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The structure of the interstellar mediumWe have compared theoretical H I models to a large area H I channel map centered at 1 = 205 deg, b = 0 deg. One set of models were calculated in which uncorrelated clouds of H I populate space. Of the cloud models considered, which include 'Spitzer'-type clouds and the McKee-Ostriker formulation, none were able to reproduce the data successfully. In another class of models, holes and holes with shells permeate an otherwise continuous H I medium. Although not entirely successful, these models contain characteristics that are similar to the data. In order to reproduce the amplitude of the H I variations on angular scales of over 1 deg, the volume occupied by ionized gas must be less than 30 percent, in sharp conflict with the models that suggest that the volume of the ISM is dominated by hot gas.
Document ID
19930035045
Acquisition Source
Legacy CDMS
Document Type
Conference Proceedings
Authors
Bregman, Joel N.
(NASA Headquarters Washington, DC United States)
Ashe, Gregory A.
(Michigan Univ. Ann Arbor, United States)
Date Acquired
August 15, 2013
Publication Date
January 1, 1991
Publication Information
Publication: In: The interstellar disk-halo connection in galaxies (A93-18998 05-90)
Publisher: Kluwer Academic Publishers
Subject Category
Astrophysics
Accession Number
93A19042
Distribution Limits
Public
Copyright
Other

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