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Author name code: testerman
ADS astronomy entries on 2022-09-14
author:"Testerman, L."
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Title: Fourier Transform Spectrometer Observations of Solar Carbon
Monoxide. II. Simultaneous Cospatial Measurements of the Fundamental
and First-Overtone Bands, and CA II K, in Quiet and Active Regions
Authors: Ayres, T. R.; Testerman, L.; Brault, J. W.
1986ApJ...304..542A Altcode:
Fourier transform spectrometry has yielded simultaneous cospatial
measurements of important diagnostics of thermal structure in the high
solar photosphere and low chromosphere. It is noted that the anomalous
behavior of the fundamental bands of CO in quiet areas near the limb is
accentuated in an active region plage observed close to the limb. The
difference between the core temperatures of the CO fundamental bands
in a plage and a nearby quiet region at the limb is larger than the
corresponding brightness temperature differences in the inner wings
of the Ca II line measured in a quiet region and several plages
closer to the disk center. Numerical simulations indicate that the
disparate behavior of the CO bands with respect to Ca II K cannot be
reconciled with existing single component thermal structure models;
a two-component atmosphere is required.
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Title: Book-Review - Solar Flux Atlas from 296 TO 1300-NM
Authors: Kurucz, R. L.; Furenlid, I.; Brault, J.; Testerman, L.
1985S&T....70...38K Altcode:
No abstract at ADS
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Title: Solar flux atlas from 296 to 1300 nm
Authors: Kurucz, Robert L.; Furenlid, Ingemar; Brault, James;
Testerman, Larry
1984sfat.book.....K Altcode:
No abstract at ADS
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Title: Absolute oscillator strengths for lines of neutral cobalt
between 2276 A and 9357 A and a redetermination of the solar cobalt
abundance
Authors: Cardon, B. L.; Smith, P. L.; Scalo, J. M.; Testerman, L.;
Whaling, W.
1982ApJ...260..395C Altcode:
Absolute oscillator strengths of neutral cobalt have been
determined from hook measurements for 159 transitions and emission
intensity measurements for 314 transitions between 2276 Å and 9357
Å. Ninety-five of these transitions were subjected to the procedure
developed by Cardon, Smith, and Whaling which fits combined absorption
and emission data to a set of consistent, optimum, relative oscillator
strengths and upper level lifetimes. These relative values were
normalized to the radiative lifetimes of Figger et al. and of Marek
and Vogt obtained by pulsed laser fluorescence. Absolute oscillator
strengths for 362 transitions and 36 lifetimes were determined. Typical
uncertainties in the reported absolute oscillator strengths are ±15-25%
(2/3 confidence level). <P />Equivalent widths were obtained for
nineteen solar cobalt lines with the McMath solar telescope at Kitt
Peak National Observatory. These widths were used to redetermine the
solar cobalt abundance, assuming the photospheric model of Holweger
and a microturbulence velocity of 1.0 km s<SUP>-1</SUP>. The adopted
solar cobalt abundance is the mean value log Co/N<SUB>H</SUB>> + 12 =
4.92 ± 0.08 (±19%), from the 19 cobalt transitions. This value is in
excellent agreement with the solar values of Ross and Aller, of Biemont,
and of Holweger and that of Cameron for carbonaceous chondrites.
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Title: Infrared bands of C2 in the solar photospheric spectrum
Authors: Brault, J. W.; Testerman, L.; Grevesse, N.; Sauval, A. J.;
Delbouille, L.; Roland, G.
1982A&A...108..201B Altcode:
Lines of the C<SUB>2</SUB> Phillips system have been successfully
searched for on new tracings of high resolution solar spectra. From a
rather large number of lines of the (0,0), (1,0), and (0, 1) bands,
we derive empirical values for the band oscillator strengths:
f<SUB>00</SUB> = 1.41 10<SUP>-3</SUP>, f<SUB>10</SUB> = 1.38
10<SUP>-3</SUP>, and f<SUB>01</SUB> = 1.12 10<SUP>-3</SUP>. These
solar f-values are discussed in section 3.1 and compared with recent
laboratory data. <P />For the Ballik-Ramsay system, only a few
unblended solar lines have been available, from which we deduced 0.6
10<SUP>-3</SUP> ≪ f<SUB>00</SUB> ≪ 1.2 10<SUP>-3</SUP>.
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Title: Fourier Transform Spectrometer observations of solar carbon
monoxide. I - The fundamental and first overtone bands in the
quiet sun
Authors: Ayres, T. R.; Testerman, L.
1981ApJ...245.1124A Altcode:
Measurements of the 2200/cm fundamental and 4300/cm first overtone
vibration-rotation band systems of solar carbon monoxide, were obtained
with the Fourier Transform Spectrometer of the McMath telescope at
Kitt Peak. The overtone measurements were taken at the east, north,
and west heliocentric limbs, and at disk center. Observations of the
strong fundamental bands were obtained at disk center and near the
north limb. The low core brightness temperatures of the strongest
fundamental carbon monoxide lines near the limb, reported previously
by Noyes (1972) and Hall (1974), are confirmed. The possibility that
thermal inhomogeneities might be responsible for the unusual behavior of
the fundamental carbon dioxide lines have been examined. The somewhat
discordant behavior of the fundamental lines at disk center compared
with the north limb seems to favor a limb shadowing effect. The
first overtone limb equivalent widths and the best-fit thermal and
microvelocity models indicate a solar carbon abundance of 0.004 (on
the scale with A<SUB>H</SUB> = 1) for an oxygen-to-carbon abundance
ratio of 2.
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Title: Thermal Bifurcation in Solar Calcium Plages
Authors: Ayres, T. R.; Linsky, J. L.; Testerman, L.; Brault, J.
1981BAAS...13..915A Altcode:
No abstract at ADS
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Title: Quadrupole transitions of the 1<-0 band of N<SUB>2</SUB>
observed in a high resolution atmospheric spectrum.
Authors: Camy-Peyret, C.; Flaud, J. -M.; Delbouille, L.; Roland, G.;
Brault, J. W.; Testerman, L.
1981JPhys..42L.279C Altcode:
No abstract at ADS
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Title: Applications of Kitt Peak's One-Meter Fourier Transform
Spectrometer
Authors: Testerman, L.; Hubbard, R.
1980BAAS...12..916T Altcode:
No abstract at ADS
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Title: KPNO FTS Measurements of the Fundamental and First Overtone
Bands of Solar Carbon Monoxide
Authors: Ayers, T. R.; Testerman, L.
1979BAAS...11..732A Altcode:
No abstract at ADS
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Title: Motions in the Atmosphere of Alpha Orionis
Authors: Goldberg, L.; Testerman, L.; Willmarth, D.
1979BAAS...11..682G Altcode:
No abstract at ADS
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Title: The center-to-limb behavior of Ca i λ6573 and [Ca ii] λ7324
Authors: Ayres, T. R.; Testerman, L.
1978SoPh...60...19A Altcode: 1978SoPh...60...19.
Center-to-limb measurements of the Ca I λ6573 intercombination line and
the Ca II λ7324 forbidden line are compared with synthetic profiles
based on a simple representation of the non-LTE Ca-Ca<SUP>+</SUP>
ionization equilibrium. The effects of photoionizations from low
lying excited states of neutral calcium are found to reduce the
sensitivity of the λ6573 center-to-limb behavior as a thermal structure
diagnostic. The synthetic center-to-limb behavior is also sensitive to
uncertainties in the nonthermal broadening. Nevertheless, the measured
center-to-limb behavior of λ6573 favors a `cool' photospheric model
similar to the Vernazza, Avrett, and Loeser model M over hotter models
based on the Ca II K wings. The non-LTE calcium abundance obtained
from the disk center equivalent widths of λ6573 and λ7324 using
the best fit model is A<SUB>Ca</SUB>≅2.1±0.2 × 10<SUP>-6</SUP>
(by number relative to hydrogen). Applications of these lines as
diagnostics of the Ca-Ca<SUP>+</SUP> ionization equilibrium in other
stars are briefly discussed.
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Title: Transition probabilities in Ti I and the solar titanium
abundance.
Authors: Whaling, W.; Scalo, J. M.; Testerman, L.
1977ApJ...212..581W Altcode:
Branching ratios have been measured for 103 lines from 14 levels in
Ti I, and absolute transition probabilities have been determined by
combining these branching ratios with the radiative lifetimes measured
by Roberts, Sorensen, and Andersen (1973) by the beam-foil method. The
solar equivalent width at the disk center has been measured for 23 of
these lines on the preliminary edition of the Kitt Peak Solar Atlas. The
solar Ti abundance has been computed by matching the equivalent widths
of 15 of the weakest lines and by fitting the profiles of 16 lines. The
two methods yield an average photospheric abundance log (N(Ti)/N(H))
+ 12 = 4.98 plus or minus 0.15 based on the HSRA solar model.
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Title: Applications of Fourier analysis to broadening of stellar
line profiles. III. Solar microturbulence and macroturbulence from
iron lines.
Authors: Smith, M. A.; Testerman, L.; Evans, J. C.
1976ApJ...207..308S Altcode:
Kitt Peak solar profiles of iron lines obtained at = 0.63 have been
utilized to study the solar velocity field. The high quality of these
data and the lack of influence of rotation make possible a modeling of
the macroturbulent velocity distribution as well as a determination of
the micro- turbulence. The analysis was performed by matching computed
and observed criteria in both the wavelength and the Fourier transform
domains. The principal ambiguities in evaluating microturbulence are
caused by the uncertainty in the functional form of macroturbulence
and in the value of the atomic damping constants. The form of the first
sidelobe in the data transfbrms indicates the existence of a low (k +
41 km s-1) micro- turbulence at intermediate photo spheric regions which
increases toward larger depths. Attempts were made to fit profiles
with macroturbulences of a wide variety of functional forms. In the
wavelength representation the Voigt distribution gives the best overall
fit, whereas in the transform domain an exponential function matches
the observed sidelobe best. A comparison of all the results (Table 2)
shows only a small disparity in best-fit parameters around a mean of
2.0 km 1 A triangular macrovelocity distribution which is similar to
that predicted by a radial-tangential model is recovered explicitly by
deconvolution. However, for practical reasons a good one-parameter fit
to it is provided by the exponential function. Because this function
is very dissimilar to the rotation function, it should be possible
to evaluate macroturbulence and rotation separately in sharp-lined
late-type stars. Subject headings: line profiles - Sun: atmospheric
motions - Sun: spectra
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Title: The Ability of Current Micro-Velocity Models to Represent
Center-Limb Line Profiles
Authors: Evans, J. C.; Testerman, L.
1975SoPh...45...41E Altcode:
We present results on the ability of microturbulence, LTE line
formation, and a homogeneous thermal model to realistically
represent the center-limb variation of temporally and spacially
averaged solar line profiles. We have used three somewhat similar
semi-empirical thermal models in combination with five current
microturbulence models which cover the gamut of homogeneous-isotropic to
nonhomogeneous-anisotropic. From high resolution photoelectric data for
λ λ5000-6000 at five μ-values (1, 0.63, 0.4, 0.25, 0.16) obtained
at KPNO, we selected 17 Fe I and 5 Fe II line profiles to unblend
and symmetrize for study. An iterative scheme has been developed to
calculate theoretical profiles for the various combination of models and
compare them to the observed profile using the abundance at each limb
position and the magnitude of the pressure broadening at the center
of the disc as parameters. We find that a microturbulence model, for
which the radial and tangential components increase into deeper layers
with ξ<SUB>tan</SUB>>ξ<SUB>rad</SUB>, produces a reasonable good
center-limb fit for lines less than 100 mÅ. However, for lines stronger
than 140 mÅ, microturbulence models with no depth dependence produce
the best match between theory and observation. Thus, there is reason
to question the uniqueness of the microturbulence concept.
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Title: Five-Minute Oscillations of Solar Equivalent Widths
Authors: Holweger, H.; Testerman, L.
1975SoPh...43..271H Altcode:
Equivalent widths of weak and moderately strong Fraunhofer lines
observed in an area roughly 3500 × 10000 km in extent are found
to show small variations of the order of 1 mÅ, on a time scale of
minutes. The dependence of amplitude on line strength and excitation
closely fits that predicted for a compressional disturbance associated
with temperature variations that manifest themselves in the equivalent
widths. The rms amplitude is about 20K near τ<SUB>5000</SUB> =
10<SUP>-2</SUP>.
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Title: Macroturbulence broadening of solar lines with implications
for stellar studies.
Authors: Evans, J. C.; Ramsey, L. W.; Testerman, L.
1975A&A....42..237E Altcode:
This paper reports results of numerical studies of macroturbulence
broadening on solar LTE intensity profiles with a view toward applying
the results toward other solar-type stars. The results are compared
for five different velocity models with spatially and temporally
averaged center-to-limb observations. The comparisons are made through
the curve of the line-width correlation and through the curve of the
line-shape diagram. For mildly saturated lines (about 120 mA), the
solar macrovelocities are the most important of the velocity scale
sizes in determining the shape of the line core. The unsaturated weak
lines and the curve of the line-width correlation do not discriminate
between the two scale sizes of broadening, as suggested by other
studies. High-accuracy photoelectric data for Procyon used in the curve
of the line-shape indicates that macroturbulence broadening dominates
and that the microturbulence component is about 1 km/s.
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Title: High-resolution profiles of sodium and potassium lines in
Alpha Orionis.
Authors: Goldberg, L.; Ramsey, L.; Testerman, L.; Carbon, D.
1975ApJ...199..427G Altcode:
Profiles of the K I resonance line at 7698.98 A and of the D1
and D2 lines of Nai in the spectrum of a Ori have been recorded
photoelectrically using the main beam of the McMath solar telescope
at KPNO. The Na lines were observed in the fourth order of the
spectrograph and the K iline in the third order, providing a resolving
power of approximately 50 mA. The observed profiles are consistent with
a model in which radiation from the stellar photo sphere is scattered
and reemitted by an expanding envelope or envelopes of radius large
compared with that of the photosphere. Each blueshifted absorption
core appears to consist of two components of approximately the same
intensity. The first has a heliocentric radial velocity of + 11-13 km ,
which agrees very well with measurements of other resonance lines by
other observers, whereas the second is in the range + 6 km 1 and appears
not to have been detected previously. Subject headings: circumstellar
shells - late-type stars - stellar winds - stars, individual
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Title: Ni I transition probabilities and the solar nickel abundance.
Authors: Lennard, W. N.; Whaling, W.; Scalo, J. M.; Testerman, L.
1975ApJ...197..517L Altcode:
Absolute transition probabilities have been measured for 97 lines from
11 levels in Ni I using the beam-foil lifetime and branching-ratio
technique. We have measured equivalent widths at the disk center
from the Preliminary Edition of the Kitt Peak Solar Atlas for 49
of the above lines. An empirical solar curve of growth has been
constructed to test the consistency of the transition probabilities
and equivalent widths. The solar Ni abundance has been computed (1)
by matching the equivalent widths of the 10 weakest lines, and (2) by
fitting the profiles of 19 lines. Both methods agree within experimental
uncertainty and yield an average photospheric Ni abundance of 6.28 +
0.09. Subject headings: abundances, solar - transition probabilities
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Title: High Resolution Profiles of Sodium and Potassium Lines in
α Orionis.
Authors: Goldberg, L.; Ramsey, L.; Testerman, L.; Carbon, D.
1975BAAS....7..233G Altcode:
No abstract at ADS
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Title: An Abundance Analysis by Center and Limb Profile Fitting
Authors: Testerman, Larry
1974BAAS....6R.295T Altcode:
No abstract at ADS
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Title: Center-Limb Velocity Broadened Profiles.
Authors: Testerman, L. K.; Evans, J. C.
1973BAAS....5..445T Altcode:
No abstract at ADS
