Physical state of the galactic-halo gas

Details Physical state of the galactic-halo gas Physical state of the galactic-halo gas

Feb 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988azh....65...25k&link_type=abstract

Astronomicheskii Zhurnal (ISSN 0004-6299), vol. 65, Jan.-Feb. 1988, p. 25-34. In Russian.

Astronomy and Astrophysics

Astronomy

2

Gas Density, Gas Temperature, Intergalactic Media, Interstellar Gas, Electron Scattering, Halos, Ion Distribution, Magnetohydrodynamic Waves, Taylor Instability

Scientific paper

Different mechanisms of the heating of galactic halo gas are considered. It is shown that halo gas cannot be in hydrostatic equilibrium: the models of heating gas by electron heat conduction and by dissipation of Alfvén waves are subject to Rayleigh-Taylor instability, promoting the origin of large-scale convective motions in the hot coronal gas. Such a model in which large-scale motions are realized by upstreaming hot coronal gas and falling clouds, which are produced by convective-thermal instability at the heights ≡1 - 3 kpc, is able to explain the balance of gas, balance of mass and distribution of ions C IV, Si IV, and N V.

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