Dissipation of thick accretion disks

Details Dissipation of thick accretion disks Dissipation of thick accretion disks

Jun 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983ap%26ss..93..295c&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 93, no. 2, June 1983, p. 295-303.

Astronomy and Astrophysics

Astrophysics

2

Accretion Disks, Astronomical Models, Eddy Viscosity, Energy Dissipation, Magnetohydrodynamic Turbulence, Stellar Mass Accretion, High Reynolds Number, Isentropic Processes, Orbital Mechanics, Solar System, Stellar Evolution

Scientific paper

A thick accretion disk which is isentropic cannot have simple laminar flow because fluid elements follow orbits which intersect the orbits of other fluid elements, leading to turbulence in astrophysical disks which have very large Reynolds numbers. The turbulence in such disks is estimated using molecular analogies for the behavior of the fluid elements. The usual empirical dissipation parameter "α" is found to be equal to 0.25 under normal circumstances. Characteristic local disk parameters are calculated for a variety of conditions at different distances from a central star of one solar mass. Circumstances involving low midplane optical depths or external heating which can lead to large reductions in the turbulence are discussed.

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