Wuppertal 2015 – scientific programme

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EP: Fachverband Extraterrestrische Physik

EP 12: Exoplaneten/Astrophysik

EP 12.6: Talk

Friday, March 13, 2015, 12:15–12:30, G.10.02 (HS 9)

Transport of magnetic turbulence in supernova remnants — •Robert Brose^1,2, Igor Telezhinsky^2,3, and Martin Pohl^2,3 — ¹Humboldt-Universitaet zu Berlin, Institute of Physics, Unter den Linden 6, 10099 Berlin, Germany — ²DESY, Platanenaallee 6, 15738 Zeuthen, Germany — ³University of Potsdam, Institute of Physics & Astronomy, Karl-Liebknecht-Strasse 24/25, 14476 Potsdam, Germany

To model the acceleration of cosmic rays in Supernova remnants, we solve a time-dependent transport equation for magnetic turbulence accounting for advection and cascading.

We consider upstream and downstream moving Alfven waves and use the diffusion coefficient, derived from their energy density, to solve a CR transport equation, as described by Telezhinsky, et al., in a test-particle approach combined with 1-D hydrodynamical simulations of the remnant evolution. Thus both equations are coupled via the diffusion coefficient respectively the energy density of the magnetic turbulence and the growth rates so that the acceleration process is treated self-consistently.

We show that the evolution of the maximum CR energy and the decay of turbulence results in softer particle spectra for old remnants. Further evidence is presented that the used injection model might be crucial to explain observed spectral breaks.