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SYPA: Symposium Plasma-Astrophysik
SYPA 1: Plasma Astrophysics
SYPA 1.8: Vortrag
Donnerstag, 20. März 2014, 17:30–17:45, SPA Kapelle
Numerical plasma model for simulation of supernova remnant precursors — •Tatyana Liseykina1, Galina Dudnikova2, and Mikhail Malkov3 — 1Institut für Physik, Universität Rostock, Germany — 2University of Maryland, USA — 3University of California at San Diego, USA
We present a numerical plasma model for simulation of the physical processes in supernova remnant shock precursors. In this model only the cosmic ray (CR) population is modelled kinetically. For the treatment of the magnetic field and the velocity field of the background plasma the ideal compressible MHD equations with sources (CR current and CR pressure gradient) are used. An advantage of such a hybrid model is the possibility to study the most important CR driven instabilities on the ion timescale, neglecting the high-frequency modes associated with electrons. Moreover, the realistic CR-to-background density ratio (∼ 10−5) and the realistic ion-to-electron mass ratio can be used. Furthermore, the hybrid approach can reduce the computational expense relative to a fully kinetic approach while treating some particle populations (CR population in our case) with greater accuracy than MHD allows.