Equilibrium structure of self-gravitating Keplerian disks

Details Equilibrium structure of self-gravitating Keplerian disks Equilibrium structure of self-gravitating Keplerian disks

May 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995a%26a...297..135h&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 297, no. 1, p. 135-140

Astronomy and Astrophysics

Astrophysics

11

Accretion Disks, Equilibrium, Gravitational Effects, Stellar Gravitation, Stellar Models, Stellar Rotation, Hydrodynamics, Protostars, Stellar Mass, Two Dimensional Models

Scientific paper

We present two-dimensional equilibrium models of realistic, self-gravitating Keplerian disks of arbitrary thickness surrounding a gravitating central object (star), which is approximated by a point mass. The point mass and the disk mass of the computed models are in solar units (0.6, 0.39), (0.6, 1.4), (1.4, 0.006), (1.4, 0.011), (3.5, 0.29) amd (10.0, 0.28), respectively. The configuration consisting of a central star of 0.6 solar mass and a surrounding disk of 0.39 solar mass is similar to that obtained in the two-dimensional hydrodynamical calcualtion of Bodenheimer et al. (1991). This shows that we are able to construct equilibirum disk models, which approximate quasi-equilibirum evolutionary stages of accretion disks encountered during proto-star formation. Equilibrium models with a more massive central object, e.g. the (3.5 solar mass, 0.29 solar mass) model system, can be considered as describing a black hole surrounded by a thick disk, i.e. being representative of systems like SS 433.

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