Formation of a giant Galactic gaseous halo - Metal absorption lines and high-velocity clouds

Details Formation of a giant Galactic gaseous halo - Metal absorption lines and high-velocity clouds Formation of a giant Galactic gaseous halo - Metal absorption lines and high-velocity clouds

May 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...390..405l&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 390, no. 2, May 10, 1992, p. 405-422.

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30

Cooling Flows (Astrophysics), Galactic Structure, Halos, Interstellar Matter, Milky Way Galaxy, Quasars, Absorption Spectra, Abundance, Astronomical Models, Computational Astrophysics, Hydrodynamics, Line Spectra, Metallicity

Scientific paper

A 2D axisymmetric hydrodynamic code based upon the chimney model of the interstellar medium - a new version of a galactic fountain - is used to simulate a Galactic gaseous halo formed through the interstellar disk-halo connection. The abundance of each ion of H, He, and heavy elements is calculated according to the hydrodynamic and thermal state of the halo gas in order to reproduce the column densities of C IV, N V, O VI, and Si IV in the observed absorption lines of halo stars. The distribution and ballistic motions of the clouds in the Galactic gravitational field are calculated on the assumption that the radiatively cooled halo gas condenses into clouds due to thermal instabilities. It is found that a cooled-type halo with gas temperature between 500,000 and 1,000,000 K and density between 0.001 and 0.01/cu cm at the disk-halo interface can reproduce observational facts about the Galaxy. It is concluded that C IV systems greater than 50 kpc correspond to the wind-type halo, and that Mg II and Ca II systems can be detected in a very restricted region (not greater than 20 kpc).

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