MHD simulations of rayleigh-taylor instability in young supernova remnants |
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Authors: | Byung-Il Jun Michael L Norman |
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Institution: | (1) Laboratory for Computational Astrophysics National Center for Supercomputing Applications Department of Astronomy, University of Illinois, Urbana-Champaign, USA |
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Abstract: | Radio observations shows that young supernova remnants such as Tycho and Cas A generally exhibit a circular clumpy shell. This shell shows a radial magnetic field whose equipartition strength is 2 to 3 orders of magnitude higher than the interstellar field. A simple compression of the ambient field by the shock can explain neither of these observations. We show that the Rayleigh-Taylor instability which occurs at the ejecta/ISM interface can explain these observations. We have done MHD simulations of the instability in the shell of Type-I supernova remnants for the first time by utilizing moving grid technique. Our simulation shows that Rayleigh-Taylor and Kelvin-Helmholtz instabilities amplify ambient magnetic fields locally and produce the clumpy radio shell. Strong magnetic field lines draped around the Rayleigh-Taylor fingers produce the radial B-vector polarization, whereas thermal bremsstrahlung from the dense fingers themselves produce the clumpy X-ray emission. |
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Keywords: | Supernova Remnants Instability MHD Simulation |
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