Dynamics of a self-gravitating gas disk in an ovally distorted gravitational potential

Details Dynamics of a self-gravitating gas disk in an ovally distorted gravitational potential Dynamics of a self-gravitating gas disk in an ovally distorted gravitational potential

Jun 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991pasj...43..469f&link_type=abstract

Astronomical Society of Japan, Publications (ISSN 0004-6264), vol. 43, no. 3, 1991, p. 469-484.

Other

19

Galactic Nuclei, Gas Dynamics, Gravitational Fields, Many Body Problem, Accretion Disks, Active Galactic Nuclei, Computerized Simulation, Spiral Galaxies

Scientific paper

The dynamical behavior of a self-gravitating gaseous disk is studied in the central region of a galaxy in response to a fixed, ovally distorted gravitational potential. The gas disk is modeled as an ensemble of inelastically interacting gas clouds and followed using an N-body simulation. To observe the behavior of gas near the center, gas flow within a few turn-over-radii of the rotation curve is simulated. The gas accumulates and forms an oval ring at the turn over radius, where the rotation curves switches from an inner rigid type to another differential type. As the self-gravitation of the gas increases, the ring becomes asymmetric and a large gas clump appears at either end of the major axis of the bar; if the gas mass amounts to more than 10 percent of the total mass, the asymmetry of the flow and gas clumping increases, the gas flow becomes highly unsteady and occasionally the gas passes through the very center of the galaxy, indicating a dynamical inflow of gas to the center. This could provide a fueling mechanism for activities in galactic nuclei.

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