Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...21113910s&link_type=abstract
American Astronomical Society, AAS Meeting #211, #139.10; Bulletin of the American Astronomical Society, Vol. 39, p.986
Astronomy and Astrophysics
Astronomy
Scientific paper
We present the analysis of numerical simulations done on a strong shock passing a spherical cloud. The problem is considered in full three-dimensional magnetohydrodynamics with a variety of initial magnetic field strengths and orientations. We assume that the interaction occurs on timescales much shorter than gravitational collapse, radiative cooling, and heat conduction. Thus, the problem is defined for a given initial field and cloud setup by three quantities: the mach number MS which we take to be 10, the adiabatic index γ = 5/3, and the smooth profile's central overdensity χ = 10. At early times, the structure of the shocked cloud is relatively insensitive to the initial configuration of the magnetic field. The parallel magnetic field confines the turbulent instabilities developed in the cloud, and delays its complete destruction by a few dynamical timescales. The strong field suppresses the mixing rate at late times. A region of sustained strong vorticity and field develops downwind of the cloud and appears to drift away in time. Even weak fields can drastically influence the evolution of the cloud compared to the hydrodynamic case, which may affect the pattern of x-ray emission from shocked clouds associated with, for example, supernovae.
Shin Mincheol
Snyder Gregory
Stone Jacqueline
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