The early radiation spectrum, cooling, and escape of supernova shock-accelerated cosmic rays

Details The early radiation spectrum, cooling, and escape of supernova shock-accelerated cosmic rays The early radiation spectrum, cooling, and escape of supernova shock-accelerated cosmic rays

Apr 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979apj...229..682c&link_type=abstract

Astrophysical Journal, Part I, vol. 229, Apr. 15, 1979, p. 682-693. Research supported by the U.S. Department of Energy and NSF

Astronomy and Astrophysics

Astrophysics

15

Cosmic Rays, Particle Acceleration, Radiation Spectra, Shock Waves, Stellar Mass Ejection, Supernovae, X Ray Sources, Doppler Effect, Electron Recombination, Energy Dissipation, Interstellar Gas, Stellar Envelopes, Stellar Luminosity, Surface Cooling, Temperature Distribution

Scientific paper

The early radiation spectrum emitted by the expanded and cooling shock-ejected outer layers of a Type I supernova is derived for a model in which the presupernova star is a minimum-mass highly compact white dwarf. It is found that the outer electrons of matter ejected with energies less than 5 GeV/n will recombine before again becoming ionized by interaction with the interstellar medium, that the K-shell electrons high-Z matter up to an energy of 50,000 GeV/n will recombine before stripping about 1000 yr later in the interstellar medium, and that the formation of relativistic grains is unlikely. The results indicate that a compact presupernova star without an extended envelope should produce both cosmic rays and a burst of radiation, after which the supernova should not be visible until heating at a later time causes a slow rise to maximum luminosity. It is concluded that an observable X-ray burst of several times 10 to the 43rd erg should occur in a few tenths of a second and have a flat spectrum.

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