Orateur
Dr
Daria Kosenko
(Astronomical Institut Utrecht)
Description
We present numerical models for supernova remnant evolution, using a
new version of the hydrodynamical code SUPREMNA. We added cosmic ray
diffusion equation to the code scheme, employing two-fluid
approximation. We investigate the dynamics of the simulated supernova
remnants with different values of cosmic ray acceleration efficiency
and diffusion coefficient. We compare the numerical models with
observational data of Tycho's and SN1006 supernova remnants. We find
models which reproduce the observed locations of the blast wave,
contact discontinuity, and reverse shock for the both remnants, thus
allowing us to estimate the contribution of cosmic ray particles into
total pressure and cosmic-ray energy losses in these supernova
remnants. We derive that the energy losses due to cosmic rays escape
in Tycho's supernova remnant are 10-20% of the kinetic energy flux and
20-50% in SN1006.
