Other
Scientific paper
Oct 1981
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981icar...48...49b&link_type=abstract
Icarus, vol. 48, Oct. 1981, p. 49-58.
Other
6
Interstellar Magnetic Fields, Interstellar Matter, Magnetohydrodynamic Stability, Shock Waves, Star Clusters, Stellar Evolution, Supernovae, Atmospheric Models, Perturbation Theory, Shock Fronts, Shock Wave Propagation, Star Distribution, Stellar Atmospheres
Scientific paper
A possible mechanism for the fragmentation of the expanding shock wave from a supernova to form stellar clusters is considered. A model of supernova shell expansion is constructed in which the ratio of magnetic field intensity to gas density remains constant during the one-dimensional compression of the interstellar medium by the shock, and the gas and field adjust to a quasi-equilibrium within the shell following shock passage. It is shown that the quasi-equilibrium, which may be considered as an isothermal atmosphere, is unstable to a hydromagnetic instability representing a form of the Parker instability, which results in a clumping of gas at intervals on the order of parsecs. The length and time scales of the instability are consistent with the clustering of newly formed stars observed in Canis Major R1, where there is evidence for supernova-induced star formation.
Baierlein Ralph
Herbst William
Schwing E.
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