Photoionization models for the Galactic corona

Details Photoionization models for the Galactic corona Photoionization models for the Galactic corona

Sep 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985apj...296...35f&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 296, Sept. 1, 1985, p. 35-45. Research supported by the Naturvetenskapliga

Astronomy and Astrophysics

Astrophysics

39

Coronas, Galactic Cosmic Rays, Galactic Structure, Gas Density, Photoionization, Active Galaxies, Astronomical Models, Carbon, Density Distribution, Galaxies, Helium, Hydrogen, Interstellar Gas, Iron, Nitrogen, Oxygen, Quasars, Silicon

Scientific paper

A plausible model for gas in the galactic halo is one in which low-density gas is supported by diffusing cosmic rays and is photoionized by extragalactic background radiation. The authors discuss possible sources of ionizing radiation and conclude that the radiation field is dominated by the contribution from quasars and active galaxies. They have calculated a series of models for the galactic corona with a range of characteristic densities and photoionizing fluxes. The elements H, He, C, N, O, Mg, Si, Al, and Fe were included. The observed column density of C IV sets an upper limit to the coronal density of about 2×10-3cm-3. A plausible cosmic ray-supported coronal model approximately reproduces the observed column densities of C IV, Si IV, Si III, and Al III.

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