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X-rays and γ-rays from Supernova 1987a

Published online by Cambridge University Press:  12 April 2016

P. Sutherland ,
Y. Xu ,
R. McCray  and
R. Ross
P. Sutherland
Affiliation:
Physics Dept., McMaster University, Hamilton, Ontario, Canada and Visiting Member, JILA 1986-87
Y. Xu
Affiliation:
JILA, University of Colorado and National Bureau of Standards, Boulder, Colorado, USA
R. McCray
Affiliation:
JILA, University of Colorado and National Bureau of Standards, Boulder, Colorado, USA
R. Ross
Affiliation:
Dept. of Physics, College of the Holy Cross, Worcester, Mass., USA

Summary

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The observation of X-rays and γ-rays from SN 1987a can provide important constraints on parameters for models of this unique event. We present the results of detailed Monte Carlo calculations of the fluxes to be expected in several X-ray bands and for the strong line at 847 keV associated with the decay of 56Co. Our calculations use Model 10H of Woosley, Pinto, and Ensman(1988), with 0.075M⊙ of radioactive material. If it is assumed that there is no mixing of this material with the layers above, then the X-ray fluxes do not become detectable as early as the observations made by the Ginga team in August, 1987. If these observations correspond to X-rays arising from γ-rays Compton scattered down in energy in the supernova ejecta, rather than the interaction of the ejecta with circumstellar matter, then they can only be explained by mixing outward of radioactive material or an envelope with some combination of less mass or greater kinetic energy per unit mass.

Type
Part III. Chemical and Dynamical Structures of Exploding Stars
Information
International Astronomical Union Colloquium , Volume 108: Atmospherics Diagnostics of Stellar Evolution: Chemical Peculiarity, Mass Loss, and Explosion , 1988 , pp. 394 - 398
Copyright
Copyright © Springer-Verlag 1988

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