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SN 1987A - After the peak
Woosley, S. E.
AA(Lick Observatory, Santa Cruz; Lawrence Livermore National Laboratory, Livermore, CA)
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 330, July 1, 1988, p. 218-253. (ApJ Homepage)
Publication Date:
NASA/STI Keywords:
Light Curve, Stellar Cores, Stellar Evolution, Stellar Interiors, Stellar Mass, Supernova 1987a, Kinetic Energy, Neutrinos, Neutron Stars, Stellar Envelopes
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This paper attempts to present a coherent and detailed model of SN 1987A. Observations are consistent with the explosion of a star that, on the main sequence, had a mass of 19±3 M_sun; and, at the time of explosion, a helium core mass of 6±1 M_sun;. A neutron star of 1.40±0.15 M_sun; (gravitational mass) has been formed releasing 2 - 3×1053ergs of neutrinos. The kinetic energy of an explosion required to reproduce the light curve and other key data was Eexp ≈ 8×1050(Menv/5 M_sun;) ergs, with Menv the hydrogen envelope mass at the time of the explosion (5 - 10 M_sun;). Stellar models employing low metallicity are explored. Low-metallicity (Z_sun;/4) models (with no mass loss) of 15 and 20 M_sun; stars are presented, both of which burn helium as red supergiants and move back to the blue shortly before exploding. A similarly evolved 25 M_sun; star does not move back to the blue. The light curve of the supernova is now powered by the decay of 0.07 M_sun; of radioactive 56Co, as has been the case since March 1988 when the hydrogen envelope was traversed.

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