NASA Logo

NTRS

NTRS - NASA Technical Reports Server

Back to Results
Numerical models of giant planet formation with rotationA 1D quasi-spherical approximation is presently used under the assumption of hydrostatic equilibrium to model giant-planet formation processes that encompass the accretion and transport of angular momentum for both radiative and convective zones. These calculations have been conducted up to masses comparable to those of Saturn. Angular momentum transport is strong, leading to strong concentration of angular momentum in the outer convective zones which develop envelope masses greater than 30 earth masses. When the models are allowed to contract near the calculation's end, the ratio of centrifugal force to gravity at the outer radius rises sufficiently to validate the quasi-spherical approximation.
Document ID
19910063807
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
Authors
Korycansky, D. G.
(NASA Ames Research Center Moffett Field, CA, United States)
Pollack, J. B.
(NASA Ames Research Center Moffett Field, CA, United States)
Bodenheimer, P.
(Lick Observatory Santa Cruz, CA, United States)
Date Acquired
August 14, 2013
Publication Date
August 1, 1991
Publication Information
Publication: Icarus
Volume: 92
ISSN: 0019-1035
Subject Category
Lunar And Planetary Exploration
Accession Number
91A48430
Funding Number(s)
CONTRACT_GRANT: NSF AST-85-21636
Distribution Limits
Public
Copyright
Other

Available Downloads

There are no available downloads for this record.
No Preview Available