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Light Curve Models for SN 1987A and Diagnosis of Supernova Interior

Published online by Cambridge University Press:  12 April 2016

Ken’ichi Nomoto ,
Toshikazu Shigeyama  and
Masa-aki Hashimoto
Ken’ichi Nomoto
Affiliation:
Department of Earth Science and Astronomy, University of Tokyo, Tokyo
Toshikazu Shigeyama
Affiliation:
Department of Earth Science and Astronomy, University of Tokyo, Tokyo
Masa-aki Hashimoto
Affiliation:
Max-Planck-Institut fur Astrophysik, Garching

Abstract

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Presupernova evolution of the progenitor of SN 1987A, hydrodynamics of explosion (shock propagation, explosive nucleosynthesis), optical light curve due to shock heating and 56Co decay, and X-ray and γ-ray light curves are calculated and compared with the observations of SN 1987A. Constraints on the mass of the hydrogen-rich envelope Menv (i.e., mass loss history) and the helium abundance in the envelope are obtained from the progenitor’s blue-red-blue evolution as well as from the light curve. The explosion energy E and the mass and distribution of 56Ni are inferred from the light curves. Models and observations are in reasonable agreement for E/Menv = 1.5 ± 0.5 × 1050 erg/M⊙, Menv = 5 - 10 M⊙, and MNi ∼ 0.07 M⊙. Mixing of 56Ni into the envelope is indicated.

Light curves of exploding bare helium stars are also calculated to see whether the observed Type Ib supernova light curves can be accounted for.

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. 319 - 334
Copyright
Copyright © Springer-Verlag 1988

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