The rp-Process in Neutrino-driven Winds

By S. Wanajo. 2006

165 citations recorded by the source corpus.

Recent hydrodynamic simulations of core-collapse supernovae with accurate neutrino transport suggest that the bulk of the early neutrino-heated ejecta is proton rich, in which the production of some interesting proton-rich nuclei is expected. As suggested in recent nucleosynthesis studies, the rapid proton-capture (rp) process takes place in such proton-rich environments by bypassing the waiting point nuclei with β+-lives of a few minutes via the faster capture of neutrons continuously supplied from the neutrino absorption by protons. In this study, the nucleosynthesis calculations are performed with a wide range of neutrino luminosities and electron fractions (Ye), using semianalytic models of proto-neutron-star winds. The masses of proto-neutron stars are taken to be 1.4 and 2.0 M☉, where the latter is regarded as the test for somewhat high-entropy winds (about a factor of 2). For Ye > 0.52, the neutrino-induced rp-process takes place in many wind trajectories, and p-nuclei up to A ~ 130 are synthesized in interesting amounts. However, 92Mo is somewhat underproduced compared to other p-nuclei with similar mass numbers. For 0.46 < Ye < 0.49, on the other hand, 92Mo is significantly enhanced by the nuclear flows in the vicinity of the abundant 90Zr that originates from the α-process at higher temperature. The nucleosynthetic yields are averaged over the ejected masses of winds, and further, over the Ye distribution predicted by a recent hydrodynamic simulation of a core-collapse supernova. Comparison of the Ye- and mass-averaged yields to the solar compositions implies that the neutrino-driven winds can potentially be the origin of light p-nuclei up to A ~ 110, including 92,94Mo and 96,98Ru, that cannot be explained by other astrophysical sites.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/78f9f4cd3d15f61640cac5e200b08d95d5a47825

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Citations in the corpus

Neutrino-driven wind simulations and nucleosynthesis of heavy elements (2012, background): “Wanajo (2006) [50] showed that extra energy could be the outcome of an anisotropic neutrino emission.”
Protoneutron star evolution and the neutrino-driven wind in general relativistic neutrino radiation hydrodynamics simulations (2009, background): “Recently, Wanajo (2006a) and Wanajo (2006b) investigated the neutrino driven wind with respect to the r- and rp-processes.”
NUCLEOSYNTHESIS IN ELECTRON CAPTURE SUPERNOVAE OF ASYMPTOTIC GIANT BRANCH STARS (2008, background): “This can also be seen in the early neutrinodriven winds (Hoffman et al. 1996; Wanajo 2006).”
Supernova Nucleosynthesis in Population III 13-50 M☉ Stars and Abundance Patterns of Extremely Metal-poor Stars (2007, background): “Other possible production sites of Zn include the neutrinodriven wind from a protoYneutron star (e.g., Hoffman et al. 1996; Pruet et al. 2005; Fröhlich et al. 2006b;Wanajo 2006a, 2006b) and the accretion disk of a black hole (e.g., Pruet et al. 2004a, 2004b; Fröhlich et al. 2006a).”
Nucleosynthesis in the Early Galaxy (2007, background): “In addition, Fröhlich et al. (2006) and Wanajo (2006) have recently suggested that the νp-process might contribute to the Y, Sr, and Zr abundances observed in metal-poor stars.”
Galactic Chemical Evolution: Carbon through Zinc (2006, background): “A jet-like explosion (Maeda & Nomoto 2003) can efficiently increase Ti and Zn abundances and a low-density model (UN05) or neutrino process (Fröhlich et al. 2006; Wanajo 2006; Yoshida, Umeda, & Nomoto 2006) may increase Sc abundance.”