Gamma-rays from supernova remnants: Signatures of non-linear shock acceleration

Details Gamma-rays from supernova remnants: Signatures of non-linear shock acceleration Gamma-rays from supernova remnants: Signatures of non-linear shock acceleration

May 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997aipc..410.1157b&link_type=abstract

The fourth compton symposium. AIP Conference Proceedings, Volume 410, pp. 1157-1161 (1997).

Computer Science

Supernova Remnants, Gamma-Ray Sources, Gamma-Ray Bursts, Elementary Particle Processes

Scientific paper

Results from a study of non-linear effects in shock acceleration theory and their impact on the gamma-ray spectra of supernova remnants (SNRs) are presented. These non-linear effects describe the dynamical influence of the accelerated cosmic rays on the shocked plasma at the same time as addressing how the non-uniformities in the fluid flow force the distribution of the cosmic rays to deviate from pure power-laws. Such deviations are crucial to gamma-ray spectral determination. Our self-consistent Monte Carlo approach to shock acceleration, which is ideally suited to addressing SNR spectral issues, is used to predict ion and electron distributions that spawn neutral pion decay, bremsstrahlung and inverse Compton emission components for SNRs. The cessation of acceleration above critical energies in the 1 TeV-10 TeV range caused by the spatial and temporal limitations of the expanding SNR shell yields gamma-ray spectral cutoffs: the resulting emission spectra are quite consistent with Whipple's TeV upper limits to those EGRET unidentified sources that have SNR associations.

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