Speaker
Description
We study the nuclear abundances produced from neutrino process in supernova (SN) explosion. We consider the neutrino oscillation effects as neutrino scattering not only with matter, $i.e.$ electron background, but also neutrinos themselves in SN environment. The changed neutrino spectrum by $\nu$ oscillation are affected to $\nu$-nucleus reaction rate, so that the abundances during SN explosion change. The different shape of $\nu$ spectrum after oscillation depend on neutrino luminosity and averaged energy for each flavor by SN model. We investigate two different SN model for oscillation: one is the SN1987A model with equivalent neutrino luminosity for each flavor and consider only cooling phase of SN explosion with fixed neutrino temperature [1][2]. Second model is simulated SN explosion data in [3]. We average 6 models data and consider accretion and cooling phase. Our focusing elements for oscillation effect are $^{7}$Li,$^{11}$B [4], $^{92}$Nb [5], $^{98}$Tc [6] and $^{138}$La, which are mainly produced by neutrino reactions.
References
[1] T. Yoshida, M. Terasawa, T. Kajino and K. Sumiyoshi, Astrophys. J. 600, 204 (2004)
[2] T. Yoshida, T. Kajino, D. H. Hartmann, Phys. Rev. Lett. 94, 231101 (2005).
[3] E. O'Connor $et al.$, J. Phys. G 45, no. 10, 104001 (2018)
[4] Motohiko Kusakabe, Myung-Ki Cheoun, K. S. Kim, Masa-aki Hashimoto, Masaomi Ono, Ken'ichi Nomoto, Toshio Suzuki, Toshitaka Kajino, Grant J. Mathews, Astrophys. J. 872, 164 (2019)
[5] T. Hayakawa, K. Nakamura, T. Kajino, S. Chiba, N. Iwamoto, Myung-Ki Cheoun, and G. J. Mathews, ApJL 779, 1 (2013).
[6] T. Hayakawa, Heamin Ko, Myung-Ki Cheoun, M. Kusakabe, T. Kajino, M. D. Usang, S. Chiba, K. Nakamura, A. Tolstov, K. Nomoto, M. A. Hashimoto, M. Ono, T. Kawano, G. J. Mathews, Phy. Rev. Lett. 121, 102701, (2018).
| Working Group | WG1 : Neutrino Oscillation Physics |
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