Band model analysis of the H2O2 /nu/6/b/ band
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Goorvitch, D.↗
Engineering topics
Silvaggio, P. M.
Publications and source records attributed to Silvaggio, P. M..
The use of intermolecular potential functions in fitting pressure induced spectra
An example is presented which demonstrates the importance of using physically realistic derivatives of the intermolecular potential when fitting pressure-induced spectra. The use of nonrealistic derivatives may mask second-order temperature effects in the theory. As the temperature decreases, the intermolecular potential may have an important angular dependence.
Goorvitch, D.↗
Investigation of the 2-0 pressure-induced vibrational absorption spectrum of hydrogen at temperatures below ambient
A theoretical fit has been made to our laboratory measurements of the 2-0 collisionally induced H2 absorption band for temperatures of 122 and 273.3 K and at a density of 20 amagats. A Lennard-Jones 6-12 intermolecular potential and a Birnbaum-Cohen line profile have been used. The fit resulted in a chi-square of 0.2%. Line widths have also been derived as a function of temperature. The lifetimes of the states have been calculated.
Silvaggio, P. M.↗
Investigation of the 1-0 pressure-induced vibrational absorption spectrum of hydrogen at temperatures below ambient
A theoretical fit has been made to laboratory measurements of the 1-0 collisionally induced H2 absorption band over a temperature range of 100-273 K and for densities up to 22 amagats. Both the Birnbaum-Cohen and the MacTaggert-Hunt line shape profiles were used. In addition, an intermolecular potential of either a Lennard-Jones 6-12 or a Morse-spline-van der Waals has been used for each line shape. The best fit resulted in a chi-square of 5%. Line widths have also been derived as a function of temperature. The lifetimes of the states were calculated.
Goorvitch, D.↗
Intensity of the sulfur dioxide rotational spectrum
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Larkin, R. J.↗
Temperature dependence of intensities of the 8-12 micron bands of CFCl3
The absolute intensities of the 8-12 micron bands from Freon 11 (CFCl3) were measured at temperatures of 294 and 216 K. Intensities of the bands centered at 798, 847, 934, and 1082 per cm are all observed to depend on temperature. The temperature dependence for the 847 and 1082 per cm fundamental regions is attributed to underlying hot bands; for the nu2 + nu5 combination band (934 per cm), the observed temperature dependence is in close agreement with theoretical prediction. The implication of these results on atmospheric IR remote-sensing is briefly discussed.
Nanes, R.↗
Band model calculations for CFCl3 in the 8-12 micron region
A Goody random band model with a Voigt line profile is used to calculate the band absorption of CFCl3 at various pressures at room and stratospheric (216 K) temperatures. Absorption coefficients and line spacings are computed.
Silvaggio, P. M.↗
The surface and atmosphere of Pluto
A new spectrum of Pluto in the region 1.4 to 1.9 microns provides confirmation of the presence of solid methane on the planet's surface. Considerations of the vapor pressure of methane gas above the solid indicate the presence of a tenuous atmosphere of this gas, the surface partial pressure of which is variable from perihelion to aphelion. The implication of a high surface albedo, the newly derived mass of Pluto, and inferences as to the range of plausible bulk mean densities indicate that the radius of Pluto should lie in the range 1200 to 1800 km.
Cruikshank, D. P.↗
Infrared methane spectra between 1120 per cm and 1800 per cm - A new atlas
A new atlas of CH4 lines in the 1120-1800-per cm region has been generated, based on laboratory spectra taken with a Nicolet interferometer at 0.06-per cm resolution with 635-cm path length at pressures of 0.98 torr, 4.86 torr, and 19.97 torr. A compilation of line positions and line intensities includes 1339 CH4 lines, several hundred of which have not been previously observed.
Blatherwick, R. D.↗
Triton - A satellite with an atmosphere
A low-resolution infrared spectrum of Triton in the region 1.4-2.6 microns shows a broad absorption at 2.3 microns which is attributed to gaseous methane. The computed surface partial pressure of CH4, based on a random band model extrapolation of new laboratory spectra, is (1 + or - 0.5) times 10 to the -4th bars, a value consistent with the calculated vapor pressure of methane gas above methane ice at the expected temperature of Triton. There is, however, no compelling evidence for the presence of solid CH4 on the satellite's surface.
Cruikshank, D. P.↗
First results from the large probe infrared radiometer experiment
During the descent to the surface of Venus, the large probe infrared radiometer measured the net thermal radiative flux in several spectral bandpasses. Preliminary analysis has permitted us to estimate (1) the infrared extinction coefficient profile attributable to aerosols, with respect to their visible profile, in the upper atmosphere of Venus and (2) the water vapor mixing ratio below the clouds. An indication of the composition of a multicomponent cloud is seen in the data from the spectral bandpass from 6 to 7 micrometers.
Boese, R. W.↗
On the CH4 nu-4 fundamental controversy - Line-intensity measurements revisited
Because of the controversy over the value of the band strength for the nu-4 fundamental of CH4, equivalent widths of the R(0), R(1), and P(11, 11, F1) lines have been measured to compare with opposing views. The present measurements are consistent with the band strength of Ko and Varanasi (1977), who, on the basis of high-resolution line-strength measurements, propose an integrated band strength of 145 kaysers/(cm-am).
Lutz, B. L.↗
A new atlas of infrared methane spectra between 1120 per cm and 1800 per cm
An atlas of 1339 methane absorption lines in the range 1120 to 1800 reciprocal centimeters, including the nu(4) and nu(2) bands, is presented. Laboratory spectra were obtained by a Nicolet Fourier transform Michelson interferometer with a resolution of approximately 0.06 reciprocal cm and a path length of 6.35 m of 0.98, 4.86 and 19.97 torr. Observed spectra are also compared with spectral intensities calculated line-by-line on the basis of tabulated intensities of the observed spectral lines.
Blatherwick, R. D.↗