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Hot Gas in the Galaxy: How Extensive is it?

Published online by Cambridge University Press:  14 August 2015

Frank H. Shu
Frank H. Shu*
Affiliation:
University of California, Berkeley, CA 94720, USA

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Recent satellite detections of 0 VI absorption and soft X-ray emission leave little doubt that, locally, a substantial fraction of the volume of space between interstellar clouds must be filled with rarified and highly ionized gas at temperatures ranging from 2 × 105 to > 106 K. (See the reviews of Spitzer and Jenkins 1975, and Kraushaar 1977.) The physical state of this gas contrasts sharply with the theoretical picture of a largely neutral, warm, intercloud medium at ∼ 104 K developed by Pikel'ner (1967), Field, Goldsmith, and Habing (1969), and Spitzer and Scott (1969). My purpose here is to review the evidence, observational and theoretical, concerning how extensive hot gas at ∼ 106 K might be.

Type
II: Spiral Structure and Star Formation
Information
Symposium - International Astronomical Union , Volume 77: Structure and Properties of Nearby Galaxies , 1978 , pp. 139 - 146
Copyright
Copyright © Reidel 1978 

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