Astronomy and Astrophysics – Astrophysics
Scientific paper
2004-10-11
Astrophys.J. 619 (2005) 327-339
Astronomy and Astrophysics
Astrophysics
21 pages, 9 figures, to appear in The Astrophysical Journal
Scientific paper
10.1086/426313
We present results from two-dimensional numerical simulations of the interactions between magnetized shocks and radiative clouds. Our primary goal is to characterize the dynamical evolution of the shocked clouds. We perform runs in both the strong and weak magnetic field limits and consider three different field orientations. For the geometries considered, we generally find that magnetic fields external to, but concentrated near, the surface of the cloud suppress the growth of destructive hydrodynamic instabilities. External fields also increase the compression of the cloud by effectively acting as a confinement mechanism driven by the interstellar flow and local field stretching. This can have a dramatic effect on both the efficiency of radiative cooling, which tends to increase with increasing magnetic field strength, and on the size and distribution of condensed cooled fragments. In contrast, fields acting predominately internally to the cloud tend to resist compression, thereby inhibiting cooling. We observe that, even at modest strengths, internal fields can completely suppress low-temperature cooling.
Anninos Peter
Fragile Chris P.
Gustafson Kyle
Murray Stephen D.
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