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Collapse of 9 solar mass starsGeneral relativistic hydrodynamical calculations of the collapse of O + Ne + Mg cores of a 9 solar mass star are reported. Collapse is induced by rapid electron captures as the O + Ne + Mg is burned to nuclear statistical equilibrium. The high entropy in the core after burning leads to a large abundance of free protons which readily capture electrons. This leads to large neutrino losses and a correspondingly small infalling homologous core. The hydrodynamic shock thus forms at a small mass point. The shock stalls before reaching the edge of the O + Ne + Mg core and thereby fails to produce a successful supernova explosion by the direct mechanism. No enhancement in the shock energy due to nuclear burning is found.
Document ID
19880023096
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Baron, E.
(Steward Observatory, Tucson, AZ; New York, State University Stony Brook, United States)
Cooperstein, J.
(New York, State University Stony Brook; Brookhaven National Laboratory, Upton, United States)
Kahana, S.
(Brookhaven National Laboratory Upton, NY, United States)
Date Acquired
August 13, 2013
Publication Date
September 1, 1987
Publication Information
Publication: Astrophysical Journal, Part 1
Volume: 320
ISSN: 0004-637X
Subject Category
Astrophysics
Accession Number
88A10323
Funding Number(s)
CONTRACT_GRANT: NAGW-763
CONTRACT_GRANT: DE-AC02-76ER-13001
CONTRACT_GRANT: DE-AC02-76CH-00016
Distribution Limits
Public
Copyright
Other

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