Astronomy and Astrophysics – Astrophysics
Scientific paper
May 1986
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986ap%26ss.122...41b&link_type=abstract
Astrophysics and Space Science (ISSN 0004-640X), vol. 122, no. 1, May 1986, p. 41-56.
Astronomy and Astrophysics
Astrophysics
6
Galactic Structure, Star Distribution, Stellar Evolution, Chronology, H Ii Regions, Interstellar Gas, Molecular Clouds, Nonequilibrium Conditions, Stellar Mass
Scientific paper
The theory of dissipative structures, applied to star formation systems, provides a conceptual framework for the study of the behavior and evolution of these systems. As shown by an analysis of a model star formation process system, prolonged stationary star formation in localized areas and repetitive bursting star formation events can be understood as different behavioral modes of galactic dissipative structures. Young stellar associations with their H II regions and molecular clouds are manifestations of the ordered distribution of matter participating in the star formation processes. A self-organization with the appearance of ordered structures is, in general, to be expected in nonequilibrium systems in which nonlinear processes occur. However, lacking a thermodynamic theory that can be applied to self-gravitating systems, the behavior of star-forming regions can only be studied by model calculations simulating the process system within the region.
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