Statistics – Computation
Scientific paper
Feb 1990
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990arb..nasa..175t&link_type=abstract
In its Annual Research Briefs, 1989 p 175-184 (SEE N92-30149 20-34)
Statistics
Computation
Computational Fluid Dynamics, Computerized Simulation, Mathematical Models, Solar Corona, Solar System Evolution, Turbulence, Turbulent Flow, Astrophysics, Compressibility, Conductive Heat Transfer, Flow Distribution, Navier-Stokes Equation, Planetary Nebulae
Scientific paper
This 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.
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