Radio polarimetry studies of magnetic turbulence in supernova remnants.

摘要

Polarized radio emission from synchrotron radiation can give us unique information about the structure and amplitude of the magnetic fields in supernova remnants. This has implications for theories of particle acceleration at the forward shock of the SNR, in particular those that involve a strong amplification of the magnetic field through cosmic ray-induced instabilities. This turbulent magnetic field is modeled and I calculate the expected characteristics of polarized synchrotron emission and the effects of Faraday rotation as the radiation propagates through the source. The effects of an underlying homogeneous magnetic field or a compressed shock are also studied. Finally, constraints for realistic parameters describing the magnetic turbulence in the region downstream of the shock are discussed.