Thermal evaporation of gas within galaxies by a hot intergalactic medium

Details Thermal evaporation of gas within galaxies by a hot intergalactic medium Thermal evaporation of gas within galaxies by a hot intergalactic medium

Apr 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977natur.266..501c&link_type=abstract

Nature, vol. 266, Apr. 7, 1977, p. 501-503. NASA-supported research.

Astronomy and Astrophysics

Astronomy

192

Evaporation, High Temperature Gases, Intergalactic Media, Astronomical Models, Emission Spectra, Galactic Structure, Mass Transfer, Oblate Spheroids, Prolate Spheroids, Symmetry

Scientific paper

High-temperature (about 100 million K) intergalactic gas interacts with cooler embedded gas within galaxies and extragalactic clouds principally by thermal evaporation. From Cowie and McKee's (1977) model for evaporation of spherical interstellar clouds in pressure balance with a hot ambient medium, solutions are obtained for oblate and prolate spheroidal symmetry. The results are applied to evaporation of gases within spiral and elliptical galaxies, and can be extended to evaporation of filamentary clouds in the interstellar medium.

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