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A new site for the astrophysical gamma-processThe study suggests that the requisite thermodynamic conditions may occur when carbon-oxygen white dwarfs explode by deflagration or detonation. When these stars undergo such explosive disruption, there will be a region near the surface where the burning temperature lies in the 2.4-3.2 range. To examine this astrophysical site, calculations are performed for an s-process nucleosynthesis during helium shell flashes and the nuclear transmission taking place when such mass zones are heated by the deflagration or detonation wave, and the results are compared with the solar-system distribution of the p-isotopes. It is demonstrated that Type Ia supernovas provide a viable site for the gamma process, and that the same thermodynamic conditions would also exist in Type II-p powered supernovas, provided that they are powered by detonation.
Document ID
19910051965
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Howard, W. Michael
(Lawrence Livermore National Lab. Livermore, CA, United States)
Meyer, Bradley S.
(Lawrence Livermore National Laboratory Livermore, CA, United States)
Woosley, S. E.
(California, University Santa Cruz, United States)
Date Acquired
August 15, 2013
Publication Date
May 20, 1991
Publication Information
Publication: Astrophysical Journal, Part 2 - Letters
Volume: 373
ISSN: 0004-637X
Subject Category
Astrophysics
Accession Number
91A36588
Funding Number(s)
CONTRACT_GRANT: NAGW-1273
CONTRACT_GRANT: W-7405-ENG-48
CONTRACT_GRANT: NSF AST-88-13649
Distribution Limits
Public
Copyright
Other

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