Nonthermal Emission from a Supernova Remnant in a Molecular Cloud

Details Nonthermal Emission from a Supernova Remnant in a Molecular Cloud Nonthermal Emission from a Supernova Remnant in a Molecular Cloud

2000-03-16

arxiv.org/abs/astro-ph/0003235v1

Astrophys.J. 538 (2000) 203-216

Astronomy and Astrophysics

Astrophysics

14 pages, 4 figure, Astrophysical Journal, v.538, 2000 (in press)

Scientific paper

10.1086/309103

In evolved supernova remnants (SNRs) interacting with molecular clouds, such as IC 443, W44, and 3C391, a highly inhomogeneous structure consisting of a forward shock of moderate Mach number, a cooling layer, a dense radiative shell and an interior region filled with hot tenuous plasma is expected. We present a kinetic model of nonthermal electron injection, acceleration and propagation in that environment and find that these SNRs are efficient electron accelerators and sources of hard X- and gamma-ray emission. The energy spectrum of the nonthermal electrons is shaped by the joint action of first and second order Fermi acceleration in a turbulent plasma with substantial Coulomb losses. Bremsstrahlung, synchrotron, and inverse Compton radiation of the nonthermal electrons produce multiwavelength photon spectra in quantitative agreement with the radio and the hard emission observed by ASCA and EGRET from IC 443. We distinguish interclump shock wave emission from molecular clump shock wave emission accounting for a complex structure of molecular cloud. Spatially resolved X- and gamma- ray spectra from the supernova remnants IC 443, W44, and 3C391 as might be observed with BeppoSAX, Chandra XRO, XMM, INTEGRAL and GLAST would distinguish the contribution of the energetic lepton component to the gamma-rays observed by EGRET.

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