Hard X-ray and Gamma-Ray Emission from Shell Supernova Remnants

Details Hard X-ray and Gamma-Ray Emission from Shell Supernova Remnants Hard X-ray and Gamma-Ray Emission from Shell Supernova Remnants

Dec 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998tx19.confe.642r&link_type=abstract

Abstracts of the 19th Texas Symposium on Relativistic Astrophysics and Cosmology, held in Paris, France, Dec. 14-18, 1998. Eds.:

Astronomy and Astrophysics

Astrophysics

Scientific paper

Strong shock waves in shell supernova remnants have been shown to be capable of accelerating particles to energies in excess of 100 TeV. Electrons of these energies produce hard X-ray synchrotron emission and TeV inverse-Compton emission by upscattering cosmic microwave background photons. However, bremsstrahlung from suprathermal, nonrelativistic electrons can also produce hard X-ray emission. I calculate model X-ray and gamma-ray images and spectra from both Type Ia and core-collapse supernova remnants. Type Ia remnants are presumed to expand into uniform material, while core-collapse remnants expand into a pre-existing stellar wind with azimuthal magnetic field. Current and planned X-ray and gamma-ray observatories should be able to detect several supernova remnants in each class, and can discriminate between these processes, constraining the physics of shock acceleration to very high energies.

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