Abstract
Abstract The radio emission from supernovae is observed in the first days or years after the explosion. It has a power law spectrum with a low-frequency cut-off moving with time to lower frequencies. The size of radio emitting region increases with time at a rate consistent with the rate of supernova envelope expansion. This kind of spectrum evolution was described by the free-free absorption in the circumstellar matter accumulated by the stellar wind of the pre-supernova or by the synchrotron self-absorption. The synchrotron emission of supernovae is produced by relativistic electrons which are most likely accelerated by the shock associated with the expanding envelope. Three different mechanisms of the shock acceleration were discussed. The first-order Fermi, or diffusive shock acceleration can provide observed flux density of all detected supernovae, but requires very high mass-loss rate and magnetic field. Of the two quasi-perpendicular mechanisms the acceleration by lower-hybrid waves seems to be not...
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