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When will a pulsar in supernova 1987a be seen?The means by which a pulsar might be detected in the remnant of supernova 1987a in the Large Magellanic Cloud is examined. One possibility is that the slower-than-radioactive decay typically seen in the type II light curves is itself the sign of powering by the underlying pulsar, with the decline representing not the spinning down of the pulsar but rather the declining nebular opacity that would allow increasing amounts of the energy to escape as gamma rays. The test of this hypothesis (if the supernova conforms to type II expectations) would be to look for the 'missing' energy in the form of those gamma rays that escape from the remnant instead of powering it.
Document ID
19880031150
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
Authors
Michel, F. Curtis
(California Inst. of Tech. Pasadena, CA, United States)
Kennel, C. F.
(California Inst. of Tech. Pasadena, CA, United States)
Fowler, William A.
(California Institute of Technology Pasadena, United States)
Date Acquired
August 13, 2013
Publication Date
November 13, 1987
Publication Information
Publication: Science
Volume: 238
ISSN: 0036-8075
Subject Category
Astrophysics
Accession Number
88A18377
Funding Number(s)
CONTRACT_GRANT: NSF PHY-85-05682
CONTRACT_GRANT: NSF PHY-86-04197
CONTRACT_GRANT: NSF AST-85-11709
CONTRACT_GRANT: NGL-05-007-190
Distribution Limits
Public
Copyright
Other

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