Gas flow in a two component galactic disk

Details Gas flow in a two component galactic disk Gas flow in a two component galactic disk

Jun 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994ap%26ss.216..347n&link_type=abstract

Astrophysics and Space Science, vol. 216, no. 1-2, p. 347-351

Astronomy and Astrophysics

Astrophysics

1

Galactic Evolution, Galactic Halos, Gas Dynamics, Gas Flow, Gravitational Fields, Interstellar Gas, Magnetohydrodynamic Flow, Stellar Envelopes, Stellar Gravitation, Stellar Models, Galactic Mass, Gravitation Theory

Scientific paper

Numerical simulations of two-component (stars + gas) self-gravitating galactic disks show that the interstellar gas can significantly affect the dynamical evolution of the disk even if its mass fraction (relative to the total galaxy mass) is as low as several percent. Aided by efficient energy dissipation, the gas becomes gravitationally unstable on local scale and forms massive clumps. Gravitational scattering of stars by these clumps leads to suppression of bar instability usually seen in heavy stellar disks. In this case, gas inflow towards the galactic center is driven by dynamical friction which gas clumps suffer instead of bar forcing.

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