Nature of the coronae of spiral galaxies

Details Nature of the coronae of spiral galaxies Nature of the coronae of spiral galaxies

Mar 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975pazh....1....3k&link_type=abstract

Pis'ma v Astronomicheskii Zhurnal, vol. 1, Mar. 1975, p. 3-7. In Russian.

Astronomy and Astrophysics

Astronomy

10

Coronas, Galactic Structure, Spiral Galaxies, Star Clusters, Andromeda Galaxy, Dwarf Stars, Subdwarf Stars, Ultraviolet Radiation, X Ray Astronomy

Scientific paper

Some concrete limits are placed on the possible nature of the matter constituting the coronae of spiral galaxies, including our own. The hypothesis of Einasto et al. (1974) that such a coronae consists of hot ionized gas is shown to contradict observational data on the soft X-ray background, the soft X-ray flux from M31, and estimates of the UV flux from M31. The hypothesis that the corona may consist of stars (dwarfs or subdwarfs of spectral type M5 or later) is shown to infer that such 'coronal' stars should exist in the vicinity of the sun with a space density of about 0.01 per cu pc and a velocity dispersion of about 300 km/sec. It is noted that this inference can be avoided if the hypothesized coronal stars are concentrated in dwarf clusters or even in dwarf galaxies.

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