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Iron, Cobalt, and Nickel in SN 1987ADuring the first several weeks after the explosion of SN 1987A, Fe/Co/Ni clumps, containing approx. 1% of the mass of the supernova envelope, absorbed most of the energy release by Ni-56 and Co-56 decay. As a result, the clumps expanded relative to the substrate, forming a 'nickel bubble' of low-density Fe/Co/Ni. Later the clumps captured approx. 10% of the radioactive luminosity of gamma rays and positrons. Assuming that these elements are not mixed microscopically with other elements, we find that the clumps must occupy approx. greater than 30% of the volume of the emitting region (radial velocity approx. less than 2500 km/s). The result indicates that the emission at late times is dominated by an extra source of heating and ionization, most likely photoionization by two-photon continuum from metastable helium in the gas surrounding the clumps. The resulting 'frothy' structure, consisting of bubbles of low-density Fe surrounded by higher-density filaments of H, He, and other elements, will persist and may be seen in the spectra and structure of supernova remnants.
Document ID
19970016805
Acquisition Source
Headquarters
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Li, Hongwei
(Joint Inst. for Lab. Astrophysics Boulder, CO United States)
McCray, Richard
(Joint Inst. for Lab. Astrophysics Boulder, CO United States)
Sunyaev, Rashid A.
(Institute of Space Research Moscow, USSR)
Date Acquired
August 17, 2013
Publication Date
December 20, 1993
Publication Information
Publication: The Astrophysical Journal
Publisher: American Astronomical Society
Volume: 419
Subject Category
Astrophysics
Report/Patent Number
NASA-CR-204022
NAS 1.26:204022
Accession Number
97N71525
Funding Number(s)
CONTRACT_GRANT: NAGw-2900
CONTRACT_GRANT: NAGw-766
Distribution Limits
Public
Copyright
Public Use Permitted.
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