Radio emission from supernovae in binary systems

Details Radio emission from supernovae in binary systems Radio emission from supernovae in binary systems

May 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001aipc..565...73b&link_type=abstract

YOUNG SUPERNOVA REMNANTS: Eleventh Astrophysics Conference. AIP Conference Proceedings, Volume 565, pp. 73-76 (2001).

Astronomy and Astrophysics

Astrophysics

Supernova Remnants, Mass Loss And Stellar Winds, Supergiant Stars

Scientific paper

We have started a study of the radio emission from supernovae (SNe) exploding in binary systems. Here, we present our results for the case of a Type II SN in a wide binary system, which is viewed pole-on, and in which the companion star is a massive Main Sequence star. At early times the light curves rise more slowly than in the single-star case and are sensitive functions of the separation of the two stars. At late times the light curves are strongly affected by the regions of highly compressed material and the fluxes are higher than in the single-star case. For a given mass loss rate of the SN progenitor star the radio emission of a binary system SNII mimicks the emission that would be produced by a single-star SNII with a higher mass loss rate. .

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