BEXCO - Room B(103/104/105)
[CRI019] Non-linear diffusive shock acceleration in young supernova remnants
Non-linear diffusive shock acceleration (NDSA) is believed to be the mechanism responsible for the acceleration of cosmic-rays in supernova remnants. But current steady-state models fail to reproduce spectral features observed in supernova remnants, like spectral breaks or soft spectra at the highest energies. We present a fully time-dependent NDSA-model in which we simultaneously solve the transport equation for cosmic rays, magnetic turbulence, and the hydrodynamical equations for the thermal plasma. The transport equations for cosmic rays and magnetic turbulence are coupled via the cosmic-ray gradient and the spatial diffusion coefficient of the cosmic rays, respectively, while the cosmic-ray pressure modifies the shock structure. Our simulations are 1-D and consider resonant amplification of Alfven waves as scattering turbulence. We apply our model to young type-Ia supernova remnants and point out the differences to existing steady-state models.