Other
Scientific paper
Aug 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006iaujd...9e..44a&link_type=abstract
Supernovae: One Millennium After SN1006, 26th meeting of the IAU, Joint Discussion 9, 17-18 August 2006, Prague, Czech Republic,
Other
Scientific paper
Power law X-ray spectra at photon energies > 5 keV from the young supernova remnants (SNRs) are commonly interpreted as a synchrotron emission of the electrons accelerated at the front of the forward shock wave up to the hundred of TeV energies. At the same time it is assumed that there is a quite strong amplification of the magnetic field in the vicinity of the shock front. Very narrow rims of the emission area are considered as a strong argument in favour of such explanation. This approach faces some difficulties. Particularly this is connected with problem of the strong amplification of the magnetic field near the front of the shock wave: apart from the energy problems the physics of this phenomenon is not understood well and there is no other independent observational facts supporting such possibility. The absence of an exact theory of a strong turbulence allows us to seek other possible models explaining the power law X-ray spectra from young SNRs. This is related to a narrow layer of the shock transition, where the stochastic pulsations of the electric field may accelerate the electrons to the suprathermal energies enough for them to radiate the bremsstrahlung X-rays. In this small region these electrons may have different energy distributions and they may manifest themselves in other wavebands, especially, in the difficult for observations range of ~100 keV. We considered several possible distribution functions of the heated and/or accelerated electrons in the region of the shock front, and calculated expected from them emissions in the wide range of electromagnetic wavelengths.
Asvarov A. I.
Kasumov F. K.
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