Supernova neutrino process and sensitivity to neutrino temperatures

T. Hayakawa; K. Nakamura; M. Kusakabe; T. Kajino; S. Chiba; N. Iwamoto; M. K. Cheoun; G. J. Mathews

Supernova neutrino process and sensitivity to neutrino temperatures

T. Hayakawa
, K. Nakamura
, M. Kusakabe
, T. Kajino
, S. Chiba
, N. Iwamoto
, M. K. Cheoun
, G. J. Mathews

National Institutes for Quantum Science and Technology
Fukuoka University
University of Notre Dame
The University of Tokyo
Institute of Science Tokyo
Japan Atomic Energy Agency
Soongsil University

Research output: Contribution to journal › Conference article › peer-review

Abstract

Some rare isotopes are produced by neutrino-induced reactions in supernova (SN) explosions (v-process). The isotope ⁹²Nb decays to ⁹²Zr with a half-life of 3.47 × 10⁷ years. Although this isotope does not exist in the present solar system, the initial abundance ratio for ⁹²Nb/⁹³Nb at the time of solar system formation (SSF) have been measured in primitive meteorites. The astrophysical origin of ⁹²Nb, however, has remained unknown. The SN v-process origin for ⁹²Nb has been proposed and the SN calculation has demonstrated the v-process origin of ⁹²Nb. The abundances of ν-isotopes depend on neutrino temperatures. In the calculation, the average energies of kT = 3.2, 4.0, 6.0 MeV for the electron neutrino, anti-electron neutrino, and the other neutrinos (v_μ and v_τ), respectively, were used. The observed ratio of ⁹²Nb/⁹³Nb ∼ 10-⁵ can be explained by the v-process.

Original language	English
Article number	249
Journal	Proceedings of Science
Volume	2016-September
State	Published - 2016
Externally published	Yes
Event	26th International Nuclear Physics Conference, INPC 2016 - Adelaide, Australia Duration: 11 Sep 2016 → 16 Sep 2016

Cite this

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title = "Supernova neutrino process and sensitivity to neutrino temperatures",

abstract = "Some rare isotopes are produced by neutrino-induced reactions in supernova (SN) explosions (v-process). The isotope 92Nb decays to 92Zr with a half-life of 3.47 × 107 years. Although this isotope does not exist in the present solar system, the initial abundance ratio for 92Nb/93Nb at the time of solar system formation (SSF) have been measured in primitive meteorites. The astrophysical origin of 92Nb, however, has remained unknown. The SN v-process origin for 92Nb has been proposed and the SN calculation has demonstrated the v-process origin of 92Nb. The abundances of ν-isotopes depend on neutrino temperatures. In the calculation, the average energies of kT = 3.2, 4.0, 6.0 MeV for the electron neutrino, anti-electron neutrino, and the other neutrinos (vμ and vτ), respectively, were used. The observed ratio of 92Nb/93Nb ∼ 10-5 can be explained by the v-process.",

author = "T. Hayakawa and K. Nakamura and M. Kusakabe and T. Kajino and S. Chiba and N. Iwamoto and Cheoun, \{M. K.\} and Mathews, \{G. J.\}",

note = "Publisher Copyright: {\textcopyright} Copyright owned by the author(s).; 26th International Nuclear Physics Conference, INPC 2016 ; Conference date: 11-09-2016 Through 16-09-2016",

year = "2016",

language = "英语",

volume = "2016-September",

journal = "Proceedings of Science",

issn = "1824-8039",

publisher = "Sissa Medialab Srl",

}

TY - JOUR

T1 - Supernova neutrino process and sensitivity to neutrino temperatures

AU - Hayakawa, T.

AU - Nakamura, K.

AU - Kusakabe, M.

AU - Kajino, T.

AU - Chiba, S.

AU - Iwamoto, N.

AU - Cheoun, M. K.

AU - Mathews, G. J.

N1 - Publisher Copyright: © Copyright owned by the author(s).

PY - 2016

Y1 - 2016

N2 - Some rare isotopes are produced by neutrino-induced reactions in supernova (SN) explosions (v-process). The isotope 92Nb decays to 92Zr with a half-life of 3.47 × 107 years. Although this isotope does not exist in the present solar system, the initial abundance ratio for 92Nb/93Nb at the time of solar system formation (SSF) have been measured in primitive meteorites. The astrophysical origin of 92Nb, however, has remained unknown. The SN v-process origin for 92Nb has been proposed and the SN calculation has demonstrated the v-process origin of 92Nb. The abundances of ν-isotopes depend on neutrino temperatures. In the calculation, the average energies of kT = 3.2, 4.0, 6.0 MeV for the electron neutrino, anti-electron neutrino, and the other neutrinos (vμ and vτ), respectively, were used. The observed ratio of 92Nb/93Nb ∼ 10-5 can be explained by the v-process.

AB - Some rare isotopes are produced by neutrino-induced reactions in supernova (SN) explosions (v-process). The isotope 92Nb decays to 92Zr with a half-life of 3.47 × 107 years. Although this isotope does not exist in the present solar system, the initial abundance ratio for 92Nb/93Nb at the time of solar system formation (SSF) have been measured in primitive meteorites. The astrophysical origin of 92Nb, however, has remained unknown. The SN v-process origin for 92Nb has been proposed and the SN calculation has demonstrated the v-process origin of 92Nb. The abundances of ν-isotopes depend on neutrino temperatures. In the calculation, the average energies of kT = 3.2, 4.0, 6.0 MeV for the electron neutrino, anti-electron neutrino, and the other neutrinos (vμ and vτ), respectively, were used. The observed ratio of 92Nb/93Nb ∼ 10-5 can be explained by the v-process.

UR - https://www.scopus.com/pages/publications/85034605166

M3 - 会议文章

AN - SCOPUS:85034605166

SN - 1824-8039

VL - 2016-September

JO - Proceedings of Science

JF - Proceedings of Science

M1 - 249

T2 - 26th International Nuclear Physics Conference, INPC 2016

Y2 - 11 September 2016 through 16 September 2016

ER -

Supernova neutrino process and sensitivity to neutrino temperatures

Abstract

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