Ortho- and para-hydrogen in dense clouds, protoplanets, and planetary atmospheres

Details Ortho- and para-hydrogen in dense clouds, protoplanets, and planetary atmospheres Ortho- and para-hydrogen in dense clouds, protoplanets, and planetary atmospheres

Aug 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978apj...223..854d&link_type=abstract

Astrophysical Journal, Part 1, vol. 223, Aug. 1, 1978, p. 854-858.

Astronomy and Astrophysics

Astrophysics

12

Abundance, Hydrogen Clouds, Interstellar Matter, Planetary Atmospheres, Stellar Evolution, Ion Production Rates, Raman Spectroscopy, Reaction Kinetics, Specific Heat

Scientific paper

If ortho- and para-hydrogen achieve a thermal ratio on dynamical time scales in a molecular hydrogen cloud, then the specific heat is high enough in the temperature range 35-70 K to possibly induce hydrodynamic collapse. The ortho-para ratio in many interstellar cloud fragments is expected to meet this condition. The same may have been true for the primitive solar nebula. Detailed hydrodynamic and hydrostatic calculations are presented that show the effects of the assumed ortho-para ratio on the evolution of Jupiter during its protoplanetary phase. Some possible consequences of a thermalized ortho-para ratio in the atmospheres of the giant planets are also discussed.

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