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Photodissociation and the Morphology of HI in Galaxies

Ronald J. Allen
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Abstract

Young massive stars produce Far-UV photons which dissociate the molecular gas on the surfaces of their parent molecular clouds. Of the many dissociation products which result from this ``back-reaction'', atomic hydrogen \HI is one of the easiest to observe through its radio 21-cm hyperfine line emission. In this paper I first review the physics of this process and describe a simplified model which has been developed to permit an approximate computation of the column density of photodissociated \HI which appears on the surfaces of molecular clouds. I then review several features of the \HI morphology of galaxies on a variety of length scales and describe how photodissociation might account for some of these observations. Finally, I discuss several consequences which follow if this view of the origin of HI in galaxies continues to be successful.

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Ronald J. Allen. 2004-06-30. Photodissociation and the Morphology of HI in Galaxies. https://doi.org/10.1007/978-1-4020-2862-5_63

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