Protostellar disks and the primitive solar nebula

Details Protostellar disks and the primitive solar nebula Protostellar disks and the primitive solar nebula

May 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987pggp.rept...97c&link_type=abstract

In NASA, Washington, Reports of Planetary Geology and Geophysics Program, 1986 p 97-99 (SEE N87-23341 16-91)

Statistics

Computation

Computational Fluid Dynamics, Cosmology, Gravitational Effects, Nebulae, Protostars, Stellar Mass Accretion, Angular Momentum, Energy Spectra, Energy Transfer, Mass Transfer

Scientific paper

The objective is to obtain quantitative information on the turbulent transport of mass, angular momentum, and energy under the conditions that characterize the solar nebula, by direct numerical calculations. These calculations were made possible by research conducted on supercomputers (Cray XMP and Cray 2) by the Ames Computational Fluid Dynamics Branch. Techniques were developed that permitted the accurate representation of turbulent flows over the full range of important eddy sizes. So far, these techniques were applied (and verified) primarily in mundane laboratory situations, but they have a strong potential for astrophysical applications. A sequence of numerical experiments were conducted to evaluate the Reynold's stress tensor, turbulent heat transfer rate, turbulent dissipation rate, and turbulent kinetic energy spectrum, as functions of position, for conditions relevant to the solar nebula. Emphasis is placed on the variation of these properties with appropriate nondimensional quantities, so that relations can be derived that will be useful for disk modeling under a variety of hypotheses and initial conditions.

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