Non-thermal radiation from Type Ia supernova remnants

Paul P. Edmon, Hyesung Kang, T. W. Jones, Renyi Ma

Research output: Contribution to journalArticlepeer-review

20 Scopus citations


We present calculations of expected continuum emissions from Sedov-Taylor phase Type Ia supernova remnants (SNRs), using the energy spectra of cosmic ray (CR) electrons and protons from non-linear diffusive shock acceleration simulations. A new, general-purpose radiative process code, cosmicp, was employed to calculate the radiation expected from CR electrons and protons and their secondary products. These radio, X-ray and gamma-ray emissions are generally consistent with current observations of Type Ia SNRs. The emissions from electrons in these models dominate the radio through X-ray bands. Decays of π0s from p-p collisions mostly dominate the gamma-ray range, although for a hot, low-density ISM case (nISM= 0.003cm-3), the pion decay contribution is reduced sufficiently to reveal the inverse Compton contribution to TeV gamma-rays. In addition, we present simple scalings for the contributing emission processes to allow a crude exploration of model parameter space, enabling these results to be used more broadly. We also discuss the radial surface brightness profiles expected for these model SNRs in the X-ray and gamma-ray bands.

Original languageEnglish (US)
Pages (from-to)3521-3536
Number of pages16
JournalMonthly Notices of the Royal Astronomical Society
Issue number4
StatePublished - Jul 2011


  • Acceleration of particles
  • Cosmic rays
  • ISM: supernova remnants
  • Radiation mechanisms: non-thermal


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