Nucleosynthesis in Early Supernova Winds II: The Role of Neutrinos

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One of the outstanding unsolved riddles of nuclear astrophysics is the origin of the so called ''p-process'' nuclei from A = 92 to 126. Both the lighter and heavier p-process nuclei are adequately produced in the neon and oxygen shells of ordinary Type II supernovae, but the origin of these intermediate isotopes, especially {sup 92,94}Mo and {sup 96,98}Ru, has long been mysterious. Here we explore the production of these nuclei in the neutrino-driven wind from a young neutron star. We consider such early times that the wind still contains a proton excess because the rates for {nu}{sub e} and positron ... continued below

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Pruet, J; Hoffman, R; Woosley, S; Janka, H & Buras, R November 4, 2005.

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One of the outstanding unsolved riddles of nuclear astrophysics is the origin of the so called ''p-process'' nuclei from A = 92 to 126. Both the lighter and heavier p-process nuclei are adequately produced in the neon and oxygen shells of ordinary Type II supernovae, but the origin of these intermediate isotopes, especially {sup 92,94}Mo and {sup 96,98}Ru, has long been mysterious. Here we explore the production of these nuclei in the neutrino-driven wind from a young neutron star. We consider such early times that the wind still contains a proton excess because the rates for {nu}{sub e} and positron captures on neutrons are faster than those for the inverse captures on protons. Following a suggestion by Froehlich et al. (2005), they also include the possibility that, in addition to the protons, {alpha}-particles, and heavy seed, a small flux of neutrons is maintained by the reaction p({bar {nu}}{sub e}, e{sup +})n. This flux of neutrons is critical in bridging the long waiting points along the path of the rp-process by (n,p) and (n,{gamma}) reactions. Using the unmodified ejecta histories from a recent two-dimensional supernova model by Janka, Buras, and Rampp (2003), they find synthesis of p-rich nuclei up to {sup 102}Pd. However, if the entropy of these ejecta is increased by a factor of two, the synthesis extends to {sup 120}Te. Still larger increases in entropy, that might reflect the role of magnetic fields or vibrational energy input neglected in the hydrodynamical model, result in the production of numerous r-, s-, and p-process nuclei up to A {approx} 170, even in winds that are proton-rich.

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PDF-file: 33 pages; size: 0 Kbytes

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  • Journal Name: Astrophysical Journal; Journal Volume: 1028

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  • Report No.: UCRL-JRNL-216874
  • Grant Number: W-7405-ENG-48
  • Office of Scientific & Technical Information Report Number: 887279
  • Archival Resource Key: ark:/67531/metadc886297

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  • November 4, 2005

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  • Sept. 21, 2016, 2:29 a.m.

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  • Nov. 30, 2016, 1:38 p.m.

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Pruet, J; Hoffman, R; Woosley, S; Janka, H & Buras, R. Nucleosynthesis in Early Supernova Winds II: The Role of Neutrinos, article, November 4, 2005; Livermore, California. (digital.library.unt.edu/ark:/67531/metadc886297/: accessed September 26, 2018), University of North Texas Libraries, Digital Library, digital.library.unt.edu; crediting UNT Libraries Government Documents Department.