Theoretical line profiles in the ultraviolet spectra of early-type stars.
Theoretical line profiles in UV spectra of two early B stars from 911.6 to 3000 angstroms
STELLAR SPECTRUM↗
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Search indexed NASA NTRS and DOE OSTI research on propulsion, heat transfer, battery materials and energy systems. Follow report and document links to the original sources.
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A study of the green TiO band in the sunspot spectrum.
Sunspot spectra green TiO equivalent line widths measured on high dispersion spectrogram, obtaining rotational temperature
Makita, M.↗
Analysis of F and G subdwarfs. III - An abundance analysis of the subdwarf mu Cassiopeia.
Model atmosphere abundance analysis of subdwarf mu Cassiopeia by measuring spectral line widths and comparing with sun
Cohen, J. G.↗
Electron-spin memory in the optical-pumping cycle of F centers in alkali halides and electron-spin resonance of the relaxed excited state.
Electron spin memory in optical pumping cycle of potassium halides F centers, measuring relaxed excited state g factors and spin resonance line widths
Mollenauer, L. F.↗
Studies of methane absorption in the Jovian atmosphere. II
Methane abundance in Jovian atmosphere deduced from line equivalent widths, obtaining line intensity for J manifolds
Fox, K.↗
Properties of axicon systems for collecting foil-excited accelerator beam spectra
Axicon systems for spectroscopy of light emitted by foil-excited accelerator beams, discussing scattering contribution to spectral line widths
Stoner, J. O., Jr.↗
Deconvolution of Fabry-Perot profiles
Diagram extracting Lorentzian line widths from Fabry-Perot interferometer profiles
Day, R. A.↗
Pressure-broadened linewidths in the electric- field-induced spectrum of H2
Pressure broadened line widths in electric field induced fundamental hydrogen spectral band, noting linear variation with density
Barnes, W. L.↗
Absorption coefficients of O2 at the Lyman- alpha line and of other O2 transmission windows
Oxygen absorption coefficients at Lyman alpha line and other transmission windows, verifying dependence on pressure source line width and doublet separation
Ogawa, M.↗
Criteria for the discovery of beta Cephei stars according to the mu-mechanism theory
Beta Cephei star discovery criteria, examining mu-mechanism theory by He and N overabundances, far UV flux, spectral line width and binary character
Simon, N. R.↗
Improving laser beam coherence - A concept
Laser frequencies may be reduced to single frequency or selected frequencies. For single frequency performance, spacing of frequencies falls in natural line width. For two or more frequencies, thicker spacing is used. Configuration adapts to operation with Kerr or Pockel cell for Q switching.
Heflinger, L. O.↗
Observation of CO emission at 2.6 millimeters from IRC plus 10216
IR object IRC plus 10216 carbon monoxide emission at 2.6 mm, noting spectral line width, thermal emission and mass
Jefferts, K. B.↗
The 5520 A band of ammonia in the spectrum of Jupiter
Equivalent line widths of 5520 A ammonia band in Jupiter spectrum
Owen, T.↗
An electron paramagnetic resonance study of hydrogen atoms trapped in gamma-irradiated calcium phosphates
Hydrogen atoms trapped in gamma irradiated calcium phosphates, studying radiation yields, electron paramagnetic resonance line widths, dose saturation and relaxation
Virmani, Y. P.↗
Laboratory measurement of the 6-centimeter formaldehyde transitions
Formaldehyde transitions in ground and excited states at 6 cm, attaining line widths and hyperfine structure at 1-3 kHz
Thaddeus, P.↗
Automated analysis of astronomical spectra
Automated analysis of high resolution IR astronomical spectra by computer program, presenting procedures for spectral line width, depth and frequency determination
Hutchison, R. B.↗
Interpolation constants for calculation of transmittance and rate of dissociation of molecular oxygen in the mesosphere and lower thermosphere
Values of band oscillator strengths and rotational line widths for the Schumann-Runge band system have been used to derive interpolation constants from which the transmittance and rate of dissociation of molecular oxygen can be calculated. These constants, valid for temperatures between 150 and 300 K and for column densities between 1 x 10 to the 17th power/cm sq and 7 x 10 to the 24th power/cm sq, cover the wavelength range 1750 and 2050A.
Hudson, R. D.↗
Photodissociation rates of molecular oxygen in the mesosphere and lower thermosphere.
Use of recently obtained band oscillator strengths and predissociation line widths, for the Schumann-Runge band system to calculate the photodissociation rate of molecular oxygen as a function of column density and temperature by solar radiation between 1025 and 2500 A. Data are presented from which the mean transmission and photodissociation rates for given wavelength intervals between 1750 and 2025 A can be calculated for column densities between 10 to the 17th and 10 to the 23rd molecules/sq cm and for temperatures between 150 and 300 K. Also, the production of vibrationally excited oxygen molecules as a result of fluorescence in the Schumann-Runge bands is discussed.
Hudson, R. D.↗