Non-thermal radiation from Type Ia supernova remnants

作者：Edmon Paul P^*; Kang Hyesung; Jones T W; Ma Renyi

来源：Monthly Notices of the Royal Astronomical Society, 2011, 414(4): 3521-3536.

DOI：10.1111/j.1365-2966.2011.18652.x

• acceleration of particles
• radiation mechanisms: non-thermal
• cosmic rays
• ISM: supernova remnants

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 pi(0)s from p-p collisions mostly dominate the gamma-ray range, although for a hot, low-density ISM case (n(ISM) = 0.003 cm(-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.

• 出版日期2011-7