Neutrino-Induced Nucleosynthesis of<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mi>A</mml:mi><mml:mo>></mml:mo><mml:mn>64</mml:mn></mml:math>Nuclei: The<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mi>ν</mml:mi><mml:mi>p</mml:mi></mml:math>Process
Carla FröhlichDepartement für Physik und Astronomie, Universität Basel, CH-4056 Basel, SwitzerlandG. Martı́nez-PinedoGesellschaft für Schwerionenforschung, D-64291 Darmstadt, GermanyM. LiebendörferCanadian Institute for Theoretical Astrophysics, Toronto, Ontario M5S 3H8, CanadaF.‐K. ThielemannDepartement für Physik und Astronomie, Universität Basel, CH-4056 Basel, SwitzerlandEduardo BravoDepartament de Física i Enginyeria Nuclear, Universitat Politècnica de Catalunya, E-08034 Barcelona, SpainW. R. HixPhysics Division, Oak Ridge National Laboratory, Oak Ridge, Tennessee 37831, USAK. LangankeGesellschaft für Schwerionenforschung, D-64291 Darmstadt, GermanyN. T. ZinnerInstitute for Physics and Astronomy, University of Århus, DK-8000 Århus C, Denmark
2006lv
ABI
Аннотация
We present a new nucleosynthesis process that we denote as the nu p process, which occurs in supernovae (and possibly gamma-ray bursts) when strong neutrino fluxes create proton-rich ejecta. In this process, antineutrino absorptions in the proton-rich environment produce neutrons that are immediately captured by neutron-deficient nuclei. This allows for the nucleosynthesis of nuclei with mass numbers A>64, , making this process a possible candidate to explain the origin of the solar abundances of (92,94)Mo and (96,98)Ru. This process also offers a natural explanation for the large abundance of Sr seen in a hyper-metal-poor star.
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