Neutrino Nucleosynthesis in Supernovae

The neutrinos detected from the next Galactic core-collapse supernova will contain valuable information on the internal dynamics of the explosion. One mechanism leading to a temporal evolution of the neutrino signal is the variation of the induced neutrino flavor mixing driven by changes in the density profile. With one and two dimensional hydrodynamical simulations we identify the behavior and properties of prominent features of the explosion. Using these results we demonstrate the time variation of the neutrino crossing probabilities due to changes in the MSW neutrino transformations as the star explodes by using the S-matrix -Monte Carlo -approach to neutrino propagation. After adopting spectra for the neutrinos emitted from the proto-neutron star we calculate for a Galactic supernova the evolution of the positron spectra within a water Cerenkov detector and the ratio of charged current to neutral current event rates for a heavy water -SNO like -detector and find that these detector signals are feasible probes of a number of explosion features.

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“…The results of all these nucleosynthesis processes are quite sensitive to the neutrino spectra [8,9,10,11].…”

Section: Introductionmentioning

confidence: 99%

Oscillation effects and time variation of the supernova neutrino signal

2008

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“…Spin and magnetic properties of nuclei have been considerably improved by the Hamiltonians. Neutrino-induced reaction cross sections in 12 C, 4 He, Ni and Fe isotopes are obtained with the use of the new Hamiltonians, and they are found to be enhanced compared with those by conventional Hamiltonians as well as previous calculations. The production yields of 7 Li and 11 B during supernova explosions are found to be enhanced.…”

Section: Pos(nic X)123mentioning

confidence: 99%

“…Toshio Suzuki through 12 C (ν, ν x) 9 Be [12]. 6 Li is produced through 4 He(ν, ν d) 2 H(α, γ) 6 Li, 12 C(ν, ν x) 6 Li, and 9 Be(p, α) 6 Li.…”

Section: Neutrino Nucleus Reactions and Nucleosynthesis In Starsmentioning

confidence: 99%

“…When there are neutrino oscillations, charge-exchange reactions on 4 He and 12 C become important and 7 Li and 11 B are produced through the production of 7 Be and 11 C. The yield ratio N( 7 Li)/N( 11 B) becomes sensitive to the mixing angle θ 13 for the normal neutrino mass hierarchy, which can be used to determine the lower limit of θ 13 as well as if the neutrino mass hierarchy is normal or inverted [11,12].…”

Section: Neutrino Nucleus Reactions and Nucleosynthesis In Starsmentioning

confidence: 99%

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Neutrino Nucleus Reactions and Nucleosynthesis in Stars

Suzuki¹

2009

Proceedings of 10th Symposium on Nuclei in the Cosmos — PoS(NIC X)

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“…Therefore, the difference between the newly measured [36] and previous 4 He photodisintegration cross sections at 20 MeV < ∼ E γ < ∼ 30 MeV could be critical. As a result, the absolute yields of 7 Li and 11 B produced in the ν-process in core-collapse SNe would be different from one another, depending on the assumed ν-process reaction rates as demonstrated theoretically [59,62] although the ratio of 7 Li/ 11 B does not change largely. Another recent focus of photodisintegration of 4 He is on the mechanism of the core-collapse SNe.…”

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confidence: 99%

New constraints on radiative decay of long-lived particles in big bang nucleosynthesis with newHe4photodisintegration data

et al. 2009

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A recent measurement of 4 He photodisintegration reactions, 4 He(γ,p) 3 H and 4 He(γ,n) 3 He with laser-Compton photons shows smaller cross sections than those estimated by other previous experiments at Eγ < ∼ 30 MeV. We study big-bang nucleosynthesis with the radiative particle decay using the new photodisintegration cross sections of 4 He as well as previous data. The sensitivity of the yields of all light elements D, T, 3 He, 4 He, 6 Li, 7 Li and 7 Be to the cross sections is investigated. The change of the cross sections has an influence on the non-thermal yields of D, 3 He and 4 He. On the other hand, the non-thermal 6 Li production is not sensitive to the change of the cross sections at this low energy, since the non-thermal secondary synthesis of 6 Li needs energetic photons of Eγ > ∼ 50 MeV. The non-thermal nucleosynthesis triggered by the radiative particle decay is one of candidates of the production mechanism of 6 Li observed in metal-poor halo stars (MPHSs). In the parameter region of the radiative particle lifetime and the emitted photon energy which satisfies the 6 Li production above the abundance level observed in MPHSs, the change of the photodisintegration cross sections at Eγ < ∼ 30 MeV as measured in the recent experiment leads to ∼ 10 % reduction of resulting 3 He abundance, whereas the 6 Li abundance does not change for this change of the cross sections of 4 He(γ,p) 3 H and 4 He(γ,n) 3 He. The 6 Li abundance, however, could show a sizable change and therefore the future precise measurement of the cross sections at high energy Eγ > ∼ 50 MeV is highly required.

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Neutrino Nucleosynthesis in Supernovae

Cited by 5 publications

References 17 publications

Oscillation effects and time variation of the supernova neutrino signal

Oscillation effects and time variation of the supernova neutrino signal

Neutrino Nucleus Reactions and Nucleosynthesis in Stars

New constraints on radiative decay of long-lived particles in big bang nucleosynthesis with newHe4photodisintegration data

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