Orateur
Prof.
Andrei Bykov
Description
Many of the core-collapsed supernovae are expected to explode within
or in the vicinity of their parent clouds. The manifestation of the
supernova remnants (SNRs) can differ substantially for different
type of their progenitor stars. For the relatively low mass
progenitor the stellar wind and photoionizing radiation are not
sufficient to clear up substantially the surrounding cloud and
already at a radius of about a few pc the remnant is entering a
radiative phase with a shock directly interacting with the molecular
cloud. In contrast, the winds of the most massive stars blow much
larger caverns filled with structured wind resulting in different CR
particle acceleration regimes. Observations of SNRs and galactic
cosmic rays (CRs) suggest that there is a high efficiency of
conversion of the kinetic power of supernova shocks into CRs. We
discuss the specific mechanisms to convert a sizable fraction of the
power released by SNRs into CRs and fluctuating magnetic fields of
wide dynamical range of scales and the observational appearance for
the different types of SNRs. Star forming activity with clustered
supernova explosions in superbubbles observed in galaxies may affect
the observed non-thermal spectra of the starburst galaxies.
