Viscous evolution of self-gravitating galactic disks within a dark halo

Details Viscous evolution of self-gravitating galactic disks within a dark halo Viscous evolution of self-gravitating galactic disks within a dark halo

Nov 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...363...40s&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 363, Nov. 1, 1990, p. 40-49.

Statistics

Computation

41

Computational Astrophysics, Galactic Evolution, Galactic Structure, Gravitational Effects, Galactic Bulge, Galactic Rotation, Star Formation, Viscosity

Scientific paper

Viscous evolution of thin and star-forming galactic disks within a massive dark halo is investigated by taking into account the self-gravity. It is assumed that the well-known gravitational instability of a self-gravitating disk generates turbulence (as well as star formation). The disk is assumed to be in nearly centrifugal equilibrium under the action of viscosity, just like an accretion disk. Such a disk is found to be unstable to spatial oscillations of physical variables owing to the action of viscosity and self-gravity in the inner part of the disk where rotation is nearly uniform. Exponential distributions of the surface density of the stars are produced as a result of viscous evolution with star formation. Moreover, it is found that the viscous evolution creates flat rotation curves extending from the outer part where dark halo dominates to the inner part where self-gravity dominates, just as observations indicate.

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