Secular evolution of isolated barred galaxies. I - Gravitational coupling between stellar bars and interstellar medium

Details Secular evolution of isolated barred galaxies. I - Gravitational coupling between stellar bars and interstellar medium Secular evolution of isolated barred galaxies. I - Gravitational coupling between stellar bars and interstellar medium

Feb 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993a%26a...268...65f&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 268, no. 1, p. 65-85.

Statistics

Computation

275

Barred Galaxies, Galactic Evolution, Gravitational Effects, Interstellar Gas, Angular Momentum, Astronomical Models, Computational Astrophysics, Galactic Nuclei, Star Formation, Three Dimensional Models

Scientific paper

Results from 3D simulations of isolated barred galaxies are presented in which the stellar and gaseous components are modeled in a fully self-consistent way. Significant fueling of galactic nuclei can occur in noninteracting galaxies due to the presence of a nonaxisymmetric potential induced by the bar formation and the work done by this potential on a dissipative gaseous component. Bar-driven fueling of galactic nuclei in noninteracting galaxies is essentially regulated by the dynamic parameters characterizing the simulations. Due to shocks, the cold or warm gaseous component cannot remain on self-crossing trajectories. The gas is sensitive to vertical resonances induced by the bar and can leave the galactic plane to follow 3D orbit families. If the gas is cold or warm, a strong gaseous bar cannot survive without a stellar bar, and the b/a axis ratio of a gaseous bar is always smaller than the one of a stellar bar. The bar pattern speed of collisionless systems decreases with time but the bar pattern speed for systems including a dissipative component can increase. Accretion of large amounts of mass by the central regions leads to destruction of the bar.

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