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Turbulent transport in the solar nebulaThis paper describes the current state of an ongoing project to simulate turbulent flow in a solar nebula, which is the flattened disk of dust and gas out of which a solar system forms. The goal of this project is to determine a model for the transport of mass and angular momentum in the nebula. The nebula flow exhibits compressibility, thermal conduction, viscosity, internal heating through viscous dissipation, a stable shear due to Keplerian rotation, and a gravitational acceleration in the vertical direction which is linear with altitude. These properties combine to give flow patterns not seen in terrestrial applications. Primordial solar systems are known to exist and are presumably undergoing an evolution similar to the early stages of our own solar system; for example, the IRAS infrared telescope has discovered such a protoplanetary system around the star Vega. Solar nebula evolution is the subject of much research in the astrophysical community. In the long run, researchers hope to gain a better understanding of planetary formation and the processes which dissipate the solar nebula with time.
Document ID
19920020920
Acquisition Source
Legacy CDMS
Document Type
Other
Authors
Thompson, K. W.
(Stanford Univ. CA, United States)
Date Acquired
September 6, 2013
Publication Date
February 1, 1990
Publication Information
Publication: Annual Research Briefs, 1989
Subject Category
Solar Physics
Accession Number
92N30163
Distribution Limits
Public
Copyright
Work of the US Gov. Public Use Permitted.
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