Brillouin scattering in liquids excited by the he-ne maser.
Brillouin scattering in liquids excited by He-Ne maser and observed by Fabry-Perot interferometer, noting acoustic wave velocity and line broadening
ACOUSTIC VELOCITY↗
SEARCH · Engineering Papers
Results for “LINE WIDTHS”
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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The uv lines of fe xiv in the solar corona.
Relative line strengths of UV lines of Fe XIV CALCULATED for solar corona
CORONA↗
Correlation of the orbach relaxation coefficient with optical linewidths - laf sub 3-er super 3 super plus.
Excited state lifetime equivalence to Orbach relaxation coefficient correlated with optical linewidths of trivalent erbium doped lanthanum fluoride
EXCITED STATE↗
Electron Impact Broadening of Isolated Ion Lines
Electron impact broadening of isolated ion spectral lines
SPECTRAL LINE WIDTH↗
Spectroscopy with gas lasers.
Optical- and IR-maser spectroscopy of inhomogeneously broadened resonances, using gas lasers
INFRARED MASER↗
Observations of circularly polarized OH EMISSION and narrow spectral features.
OH emission and narrow spectral features made with circularly polarized field horn on 140-ft radio telescope in November 1965
GALACTIC RADIO WAVE↗
On the interpretation of the line spectra of quasi-stellar objects.
Electron scattering interpretation of ionization, emission and absorption line spectra of quasi- stellar object
ELECTRON SCATTERING↗
Electron-impact broadening of isolated ion lines.
Discrepancies in electron-impact broadening of isolated ion lines due to neglect of collision- induced transitions between upper and lower levels of line and Coulomb interactions with perturbed ions
COULOMB COLLISION↗
A solar iron abundance determination using lines in the near UV
Solar iron abundance determination using lines in near ultraviolet
SPECTRAL LINE WIDTH↗
Spectral-Line Profiles for a Fast-Ion-Beam Source
Exact expression for line profile of stigmatic spectrograph without vignetting, noting results with foil-excited ions as light source
SPECTRAL LINE WIDTH↗
Millidegree noise thermometry.
Millidegree noise thermometry based on linewidth of Josephson radiation
JOSEPHSON CURRENT↗
Surface-gravity determinations for main-sequence B stars
Astronomical models for computing surface gravity of B stars from hydrogen line equivalent widths
Peterson, D. M.↗
Surface-gravity determinations for main- sequence B stars.
Main sequence B stars surface gravity determinations from comparison between model atmosphere computed and observed H gamma line equivalent widths
Peterson, D. M.↗
Infrared absorptance of carbon monoxide at low temperatures.
IR absorptance of CO below room temperature, determining strength and half widths of lines in R branch of fundamental band
Hoover, G. M.↗
Studies of methane absorption in the Jovian atmosphere. I.
Methane rotational temperature in Jovian atmosphere deduced from equivalent widths of lines at 1.1 micron band
Fox, K.↗
High dispersion observations of Venus during 1972. The CO2 band at 7820 angstrom
Photographic plates of Venus which show the spectrum of the carbon dioxide band at 7820A were obtained at Table Mountain Observatory in September-October 1972. These spectra showed a semi-regular 4-day variation in the CO2 abundance over the disk of the planet. Evidence for temporal variations in the rotational temperature of this band and temperature variations over the disk was found. The two quantities, CO2 abundance and temperature, do not show any obvious relationship; however, an increase in the temperature usually is accompanied by a decrease in the abundance of CO2. The average temperature, found from a curve of growth analysis assuming a constant CO2 line of width, is 249 plus or minus 1.4 K (one standard deviation).
Young, L. D. G.↗
High-dispersion spectroscopic observations of Venus during 1968 and 1969. II - The carbon-dioxide band at 8689 A
Results are reported for an extensive series of high-resolution spectroscopic observations of the CO2 band at 8689 A in the atmosphere of Venus which were made over a period of one year at a dispersion of 2 A/mm for Venus phase angles varying from 10 to 126 deg. The equivalent widths of lines in the band are measured, the rotational temperature is calculated, and the CO2 abundance over various areas on the planet is determined. The results are compared with those of previous observations of the CO2 bands at 8689, 7820, and 7883 A, and good agreement is found regarding the temperatures and abundances derived for the different bands. It is concluded that the CO2 abundance varies over the planet and that its distribution does not remain constant with time.
Schorn, R. A. J.↗
Observations of Lorentzian lines with slits of finite widths
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Sulzmann, K. G. P.↗