2008
DOI: 10.1086/591266
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Neutrino‐Nucleus Reaction Cross Sections for Light Element Synthesis in Supernova Explosions

Abstract: The neutrino-nucleus reaction cross sections of 4 He and 12 C are evaluated using new shell model Hamiltonians. Branching ratios of various decay channels are calculated to evaluate the yields of Li, Be, and B produced through the -process in supernova explosions. The new cross sections enhance the yields of

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Cited by 115 publications
(220 citation statements)
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References 62 publications
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“…In fact, the large uncertainties in the ν yields of 11 B do not allow one to perform an accurate evaluation of the B evolution: instead the observed B evolution (resulting from both GCR and ν-process) has to be used to constrain the 11 B yields of CCSN. Thus, Yoshida et al (2008) argued that the temperature of ν μ,τ − and ν μ,τ − neutrinos inferred from the supernova contribution of 11 B in Galactic chemical evolution models is constrained to the 4.3-6.5 MeV range. Notice that the ν-yields of 11 B depend also on other factors: the available amount of 12 C in the C-shell, which in turn depends -among other things -on 3-α and 12 C(α, γ) reaction rates (see Austin et al 2011); and the compactness of the exploding star, which enhances the neutrino flux (see Nakamura et al 2010, for progenitor stars of type Ic supernova).…”
Section: Evolution Of B Isotopesmentioning
confidence: 99%
“…In fact, the large uncertainties in the ν yields of 11 B do not allow one to perform an accurate evaluation of the B evolution: instead the observed B evolution (resulting from both GCR and ν-process) has to be used to constrain the 11 B yields of CCSN. Thus, Yoshida et al (2008) argued that the temperature of ν μ,τ − and ν μ,τ − neutrinos inferred from the supernova contribution of 11 B in Galactic chemical evolution models is constrained to the 4.3-6.5 MeV range. Notice that the ν-yields of 11 B depend also on other factors: the available amount of 12 C in the C-shell, which in turn depends -among other things -on 3-α and 12 C(α, γ) reaction rates (see Austin et al 2011); and the compactness of the exploding star, which enhances the neutrino flux (see Nakamura et al 2010, for progenitor stars of type Ic supernova).…”
Section: Evolution Of B Isotopesmentioning
confidence: 99%
“…To describe the 2nd decay process, one needs to consider the branching ratios for the decay. We estimate these using a Hauser-Feshbach (HF) statistical model [19][20][21][22][23]. One also needs calculations of the transmission coefficients for the emitted particles.…”
Section: ν-Process Reactionsmentioning
confidence: 99%
“…[48]). The alpha rich freeze-out of such proton-rich matter favors the production of α nuclei (mainly 56 Ni) with some free protons left [49]. We note that this freeze-out also results in enhanced abundances of selected nuclei in the Ca-Fe mass range bringing them into better agreement with observation [9].…”
Section: The νP Processmentioning
confidence: 52%
“…This time scale is much shorter than the beta-decay half-life of the most abundant heavy nuclei (e.g. 56 Ni, 64 Ge). As protons are more abundant than heavy nuclei, antineutrino capture occurs predominantly on protons, causing a steady supply of free neutrons for several seconds [10].…”
Section: The νP Processmentioning
confidence: 97%
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