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Discovery of narrow O VI emission from SN 1987A

Published online by Cambridge University Press:  26 May 2016

George Sonneborn ,
Peter Lundqvist ,
Rosina C. Iping  and
Derek L. Massa
George Sonneborn
Affiliation:
Laboratory for Astronomy and Solar Physics, NASA Goddard Space Flight Center, Code 681.0, Greenbelt, MD 20771, USA
Peter Lundqvist
Affiliation:
Department of Astronomy, Stockholm Observatory, SE-10691 Stockholm, Sverige
Rosina C. Iping
Affiliation:
Laboratory for Astronomy and Solar Physics, NASA Goddard Space Flight Center, Code 681.0, Greenbelt, MD 20771, USA Department of Physics, Catholic University of America, Washington DC 20064, USA
Derek L. Massa
Affiliation:
Laboratory for Astronomy and Solar Physics, NASA Goddard Space Flight Center, Code 681.0, Greenbelt, MD 20771, USA Stinger and Ghaffarian Technologies, Inc., 7701 Greenbelt Road, Suite 400, Greenbelt, MD 20770, USA

Abstract

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The 1032, 1038 Å emission lines of O vi were detected from SN 1987A by the FUSE satellite observations in 2000 and 2001. The lines are extremely narrow (fwhm < 35kms–1), indicating that the emission is not a by-product of the various circums tellar shock phenomena. The most likely origin of the O vi emission lines is recombination of the SN progenitor's red giant wind that was photoionized by the SN shock breakout on 1987 Feb 23.

Type
Part 2. Interiors of Massive Stars
Information
Symposium - International Astronomical Union , Volume 212: A Massive Star Odyssey: From Main Sequence to Supernova , 2003 , pp. 425 - 426
Copyright
Copyright © Astronomical Society of the Pacific 2003 

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