X-rays from SN 1986J - Emission of a shocked clumpy wind

Details X-rays from SN 1986J - Emission of a shocked clumpy wind X-rays from SN 1986J - Emission of a shocked clumpy wind

Sep 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...414l.101c&link_type=abstract

Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 414, no. 2, p. L101-L103.

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43

Emission Spectra, Stellar Winds, Supernovae, X Ray Spectra, Computational Astrophysics, Shock Waves, Stellar Mass Ejection, Very Long Base Interferometry

Scientific paper

An alternative view on the origin of the powerful X-ray emission from SN 1986J is proposed. The model suggests that the supernova envelope is colliding with the clumpy circumstellar wind, and the bulk of the observed X-rays originates from the shocked dense wind clumps. The required mass loss rate for the clumpy component of the wind is about 0.0001 solar mass/yr, while the filling factor is approximately equal to 0.005. The homogeneous wind is relatively rarefied and contains significantly lower mass than the clumpy component. The model of the clumpy wind is qualitatively consistent with optical and radio data.

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