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UH cosmic rays: Possible origin in massive starsThe origin of the Z greater than 28, ultraheavy, cosmic rays in supernova explosions of massive stars is considered. For Z greater than 70, the UH data is dominated by an r-process source distribution, but for the elements just beyond iron, 29 or = Z less than 36, the data cannot be explained by any single process of nucleosynthesis. This problem is solved naturally in a massive star model by secondary neutron capture reactions occuring during core helium burning and during explosive carbon burning. Interstellar propagation calculations were performed with these episodes of synthesis as source distributions, and the results offer an explanation for the current UH cosmic-ray data. The heavy element synthesis during explosive carbon burning is reexamined using more realistic initial conditions given by the post-helium-burning configuration of the star. Effects of preferential acceleration are considered, and experimental tests are discussed.
Document ID
19770025123
Acquisition Source
Legacy CDMS
Document Type
Conference Paper
Authors
Wefel, J. P.
(Chicago Univ. Chicago, IL, United States)
Schramm, D. N.
(Chicago Univ. Chicago, IL, United States)
Blake, J. B.
(Aerospace Corp. Los Angeles, United States)
Date Acquired
August 8, 2013
Publication Date
July 29, 1977
Publication Information
Publication: Aerospace Corp. Compilation of Contrib. to the 15th Intern. Cosmic Ray Conf.
Subject Category
Space Radiation
Accession Number
77N32067
Funding Number(s)
CONTRACT_GRANT: NSG-7212
CONTRACT_GRANT: NSF AST-76-21707
Distribution Limits
Public
Copyright
Work of the US Gov. Public Use Permitted.

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