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The Structure of the Interstellar Medium

Published online by Cambridge University Press:  03 August 2017

Joel N. Bregman  and
Gregory A. Ashe
Joel N. Bregman
Affiliation:
Astronomy Department, University of Michigan Ann Arbor, MI 48109-1090, USA
Gregory A. Ashe
Affiliation:
Astronomy Department, University of Michigan Ann Arbor, MI 48109-1090, USA

Abstract

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We have compared theoretical HI models to a large area (18°x12°) HI channel map centered at 1 = 205°, b = 0°. One set of models were calculated in which uncorrected clouds of HI 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 HI medium. Although not entirely successful, these models contain characteristics that are similar to the data. In order to reproduce the amplitude of the HI variations on angular scales of >1°, the volume occupied by ionized gas must be less than 30%, in sharp conflict with the models that suggest that the volume of the ISM is dominated by hot gas.

Type
III. Theory and Modelling
Information
Symposium - International Astronomical Union , Volume 144: The Interstellar Disk-Halo Connection in Galaxies , 1991 , pp. 387 - 396
Copyright
Copyright © Kluwer 1991 

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