Gamma-rays from cosmic ray interactions in supernova shellsA model is presented for the transport and interaction of cosmic rays accelerated by a pulsar and confined inside an expanding supernova remnant. Assuming that protons are accelerated at the reverse shock in the confined pulsar wind and convected into the shell via the Rayleigh-Taylor instability, the diffusion and interaction of these protons in the expanding envelope is modeled. The resulting gamma-ray flux is lower than previous estimates due primarily to the inclusion of proton adiabatic losses in the expanding pulsar wind. Energy-dependent diffusion causes the higher energy gamma-ray light curves to decay faster than those at lower energy. The predicted flux from SN1987A, for proton luminosity less than 10 exp 40 erg/s, is below the present detector sensitivities at both GeV and TeV energies, although supernovae occurring within the Galaxy may be detectable.
Document ID
19920054195
Acquisition Source
Legacy CDMS
Document Type
Conference Paper
Authors
Harding, A. K. (NASA Goddard Space Flight Center Greenbelt, MD, United States)
Mastichiadis, A. (Max-Planck-Institut fuer Kernphysik Heidelberg, Federal Republic of Germany, United States)
Protheroe, R. J. (NASA Goddard Space Flight Center Greenbelt, MD, United States)