We report on a project aimed at simulating the morphological and
spectral evolution of young supernova remnants undergoing particle
acceleration. If a sizable fraction of the energy is channeled into
energetic particles, noticeable modifications of the shock structure
are expected - and are indeed suggested by recent observations with
Chandra and XMM. We are thus developing a time-dependent 3D code which
enables us to study the shrinking of the region between the forward
and the reverse shocks, concomitantly with the development of the
Rayleigh-Taylor instability at the contact discontinuity. To model
acceleration of particles by the shock, we use a semi-analytical
non-linear kinetic model. As a first step to take into account the
back-reaction of energetic particles, the adiabatic index of the fluid
is varied accordingly at the shock front. The next step will be a
multi-fluid approach, in order to derive both the thermal and
non-thermal emission from the remnant.
View poster as pdf.