Magnetohydrodynamic Simulations of Shock-Cloud Interactions

Details Magnetohydrodynamic Simulations of Shock-Cloud Interactions Magnetohydrodynamic Simulations of Shock-Cloud Interactions

Dec 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003aas...20311102g&link_type=abstract

American Astronomical Society Meeting 203, #111.02; Bulletin of the American Astronomical Society, Vol. 35, p.1381

Astronomy and Astrophysics

Astronomy

Scientific paper

We present results of two-dimensional numerical simulations of the interactions between magnetized shocks and radiative clouds in an inhomogeneous background medium. Our primary goal is to characterize the dynamical effects of the magnetic field, so our new results are compared with an earlier study of unmagnetized radiative shock-cloud interactions. Depending upon its orientation and strength, we generally find that the magnetic field suppresses the growth of destructive instabilities in the cloud. In particular, Rayleigh-Taylor and Kelvin-Helmholtz growths are retarded as transverse magnetic field lines are stretched around the surface of the cloud. The additional magnetic pressure also causes the cloud to become more compressed, which can make cooling more efficient and potentially increase the star-formation efficiency.

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