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Ortho- and para-hydrogen in dense clouds, protoplanets, and planetary atmospheresIf 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.
Document ID
19780061630
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Decampli, W. M.
(NASA Ames Research Center Moffett Field, CA, United States)
Cameron, A. G. W.
(Harvard College Observatory and Smithsonian Astrophysical Observatory, Center for Astrophysics, Cambridge Mass., United States)
Bodenheimer, P.
(Lick Observatory Santa Cruz, Calif., United States)
Black, D. C.
(NASA Ames Research Center Space Sciences Div., Moffett Field, Calif., United States)
Date Acquired
August 9, 2013
Publication Date
August 1, 1978
Publication Information
Publication: Astrophysical Journal
Subject Category
Astrophysics
Accession Number
78A45539
Funding Number(s)
CONTRACT_GRANT: NSF AST-76-17590
CONTRACT_GRANT: NSF AST-76-81572
CONTRACT_GRANT: NGR-22-007-269
CONTRACT_GRANT: NCA2-OR660-703
Distribution Limits
Public
Copyright
Other

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