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Hot gas in and between galaxies

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Abstract

The fate of interstellar gas heated by energetic radiation and far from the galactic plane is considered. It is shown that for plausible heating rates a very hot corona forms, separated from the cooler gas in the disk by a conductive boundary layer. For heating rates exceeding a critical value a galactic wind is set up, as first shown by Mathews and Baker for elliptical galaxies. Such winds may fill the intracluster space in clusters of galaxies; further heating may drive a cluster wind, as shown by Yahil and Ostriker. It is believed that the flow problem of intracluster gas in the presence of intercluster gas is not yet adequately solved. A variety of observations at X-ray and ultraviolet wavelengths are needed to resolve these questions.

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Authors and Affiliations

  1. Center for Astrophysics, Harvard College Observatory and Smithsonian Astrophysical Observatory, Cambridge, Mass., USA

    George B. Field

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  1. George B. Field
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Field, G.B. Hot gas in and between galaxies. Astrophys Space Sci 38, 167–190 (1975). https://doi.org/10.1007/BF00646105

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  • DOI: https://doi.org/10.1007/BF00646105

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