A galactic disk as a two-fluid system - Consequences for the critical stellar velocity dispersion and the formation of condensations in the gas

Details A galactic disk as a two-fluid system - Consequences for the critical stellar velocity dispersion and the formation of condensations in the gas A galactic disk as a two-fluid system - Consequences for the critical stellar velocity dispersion and the formation of condensations in the gas

Jan 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984apj...276..127j&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 276, Jan. 1, 1984, p. 127-134.

Astronomy and Astrophysics

Astrophysics

86

Disk Galaxies, Gravitational Collapse, Interstellar Gas, Milky Way Galaxy, Molecular Clouds, Two Fluid Models, Galactic Structure, Gas Density, Radial Velocity, Spiral Galaxies, Stellar Motions, Systems Stability

Scientific paper

The consequences of treating a galactic disk as a two-fluid system for the stability of the entire disk and form of the gas in the disk are examined. It is found that the existence of even a small fraction of the total disk surface density in a cold fluid makes it much harder to stabilize the entire two-fluid disk. At the higher effective gas densities resulting from the growth of a two-fluid instability, the gas may become unstable even when it is itself originally stable. The wavelength of a typical gas instability in the inner galaxy is about 400 pc, and it contains about 10 million solar masses of interstellar matter; these instabilities may be identified with clusters of giant molecular clouds. It is suggested that many of the spiral features seen in gas-rich spiral galaxies may be material arms or arm segments resulting from sheared two-fluid gravitational instabilities.

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