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The disk-halo connection and the nature of the interstellar mediumSome results on the nature of the interstellar medium that are specifically concerned with the disk-halo interaction are discussed. Over the last five years or so it has become clear that the supernovae rate in our Galaxy is spatially clumped and the consequences of such clumping are superbubbles and supershells fed by tens or hundreds of supernovae per shell. These objects evolve and expand rapidly and soon break out of the disk of the Galaxy, feeding the halo with very significant mass, energy, and momentum. As cooling occurs, gas will rain down onto the disk of the Galaxy completing the cycle. The basic flow of physical quantities from disk to halo and vice versa are discussed. Some of the many implications are noted including aspects of dynamo theory, quasar absorption lines, the theory of galactic coronae, and the nature of the x ray background. The essential difference here with the McKee-Ostriker (1977) theory is that the filling factor of the hot gas in the disk is significantly less than unity.
Document ID
19900006544
Acquisition Source
Legacy CDMS
Document Type
Preprint (Draft being sent to journal)
Authors
Norman, Colin A. (Space Telescope Science Inst. Baltimore, MD, United States)
Ikeuchi, Satoru (Tokyo Astronomical Observatory)
Date Acquired
September 6, 2013
Publication Date
January 1, 1988
Subject Category
Astronomy
Report/Patent Number
NASA-CR-186286
PREPRINT-SERIES-232
NAS 1.26:186286
Accession Number
90N15860
Distribution Limits
Public
Copyright
Work of the US Gov. Public Use Permitted.

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