Statistics – Computation
Scientific paper
Apr 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011iaus..270..267p&link_type=abstract
Computational Star Formation, Proceedings of the International Astronomical Union, IAU Symposium, Volume 270, p. 267-274
Statistics
Computation
Stars: Formation, Ism: Structure, Globular Clusters: General, Open Clusters And Associations: General
Scientific paper
The feedback form pre-main sequence and young stars influences their vicinity. The stars are formed in clusters, which implies that the winds of individual stars collide with each other. Inside of a star cluster, winds thermalize a fraction of their kinetic energy, forming a very hot medium able to escape from the cluster in the form of a large-scale wind. Outside of the cluster, the cluster wind forms a shock front as it interacts with the ambient medium which is accreted onto the expanding shell. A variety of instabilities may develop in such shells, and in some cases they fragment, triggering second generation of star formation. However, if the cluster surpasses a certain mass (depending on the radius and other parameters) the hot medium starts to be thermally unstable even inside of the cluster, forming dense warm clumps. The formation of next generations of stars may start if the clumps are big enough to self-shield against stellar radiation creating cold dense cores.
Dale Jim
Palous Jan
Silich Sergiy
Tenorio-Tagle Guillermo
Whitworth Anthony
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