Speaker
Description
Majority of supernova remnants expand into a complex environment of the stellar wind bubble blown up either by their progenitor or their companion star, where forward shock might interact with various density inhomogeneities. Such interactions would cause formation of fast reflected shocks propagating back and forth between the forward shock, the contact discontinuity in the interior of the remnant and the reverse shock. Current investigations of particle acceleration at supernova remnant shocks usually ignore the complexity of the hydrodynamic picture. On the other hand, rapidly improving observational facilities allow now for precise spatially and temporally resolved measurements that do not always agree with simplified modelling. It is intuitive that many irregularities as compared to the classical view of non-thermal emission from supernova remnants could be connected to the particulars of the environment. This work investigates the impact of the interaction of a reflected shock with a forward shock of an SNR on the particle acceleration in the source and examines observational signatures that could potentially arise from such interactions. We demonstrate that such interaction could lead to significant variability of the X-ray and gamma-ray flux on yearly time scale accompanied with the change of the spectral shape.
