Pressure‐induced absorption in the infrared: A data base for the modelling of planetary atmospheres

Abstract

Recent progress related to the modeling of various pressure‐induced absorption bands of binary molecular systems, involving dissimilar and like pairs of molecules such as H2, He, N2, CH4, etc., is reported. The notes include references to the existing efforts based on quantum line shape computations that reproduce the laboratory measurements of pressure‐induced absorption closely. The results may be considered a most reliable data base permitting an evaluation of pressure‐induced absorption as function of frequency, temperature, and gas density for various binary molecular systems and spectral bands in the infrared region of the spectrum.

The Nitrogen Isotopic Ratio in Jupiter’s Atmosphere from Observations by the Composite Infrared Spectrometer on theCassiniSpacecraft

“…The molecular spectral data employed in the radiative transfer calculations are from the recent GEISA (Jacquinet-Husson et al 1999) and HITRAN (Rothman et al 1998) compilations. The collision-induced absorptions for H 2 , He, and CH 4 pairs have been incorporated by using the model provided by Borysow et al (1985), Borysow & Frommhold (1991), and Birnbaum, Borysow, & Orton (1996).…”

Thermal Structure of Uranus' Atmosphere

“…The pressure-induced opacity within each homogeneous atmospheric layer represents true continuum absorption and within each spectral interval can be characterized by a single monochromatic absorption coefficient following Beer's law. Absorption coefficients were calculated from routines kindly supplied by Borysow (Borysow and Frommhold 1991).…”

Radiative Balance and Dynamics in the Stratosphere of Jupiter: Results from a Latitude-Dependent Aerosol Heating Model

“…9. While these comparisons are made here for homogetemperature conditions pertaining to the jovian atmo- absorption coefficients generated from computer codes by Borysow for the rototranslational bands (see Borysow et al 1985, Borysow andFrommhold 1991). The hydrogen To find the radiative equilibrium temperature, we concoefficients depend on the ortho-para ratio.…”