An interacting binary model for SN1987A

Details An interacting binary model for SN1987A An interacting binary model for SN1987A

Jul 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987natur.328..323f&link_type=abstract

Nature (ISSN 0028-0836), vol. 328, July 23, 1987, p. 323, 324.

Computer Science

13

Binary Stars, Iue, Magellanic Clouds, Stellar Models, Supernovae, B Stars, Neutron Stars, Stellar Luminosity, Stellar Mass Ejection

Scientific paper

An alternative model for SN1987A is presented in which the progenitor was a close binary companion of Sk-69 202. In the model, the companion loses mass to Sk-69 202, eventually becoming reduced to a helium star whose core collapses, resulting in the supernova outburst. The envelope of the star is an obvious source for the hydrogen observed in the spectrum of SN1987A. The reduced luminosity of the supernova is presumed to be due to the small size of the helium star. The model predicts that the supernova ejecta will contain roughly equal numbers of hydrogen and helium atoms. The explosion will increase the orbital period and eccentricity of the binary system and give it a runaway velocity. These properties may be observable in one year, after the photosphere of the supernova has shrunk back within the binary system so that Sk-69 202 is again visible.

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