Physics
Scientific paper
Oct 1986
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986inpr.conf...43m&link_type=abstract
In NASA. Ames Research Center Summer School on Interstellar Processes: Abstracts of Contributed Papers p 43 (SEE N87-15043 06-9
Physics
Evolution (Development), Interstellar Gas, Molecular Clouds, Star Formation, Stellar Envelopes, Supernova Remnants, Supernovae, Density Distribution, Stability, Stellar Winds
Scientific paper
Correlated supernovae from an OB association can carve large cavities (greater than 100 pc) in the interstellar medium (ISM), and can punch holes completely through the disk of a spiral galaxy. Supernova remnant energy within such a cavity is thermalized before the shock reaches the supershell. Thus stellar wind theory may be used to model these superbubbles. We describe how the evolution of the superbubble depends on the density distribution of the galactic disk gas and the rate of supernovae in the OB association. At a radius of 100 to 300 pc, the supershell becomes gravitationally unstable, forming giant molecular clouds which are the sites for new star formation. This gravitational instability of the supershells provides a physical mechanism for propagating star formation and may account for the observation of bursts of star formation in galaxies.
Kafatos Menas
Mac Low Mordecai-Mar
McCray Richard
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