Theoretical light curve of SN 1987A and mixing of hydrogen and nickel in the ejecta

Details Theoretical light curve of SN 1987A and mixing of hydrogen and nickel in the ejecta Theoretical light curve of SN 1987A and mixing of hydrogen and nickel in the ejecta

Sep 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...360..242s&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 360, Sept. 1, 1990, p. 242-256. Research supported by the Institute of Spac

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193

Interstellar Chemistry, Light Curve, Metallicity, Stellar Mass Ejection, Stellar Models, Supernova 1987A, Finite Difference Theory, Hydrogen, Nickel, Stellar Luminosity, Thermodynamic Equilibrium

Scientific paper

Earlier light curve models for SN 1987A have been improved by adopting more realistic presupernova models and adopting a postexplosion elemental distribution consistent with X-ray and gamma-ray observations. The light curve shape is sensitive to the distributions of abundance and expansion velocity in the ejecta. It is found that the prepeak smooth rise and the broad peak of the light curve, respectively, are well modeled by assuming some mixing of Ni-56 into the hydrogen-rich envelope and of hydrogen into the core. The existence of the hydrogen recombination front is responsible for the formation of the plateaulike peak. For explosion energy, good agreement with the observed light curve is obtained for E/M(env) = (1.1 + or - 0./3) x 10 to the 50th ergs/solar mass. Further improvements on the early light curve, the dependence of the light curve on the distribution of Ni-56 and hydrogen, and the relation with other type II supernovae are discussed.

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