Author name code: testerman ADS astronomy entries on 2022-09-14 author:"Testerman, L." ------------------------------------------------------------------------ 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. Bibcode: 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. Title: Book-Review - Solar Flux Atlas from 296 TO 1300-NM Authors: Kurucz, R. L.; Furenlid, I.; Brault, J.; Testerman, L. Bibcode: 1985S&T....70...38K Altcode: No abstract at ADS Title: Solar flux atlas from 296 to 1300 nm Authors: Kurucz, Robert L.; Furenlid, Ingemar; Brault, James; Testerman, Larry Bibcode: 1984sfat.book.....K Altcode: No abstract at ADS 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. Bibcode: 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).

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-1. The adopted solar cobalt abundance is the mean value log Co/NH> + 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. 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. Bibcode: 1982A&A...108..201B Altcode: Lines of the C2 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: f00 = 1.41 10-3, f10 = 1.38 10-3, and f01 = 1.12 10-3. These solar f-values are discussed in section 3.1 and compared with recent laboratory data.

For the Ballik-Ramsay system, only a few unblended solar lines have been available, from which we deduced 0.6 10-3 ≪ f00 ≪ 1.2 10-3. 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. Bibcode: 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 AH = 1) for an oxygen-to-carbon abundance ratio of 2. Title: Thermal Bifurcation in Solar Calcium Plages Authors: Ayres, T. R.; Linsky, J. L.; Testerman, L.; Brault, J. Bibcode: 1981BAAS...13..915A Altcode: No abstract at ADS Title: Quadrupole transitions of the 1<-0 band of N2 observed in a high resolution atmospheric spectrum. Authors: Camy-Peyret, C.; Flaud, J. -M.; Delbouille, L.; Roland, G.; Brault, J. W.; Testerman, L. Bibcode: 1981JPhys..42L.279C Altcode: No abstract at ADS Title: Applications of Kitt Peak's One-Meter Fourier Transform Spectrometer Authors: Testerman, L.; Hubbard, R. Bibcode: 1980BAAS...12..916T Altcode: No abstract at ADS Title: KPNO FTS Measurements of the Fundamental and First Overtone Bands of Solar Carbon Monoxide Authors: Ayers, T. R.; Testerman, L. Bibcode: 1979BAAS...11..732A Altcode: No abstract at ADS Title: Motions in the Atmosphere of Alpha Orionis Authors: Goldberg, L.; Testerman, L.; Willmarth, D. Bibcode: 1979BAAS...11..682G Altcode: No abstract at ADS Title: The center-to-limb behavior of Ca i λ6573 and [Ca ii] λ7324 Authors: Ayres, T. R.; Testerman, L. Bibcode: 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+ 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 ACa≅2.1±0.2 × 10-6 (by number relative to hydrogen). Applications of these lines as diagnostics of the Ca-Ca+ ionization equilibrium in other stars are briefly discussed. Title: Transition probabilities in Ti I and the solar titanium abundance. Authors: Whaling, W.; Scalo, J. M.; Testerman, L. Bibcode: 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. 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. Bibcode: 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 Title: The Ability of Current Micro-Velocity Models to Represent Center-Limb Line Profiles Authors: Evans, J. C.; Testerman, L. Bibcode: 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 ξtan>ξrad, 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. Title: Five-Minute Oscillations of Solar Equivalent Widths Authors: Holweger, H.; Testerman, L. Bibcode: 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 τ5000 = 10-2. Title: Macroturbulence broadening of solar lines with implications for stellar studies. Authors: Evans, J. C.; Ramsey, L. W.; Testerman, L. Bibcode: 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. Title: High-resolution profiles of sodium and potassium lines in Alpha Orionis. Authors: Goldberg, L.; Ramsey, L.; Testerman, L.; Carbon, D. Bibcode: 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 Title: Ni I transition probabilities and the solar nickel abundance. Authors: Lennard, W. N.; Whaling, W.; Scalo, J. M.; Testerman, L. Bibcode: 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 Title: High Resolution Profiles of Sodium and Potassium Lines in α Orionis. Authors: Goldberg, L.; Ramsey, L.; Testerman, L.; Carbon, D. Bibcode: 1975BAAS....7..233G Altcode: No abstract at ADS Title: An Abundance Analysis by Center and Limb Profile Fitting Authors: Testerman, Larry Bibcode: 1974BAAS....6R.295T Altcode: No abstract at ADS Title: Center-Limb Velocity Broadened Profiles. Authors: Testerman, L. K.; Evans, J. C. Bibcode: 1973BAAS....5..445T Altcode: No abstract at ADS