Light-curve models for supernova SN1987A in the Large Magellanic Cloud

Details Light-curve models for supernova SN1987A in the Large Magellanic Cloud Light-curve models for supernova SN1987A in the Large Magellanic Cloud

Jul 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987natur.328..320s&link_type=abstract

Nature (ISSN 0028-0836), vol. 328, July 23, 1987, p. 320-323. Research supported by the University of Tokyo and MOESC.

Computer Science

51

Light Curve, Magellanic Clouds, Neutrinos, Stellar Envelopes, Supernovae, Pulsars, Stellar Luminosity, Stellar Mass Ejection, Stellar Winds

Scientific paper

The shock wave propagation, the subsequent expansion of ejected matter, and the optical light curve of supernova SN1987A in the LMC have been computed, and the results are discussed. It is found that the early light curve can be accounted for by the diffusive release of energy deposited by the shock wave, that the progenitor's radius should be as small as 1-3 x 10 to the 12th cm, and that the explosion energy per unit mass should be relatively large at 2-3 x 10 to the 51st erg for ejected matter of 7-10 solar masses. The light curve after eight days is well reproduced by a model with constant energy input. This input may be due to the activity of an embedded pulsar. The light curves calculated by invoking the radioactive decay of Ni-56 and Co-56 are less satisfactory in accounting for the nearly flat portion observed after 65 days. If Sk-69 202 is the progenitor of SN1987A, its explosion energy should be more than 2 x 10 to the 51st erg; this suggests that a prompt shock mechanism forms a neutron star.

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