The galactic corona

Details The galactic corona The galactic corona

Jan 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979apj...227..398c&link_type=abstract

Astrophysical Journal, Part 1, vol. 227, Jan. 15, 1979, p. 398-406.

Astronomy and Astrophysics

Astrophysics

74

Astronomical Models, Coronas, Galactic Structure, Interstellar Matter, Mass Distribution, Cosmic Rays, Halos, High Temperature Gases, Radiant Cooling, Supernova Remnants

Scientific paper

Models for the galactic corona are studied as a function of mass and energy input. The possible contribution to the galactic halo of hot gas produced by supernovae in the galactic disk is investigated, and various steady-state models for the galactic corona are analyzed under several sets of assumptions concerning the nature of energy gains and losses. Three extreme types of model are proposed, the possible influence of the galactic magnetic field is examined, and implications of cosmic-ray observations are considered. Observational constraints that can be placed on the range of possible models are discussed. It is suggested that mass exchange between the disk and halo at a rate of up to 8 solar masses per year is possible, that the coronal gas density is probably in the range from 0.001 to 0.002 H atom per cu cm, and that the coronal gas temperature is likely to range from 500,000 to 1 million K.

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