TY - JOUR
T1 - Non-thermal radiation from Type Ia supernova remnants
AU - Edmon, Paul P.
AU - Kang, Hyesung
AU - Jones, T. W.
AU - Ma, Renyi
PY - 2011/7
Y1 - 2011/7
N2 - 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.
AB - 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.
KW - Acceleration of particles
KW - Cosmic rays
KW - ISM: supernova remnants
KW - Radiation mechanisms: non-thermal
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U2 - 10.1111/j.1365-2966.2011.18652.x
DO - 10.1111/j.1365-2966.2011.18652.x
M3 - Article
AN - SCOPUS:79959823312
SN - 0035-8711
VL - 414
SP - 3521
EP - 3536
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 4
ER -