Astronomy and Astrophysics – Astronomy
Scientific paper
May 1988
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apj...328..427c&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 328, May 15, 1988, p. 427-439. Research supported by the National Radio Ast
Astronomy and Astrophysics
Astronomy
32
Astronomical Models, Interstellar Gas, Star Formation, Stellar Mass Ejection, Chemical Composition, Energy Dissipation, H Ii Regions, Hydrodynamics, Stellar Winds
Scientific paper
A 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.
Bregman Joel N.
Chiang Wei-Hwan
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