Supernova-induced collapse of magnetic interstellar clouds

Details Supernova-induced collapse of magnetic interstellar clouds Supernova-induced collapse of magnetic interstellar clouds

Oct 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985a%26a...151...33o&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 151, no. 1, Oct. 1985, p. 33-42. Research supported by Gould Computer Systems

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Gravitational Collapse, Interstellar Magnetic Fields, Magnetic Clouds, Molecular Clouds, Shock Waves, Stellar Evolution, Supernovae, Astronomical Models, Computational Astrophysics, Magnetohydrodynamics

Scientific paper

The collapse of a cool and dense interstellar cloud induced by a nearby supernova is studied. In the present model computations, the cloud is assumed to be initially spherically symmetric and in pressure equilibrium with the hot interstellar medium. In addition, the presence of a homogeneous magnetic field parallel to the direction from the supernova to the center of the cloud is assumed. The problem can then be treated by means of a two-dimensional magnetohydrodynamic code. The parameters which determine the model have been chosen in such a way that: (1) the cloud would be Jeans-stable without the supernova shock; (2) it would be compressed and collapse due to its self-gravity under the influence of a strong shock, if magnetic fields were absent. It is then found that a field of about 10 micro-G is required in order to prevent a cloud of 5000 solar masses and an average density of 8.3 x 10 to the -23rd g/cu cm from collapsing. These quantities correspond to a ratio of magnetic to gravitational energy of about 3, and a flux-to-mass ratio of roughly 12. For weaker fields, the cloud becomes gravitationally unstable and collapses.

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