Circumstellar interaction and a pulsar nebula in the supenova 1986j

Details Circumstellar interaction and a pulsar nebula in the supenova 1986j Circumstellar interaction and a pulsar nebula in the supenova 1986j

Oct 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987natur.329..611c&link_type=abstract

Nature (ISSN 0028-0836), vol. 329, Oct. 15, 1987, p. 611-612. NSF-NASA-supported research.

Physics

27

Pulsars, Stellar Envelopes, Stellar Mass Ejection, Stellar Models, Supernovae, Crab Nebula, Mass Flow Rate, Stellar Winds, Very Long Base Interferometry

Scientific paper

The supernova SN 1986j in NGC 891 was first discovered as a radio source in August 1986. The author shows that the circumstellar interaction model for radio supernovae provides an adequate fit to the existing data. A shell-like source structure is expected. The model together with VLBI observations of the radio source, implies a shock velocity of ≡104km s-1 and a pre-supernova mass loss rate of ≡10-4M_sun;yr-1 for a wind velocity of 10 km s-1. The time behaviour of the optical flux and its high luminosity suggest that a central pulsar nebula is the energy source. The radiated energy from the pulsar neula is absorbed by expanding, helium-rich material extending out to a velocity of ≡700 km s-1 or a radius of 8×1015cm on September 1986. The radius of the pulsar nebula at that time is ≡5×1015cm.

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