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A model for the interaction between stars and gas in the interstellar mediumA model for the ISM is considered in which stars lose mass and heat the gas while the gas can form into stars. Three scale-free models are calculated, and in each case the star formation instability leads to a network of dense filaments that surround hotter, more rarefied gas, all of which are close to pressure equilibrium. Depending upon the star formation and cooling laws adopted, the stars are located either in the middle of a bubble or along the inside edge of a dense filament. When a model for the ISM with a cooling curve appropriate for gas of cosmic abundance and a star formation rate proportional to the local gas density is used, the star formation instability is found to grow at temperatures below about 10,000 K. A network structure develops in which most of the mass is in neutral filaments. Newly formed stars lie adjacent to the filaments and create pressure forces that lead to filament motion.
Document ID
19880049552
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Chiang, Wei-Hwan
(Texas, University Austin; Virginia, University; National Radio Astronomy Observatory, Charlottesville, VA, United States)
Bregman, Joel N.
(National Radio Astronomy Observatory Charlottesville, VA, United States)
Date Acquired
August 13, 2013
Publication Date
May 15, 1988
Publication Information
Publication: Astrophysical Journal, Part 1
Volume: 328
ISSN: 0004-637X
Subject Category
Astrophysics
Accession Number
88A36779
Funding Number(s)
CONTRACT_GRANT: NSF AST-84-51736
CONTRACT_GRANT: NAGW-764
Distribution Limits
Public
Copyright
Other

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