Self-gravity and the global structure of accretion discs

Details Self-gravity and the global structure of accretion discs Self-gravity and the global structure of accretion discs

May 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984mnras.208..279a&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 208, May 15, 1984, p. 279-291. Research supported by th

Astronomy and Astrophysics

Astrophysics

27

Accretion Disks, Astrophysics, Gravitational Effects, Topology, Kepler Laws, Nonrelativistic Mechanics

Scientific paper

The global structure of thick, self-gravitating, steady-state accretion discs are examined, emphasizing the effects of disc self-gravity on disc topology and disc dimensions. Inertial and viscous forces are found to be negligible (when viscosity is small) as compared to gravitational, centrifugal and pressure gradient forces. The Keplerian angular momentum is employed as the main variable in the physical effects descriptions. Mass loss mechanisms of various neutral points in the pressure gradient include a new nonrelativistic one related to configurations with large relative disc mass and relative disc central density. Consideration is given to closure conditions for level surfaces, the physical consequences of topological changes as disc self-gravity becomes gradually stronger, and disc dimension sensitivity to self-gravity effects even for small disc mass. It is concluded that astrophysically relevant models of thick accretion discs must consider self-gravity effects to be self-consistent.

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