S. Orlando, F. Bocchino, M. Miceli, O. Petruk, M. L. Pumo
Published 2011-09-01Version 1
The thermal structure of the post-shock region of a young supernova remnant (SNR) is heavily affected by two main physical effects, the back-reaction of accelerated cosmic rays (CRs) and the Rayleigh-Taylor (RT) instabilities developing at the contact discontinuity between the ejecta and the shocked interstellar medium (ISM). Here, we investigate the role played by both physical mechanisms in the evolution of SNRs through detailed 3D MHD modeling. Our model describes the expansion of the remnant through a magnetized ISM, including consistently the initial ejecta clumping and the effects on shock dynamics due to back-reaction of accelerated CRs. We discuss the role of the initial ejecta clumpiness in developing strong instabilities at the contact discontinuity which may extend upstream to the main shock and beyond.
Comments: Contribution paper to "Cosmic rays and their interstellar medium environment" (CRISM-2011). The CRISM meeting proceedings will be published in a special issue of the Memorie della Societa` Astronomica Italiana
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