Possible Derivations of Ortho- and Para-H2 Ratios in the Atmospheres of the Giant Planets Using the 2 μ m Spectral Structures of (H2)2

Details Possible Derivations of Ortho- and Para-H2 Ratios in the Atmospheres of the Giant Planets Using the 2 μ m Spectral Structures of (H2)2 Possible Derivations of Ortho- and Para-H2 Ratios in the Atmospheres of the Giant Planets Using the 2 μ m Spectral Structures of (H2)2

Nov 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001jass...18...95k&link_type=abstract

Journal of Astronomy and Space Science, vol. 18, no. 2, p. 95-100

Astronomy and Astrophysics

Astronomy

Planet, Atmosphere, Molecule, Radiative Transfer, Spectroscopy

Scientific paper

We have presented an ab \ initio model of the 2 μ m spectral features of (H2)2 based on the far-infrared models of McKellar & Schaefer (1991). We have shown that the intensity variations of the 2 μ m (H2)2 features depend on the ortho/para ratios of H2. We have discussed the applicability of the variations to the atmospheres of the giant planets for the derivations of the ortho/para ratios. The signal to noise ratios of currently available spectra of the giant planets are not sufficient enough to derive accurate ortho/para ratios of these planets. Observations with longer exposure times and larger telescope apertures are required to obtain better spectra for the derivations of the ortho/para ratios of H2 in the atmospheres of the giant planets.

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