P.
1980srca.conf...67S Altcode:
No abstract at ADS
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Title: Cloudcroft Observatory Today
Authors: Schneeberger, Timothy J.; Worden, S. P.; Africano, J. L.;
Tyson, E.
1980S&T....59..109S Altcode:
No abstract at ADS
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Title: New Photometric Observations of EX Hydrae
Authors: Africano, J. L.; Quigley, R.; Schneeberger, T. J.; Worden,
S. P.
1979BAAS...11..649A Altcode:
No abstract at ADS
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Title: Observations of Coronal Oscillations above an Active Region
Authors: Egan, T. F.; Schneeberger, T. J.
1979SoPh...64..223E Altcode:
Periodic Doppler width fluctuations have been observed in Fe XIV spectra
above an active region. The oscillations have a period of 6.1 ± 0.6
min and a peak-to-peak amplitude of 0.07 ± 0.006 Å. The amplitude of
the oscillation increases with height above the limb, and is enhanced
at specific heights where we marginally detect line center intensity
oscillations. The intensity fluctuations have a period of 6.1 min,
an amplitude of 2.0 ± 1.4%, and are 180 ° out of phase with the
width oscillations. A comparison region in the quiet corona showed no
evidence of oscillatory phenomena.
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Title: Flare Activity on T Tauri Stars
Authors: Schneeberger, T. J.; Worden, S. P.; Kuhn, F. R.; Africano,
J. L.
1979BAAS...11..628S Altcode:
No abstract at ADS
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Title: High Resolution Spectra of Stellar Flares
Authors: Worden, S. P.; Schneeberger, T. J.; Deluca, E.; Giampapa, M.
1979BAAS...11..628W Altcode:
No abstract at ADS
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Title: The Ca II H and K Lines in dMe and non-dMe Stars
Authors: Giampapa, M. S.; Worden, S. P.; Schneeberger, T. J.; Cram,
L. E.
1979BAAS...11..625G Altcode:
No abstract at ADS
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Title: High-resolution line profiles of T Tau stars.
Authors: Schneeberger, T. J.; Worden, S. P.; Wilkerson, M. S.
1979ApJS...41..369S Altcode:
Thirty-three relative intensity hydrogen and sodium line profiles
obtained from spectra of 10 T Tauri stars are presented. These profiles
were derived from echelle spectrograms having a typical resolution of
0.20 A. The T Tauri stars observed span the range of emission-intensity
classes listed in Herbig and Rao (1972). Seventy percent of the H alpha
profiles show blue-displaced absorption components with velocities up to
250 km/sec. Na D emission features are observed in all the stars with
emission-intensity classes higher than 2. The Na D lines in T Tauri
show intensity changes on a time scale of months. The H alpha-line
equivalent width in T Tauri can change by 40% in 3 days.
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Title: The lifetimes of sunspot moats.
Authors: Pardon, L.; Worden, S. P.; Schneeberger, T. J.
1979SoPh...63..247P Altcode:
Daily full disk magnetograms observed with the Kitt Peak 40 channel
magnetograph have been examined for the rise time, decay time and
lifetime of sunspot moats. Eighteen well defined moats result in rise
and decay times of 0.5d ± 1d, with a lifetime at maximum development
of 6d ± 3d. The moat appears approximately 3 days after the spot is
observed in our data.
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Title: The night sky conditions at the Sacramento Peak
Observatory. I. Sky brightness.
Authors: Schneeberger, T. J.; Worden, S. P.; Beckers, J. M.
1979PASP...91..530S Altcode:
The night sky brightness at Sacramento Peak Observatory has been
monitored over a period of nine months. The average zenith sky is 21.9
± 0.1 m<SUB>υ</SUB> arc sec<SUP>-2</SUP>. The night sky brightness
shows fluctuations of up to 25% during this period. The long record
of daytime sky-brightness observations shows a strong seasonal effect
with brightest skies occurring in the early summer months. This seasonal
effect is marginally present in the night sky brightness results. Light
pollution from the closest urban areas is also detailed.
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Title: Chromospheric emission lines in the red spectrum of AD
Leonis. II. Physical conditions in flares.
Authors: Schneeberger, T. J.; Linsky, J. L.; McClintock, W.; Worden,
S. P.
1979ApJ...231..148S Altcode:
Simultaneous photometry and time-resolved spectra of the dMe flare star
AD Leo has been used to deduce flare temperatures, electron densities,
and dimensions. Photometric results for two qualitatively different
flares yield estimates of the differences in physical properties
between these flares. Flares on AD Leo are hotter and denser than their
solar counterparts, and spike-like flares occupy smaller volumes than
longer-lived flares. An upper limit to the flare X-ray luminosity is
set atL <4 x l028ergss-1. Subject headings: stars: chromospheres -
stars: emission-line - stars: flare - stars: individual
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Title: Short Time Scale Brightness Fluctuations in BP Tauri
Authors: Schneeberger, T. J.; Worden, S. P.; Africano, J. L.
1979IBVS.1582....1S Altcode:
No abstract at ADS
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Title: Short Time Scale Brightness Fluctuations in T Tauri Stars.
Authors: Schneeberger, T. J.; Worden, S. P.; Africano, J. L.
1979BAAS...11..439S Altcode:
No abstract at ADS
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Title: Period Variation of UX Ursae Majoris in 1979
Authors: Quigley, R.; Africano, J. L.; Schneeberger, T. J.; Worden,
S. P.
1979BAAS...11..445Q Altcode:
No abstract at ADS
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Title: The Cloudcroft Observatory 48 inch telescope.
Authors: Africano, J. L.; Schneeberger, T. J.; Worden, S. P.
1979BAAS...11..392A Altcode:
No abstract at ADS
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Title: Chromospheric emission lines in the red spectrum of AD
Leonis. I. The nonflare spectrum.
Authors: Giampapa, M. S.; Linsky, J. L.; Schneeberger, T. J.; Worden,
S. P.
1978ApJ...226..144G Altcode:
High-resolution red (5300-7300 A) spectra of the flare star AD Leonis
were obtained with the Kitt Peak 4 m echelle spectrograph system
at a spectral resolution of 0.22 A at Ha. A series of time-trailed
plates with 5 hours integration in total were averaged together
to obtain a representation of the star's nonflaring spectrum with
high signal-to-noise ratio. The He i A5876 triplet line and A6678
singlet line appear in emission with measured equivalent widths of
0.312 + 0.016 A and 0.058 + 0.029 A, respectively. The corresponding
triplet-to-singlet line flux ratio is 3.7, close to the ratio of the
level statistical weights. We argue that the He i lines are not produced
by recombination and cascade following photoionization by A < 504
A coronal photons, but are instead collisionally excited. We suggest
that these lines are formed in a geometrically thin chromospheric layer
at 20,000-50,000 K with a column density of nel 6 x 1018 . The sodium
D emission lines (A5890, AS 896) are found to be stellar in origin,
with measured FWHM of 0.7 A for both lines, and the Ha line has a
FWHM of 1.4 A. No other chromospheric emission lines were found in
this spectral region. Subject headings: stars: chromospheres - stars:
emission-line - stars: flare - stars: individual
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Title: The Spectrum of T Tauri Star BM AND.
Authors: Schneeberger, T. J.
1978BAAS...10Q.453S Altcode:
No abstract at ADS
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Title: Problems in the Interpretation of Cluster Membership
Probabilities
Authors: McNamara, B. J.; Schneeberger, T. J.
1978A&A....62..449M Altcode:
Summary. The degree to which the combination of proper motions of
various accuracies and deleting from the vector point diagram influences
computed cluster membership probabilities using the maximum likelihood
technique as employed by Sanders (1971) is investigated. Results
obtained from the recently published proper motion data for M 11
suggest that both of these effects can have a significant influence on
the calculated membership probabilities. Key words: galactic clusters
membership probabilities
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Title: The helium triplet-to-singlet ratio in T Tauri stars.
Authors: Schneeberger, T. J.; Linsky, J. L.; Worden, S. P.
1978A&A....62..447S Altcode:
Summary. The He ilines at 5876 and 6678 are used to determine the
triplet-to-singlet ratio for T Tauri stars DF Tau and BP Tau. The
ratio is approximately 3. Line profiles and absolute intensities are
presented. Key words: T Tauri stars helium lines
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Title: Balmer emission lines in T Tauri-like decelerating flows
Authors: Schneeberger, Timothy James
1978PhDT.......334S Altcode:
No abstract at ADS
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Title: Balmer Line Profiles in Decelerating Atomsphere
Authors: Schneeberger, Timothy J.; Beebe, H. A.
1978srca.conf...69S Altcode:
No abstract at ADS
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Title: Balmer Emission Lines in T Tauri-Like Decelerating Flows.
Authors: Schneeberger, T. J.
1978PhDT.........1S Altcode:
The star and envelope properties are chosen to approximate T Tauri
star conditions. The Sobolev approximation is used to solve the
radiative transfer problem in the envelope and the application of this
technique to decelerating atmospheres is discussed. A ten-level model
hydrogen atom including forty-five line transitions is utilized and
the effects of changes in the adopted collisional cross sections and
recombination rates are determined. The details of the solutions of
the hydrogen level populations are presented for a range of envelope
conditions. The effects of changes in the effective temperature of the
central star, the electron temperature of the envelope, the stellar mass
loss ratio and the initial flow velocity in the decelerating envelope
are discussed. The Balmer line profiles are computed by integrations
along surfaces of equal line of sight velocity. Changes in emission
line strengths and shapes and the behavior of the Balmer decrement
were determined for a range of envelope conditions.
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Title: Chromospheric Emission Lines in the Quiescent Spectrum of
the Flare Star AD Leo
Authors: Giampapa, M. S.; Linsky, J. L.; Schneeberger, T. J.; Worden,
S. P.
1977BAAS....9..593G Altcode:
No abstract at ADS
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Title: Simultaneous Photometry and Time Resolved Spectra of Flare
Star AD Leo
Authors: Schneeberger, T. J.; Worden, S. P.; Linsky, J. L.;
McClintock, W.
1977BAAS....9Q.593S Altcode:
No abstract at ADS
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Title: Alfvén waves in the corona above sunspots.
Authors: Beckers, J. M.; Schneeberger, T. J.
1977ApJ...215..356B Altcode:
From the line width in coronal arches above sunspots it is possible to
estimate the amount of Alfven wave flux escaping from the spot into the
solar corona. It is found to be less than 4 x 10 to the 7th ergs/sq
cm/s in the corona just above the spot, which is less than 0.08%
of the missing spot flux. If the Alfven-wave cooling mechanism for
spots is to be valid, these waves have therefore to escape downward
into the solar interior.
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Title: Balmer line profiles in decelerating atmospheres.
Authors: Schneeberger, T. J.; Beebe, H. A.
1977srca.conf...69S Altcode:
No abstract at ADS
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Title: Nova Vulpeculae 1976
Authors: Neff, J. S.; Smith, V. V.; Ketelsen, D. A.; Osawa, K.; Dawson,
D.; Schneeberger, T.; Roemer, T.; Solomon, S.; Whitney, C. A.; Schmidt,
T. E.; Maley, P.; Bortle, J.
1976IAUC.3001....1N Altcode:
J. S. Neff, Department of Physics and Astronomy, University of Iowa,
reports further monochromatic magnitudes, obtained with the assistance
of V. V. Smith and D. A. Ketelsen: Oct. 29.04 UT, 7.8; Nov. 1.02,
6.8. These monochromatic magnitudes, which refer to a wavelength
of 5500 A (not 6500 A, as was stated on IAUC 3000), are derived by
comparison of the continuum intensity in a 30-A band centered at
this wavelength in the spectra of the nova and the star 7 Vul, the
magnitude of the latter being assumed equal to its V magnitude of
6.3. On Oct. 29 and Nov 1 the peak flux of H-beta had increased to
some three times that of the adjacent continuum. On the latter date,
several other emission features were detected, including H-gamma,
H-delta, H-epsilon (and/or Ca II) and evidently Fe II and Ti II
lines. The following photoelectric magnitudes have been reported:
1976 UT V B - V U - B Observer Oct. 22.46 7.02 +1.29 Osawa 22.49 7.07
+1.38 +1.00 " 22.51 7.11 +1.44 +1.06 " 24.068 7.29 +1.40 +0.39 Dawson
26.094 6.87 +1.18 +0.40 Schneeberger 25.153 7.33 +1.27 +0.23 Roemer
& Solomon 29.052 7.03 +1.14 Whitney K. Osawa (Tokyo Astronomical
Observatory, Okayama Station). D. Dawson, T. Schneeberger, T. Roemer
and S. Solomon (New Mexico State University). Several reference stars
used. 61-cm reflector, Tortugas Station, and 91-cm reflector, Blue
Mesa Station. C. A. Whitney (Harvard College Observatory, Agassiz
Station). 40-cm reflector. Comparison star BD +20 4179 (assumed V =
7.29, B-V = +0.26). Delta-U (nova - comparison) = +0.51. Selected
visual magnitude estimates: Oct. 30.06 UT, 7.1 (T. E. Schmidt, Tiara
Observatory); 31.05, 7.3 (P. Maley, Houston, Texas); Nov. 1.06, 6.8
(Schmidt); 2.01, 7.0 (J. Bortle, Brooks Observatory).
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Title: Non-LTE profiles of strong solar lines
Authors: Schneeberger, T. J.; Beebe, H. A.
1976CONMS...1..110S Altcode: 1976conm....1..110S
The complete linearization method is applied to the formation of
strong lines in the solar atmosphere. Transitions in Na(I), Mg(I),
Ca(I), Mg(II), and Ca(II) are computed with a standard atmosphere and
microturbulent velocity model. The computed profiles are compared to
observations at disk center.
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Title: Emissivities and detectability of the pure rotational
transitions of molecular hydrogen
Authors: Schneeberger, T. J.
1976CONMS...1..123S Altcode: 1976conm....1..123S
The emissivities of the infrared rotational transitions of H2 are
calculated for temperatures from 10 K to 6000 K. The calculations
are made for several ratios, R, of Para (J=0) to Ortho (J=1)H2. The
possibility of detecting these transitions in interstellar molecular
clouds is discussed.
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Title: Non-LTE profiles of strong solar lines.
Authors: Schneeberger, T. J.; Beebe, H. A.
1976CNMSU...1..110S Altcode:
No abstract at ADS
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Title: Emissivities and detectability of the pure rotational
transitions of molecular hydrogen.
Authors: Schneeberger, T. J.
1976CNMSU...1..123S Altcode:
No abstract at ADS
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Title: Nova Cygni 1975
Authors: Strittmatter, P. A.; Fawley, W.; Schommer, R.; Deeter,
J.; Wallerstein, G.; Tedesco, E. F.; Herzog, A.; Schneeberger, T.;
Sherrod, C.; di Cicco, D.; Jacchia, L.
1975IAUC.2830....1S Altcode:
The following photoelectric magnitudes have been reported: 1975 UT V B
- V U - B V - R R - I b - y Observer Aug. 30.3 1.98 +0.51 -0.81 +0.57
+0.15 Strittmatter 30.40 2.01 +0.40 Fawley 30.52 2.02 " 31.25 1.92 +0.64
-0.11 Schommer 31.3 1.87 +0.62 -0.65 +0.82 +0.21 Strittmatter 31.33 1.90
+0.64 +0.02 Tedesco 31.51 2.02 +0.65 -0.15 Schommer Sept. 1.3 2.26 +0.55
-0.69 +1.03 +0.20 Strittmatter 1.31 2.61 +0.49 -0.21 Tedesco 1.47 2.80
+0.49 -0.40 Schommer 2.18 3.73 +0.34 -0.52 " 2.19 3.96 +0.38 Fawley
2.32 4.19 +0.35 " 2.38 4.24 +0.34 " 2.47 4.02 +0.31 -0.54 Schommer
P. A. Strittmatter et al. (University of Arizona). W. Fawley (University
of California, Berkeley). R. Schommer and J. Deeter (University of
Washington). From the extremely rapid decline G. Wallerstein deduces M_v
= -9.2. E. F. Tedesco, A. Herzog, T. Schneeberger and G.Garwood(New
Mexico State University). Comparison star epsilon Cyg. Errors ~
+/- 0.02. The following recent visual magnitude estimates have been
reported: Sept. 3.07, 4.2 (C. Sherrod, North Little Rock, Arkansas);
3.10, 3.7 (D. di Cicco, Waltham, Massachusetts); 3.21, 4.8 (Sherrod);
4.07, 4.8 (L. Jacchia, Cambridge, Massachusetts); 4.08, 4.9 (Sherrod);
4.10, 4.7 (di Cicco).
---------------------------------------------------------
Title: Spatial Inhomogeneities in the Cores of Strong Lines in the
Solar Spectrum.
Authors: Schneeberger, T. J.; Beebe, H. A.
1975BAAS....7..448S Altcode:
No abstract at ADS
