The properties of the gas in the galactic halo

Details The properties of the gas in the galactic halo The properties of the gas in the galactic halo

Jan 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986afz....24..123s&link_type=abstract

(Astrofizika, vol. 24, Jan.-Feb. 1986, p. 123-130) Astrophysics (ISSN 0571-7132), vol. 24, no. 1, July 1986, p. 74-78. Translati

Astronomy and Astrophysics

Astronomy

3

Interstellar Chemistry, Interstellar Gas, Milky Way Galaxy, Spaceborne Astronomy, Ultraviolet Radiation, Background Radiation, Carbon, Gas Temperature, Ion Production Rates, Particle Size Distribution, Silicon

Scientific paper

Possible mechanisms are considered by which the ions C IV and Si IV are formed. The absorption lines of these ions are observed in the spectra of stars in the galactic halo at z equal to about 1-3 kpc. It is shown that the observed quantities of these ions may be explained in the model of an absorbing region in the halo with the gas temperature of 10,000 K, the number density of the particles being given by n about equal to or less than 0.01/cu cm, and a dominant role being played by the background ultraviolet radiation in the ionization.

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