Dynamical Behavior of Gaseous Halo in a Disk Galaxy

Details Dynamical Behavior of Gaseous Halo in a Disk Galaxy Dynamical Behavior of Gaseous Halo in a Disk Galaxy

Dec 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980pthph..64.1995h&link_type=abstract

Progress of Theoretical Physics, Vol. 64, No. 6, pp. 1995-2008

Physics

60

Scientific paper

Assuming that the gas in the halo of a disk galaxy is supplied from the disk as a hot gas, we have studied its dynamical and thermal behavior by means of a time dependent, two-dimensional hydrodynamic code. Depending upon the temperature and density of the gas at the disk, three types of gaseous halo are formed, that is, a wind-type, a bound-type and a cooled-type halo. In the former two cases, the hot gaseous halo with the temperature higher than 3 × 105 K is formed, and the X-ray emission of the luminosity 1037 ˜ 1039 ergs/ s is expected in 0.3 ˜ 4 keV region. In the cooled-type halo, the halo gas collapses to the disk plane after a rapid radiative cooling, and this will be observed as infalling, high-velocity clouds. Some discussions on the role of gaseous halo for a disk galaxy are given.

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