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Non‐thermal radiation from Type Ia supernova remnants
Edmon, Paul P.,Kang, Hyesung,Jones, T. W.,Ma, Renyi Blackwell Publishing Ltd 2011 Monthly notices of the Royal Astronomical Society Vol.414 No.4
<P><B>ABSTRACT</B></P><P>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, <SMALL>cosmicp</SMALL>, 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 π<SUP>0</SUP>s from p–p collisions mostly dominate the gamma‐ray range, although for a hot, low‐density ISM case (<I>n</I><SUB>ISM</SUB>= 0.003 cm<SUP>−3</SUP>), 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.</P>