Raman scattering in the atmospheres of the major planets

Details Raman scattering in the atmospheres of the major planets Raman scattering in the atmospheres of the major planets

Jan 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978apj...219..756c&link_type=abstract

Astrophysical Journal, Part 1, vol. 219, Jan. 15, 1978, p. 756-762.

Astronomy and Astrophysics

Astrophysics

12

Atmospheric Scattering, Gas Giant Planets, Planetary Atmospheres, Planetary Radiation, Raman Spectra, Absorption Spectra, Atmospheric Attenuation, Methane, Radiative Transfer, Solar Spectra, Atmosphere, Planets, Jupiter, Saturn, Uranus, Neptune, Radiation, Giant Planets, Scattering, Spectra, Reflectivity, Optical Properties

Scientific paper

A technique is developed to calculate the detailed effects of Raman scattering in an inhomogeneous anisotropically scattering atmosphere. The technique is applied to evaluations of Raman scattering by H2 in the atmosphere of the major planets. It is noted that Raman scattering produces an insufficient decrease in the blue and ultraviolet regions to explain the albedos of all planets investigated. For all major planets, the filling-in of solar line cores and the generation of the Raman-shifted ghosts of the Fraunhofer spectrum are observed. With regard to Uranus and Neptune, Raman scattering is seen to exert a major influence on the formation and profile of strong red and near infrared CH4 bands, and Raman scattering by H2 explains the residual intensity in the cores of these bands. Raman scattering by H2 must also be taken into account in the scattering of photons into the cores of saturated absorption bands.

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