Search for solar electron anti-neutrinos due to spin-flavor precession in the Sun with Super-Kamiokande-IV
Kamiokande Collaboration, K. Abe, C. Bronner, Y. Hayato, M. Ikeda, S. Imaizumi, H. Ito, J. Kameda, Y. Kataoka, M. Miura, S. Moriyama, Y. Nagao, M. Nakahata, Y. … 展开作者
Kamiokande Collaboration, K. Abe, C. Bronner, Y. Hayato, M. Ikeda, S. Imaizumi, H. Ito, J. Kameda, Y. Kataoka, M. Miura, S. Moriyama, Y. Nagao, M. Nakahata, Y. Nakajima, S. Nakayama, T. Okada, K. Okamoto, A. Orii, G. Pronost, H. Sekiya, M. Shiozawa, Y. Sonoda, Y. Suzuki, A. Takeda, Y. Takemoto, A. Takenaka, H. Tanaka, T. Yano, R. Akutsu, S. Han, T. Kajita, K. Okumura, T. Tashiro, R. Wang, J. Xia, D. Bravo-Berguño, L. Labarga, Ll. Marti, B. Zaldivar, F. d. M. Blaszczyk, E. Kearns, J. L. Raaf, J. L. Stone, L. Wan, T. Wester, B. W. Pointin, J. Bian, N. J. Griskevich, W. R. Kropp, S. Locke, S. Mine, M. B. Smy, H. W. Sobel, V. Takhistov, P. Weatherly, J. Hill, J. Y. Kim, I. T. Lim, R. G. Park, B. Bodur, K. Scholberg, C. W. Walter, L. Bernard, A. Coffani, O. Drapier, S. El Hedri, A. Giampaolo, M. Gonin, Th. A. Mueller, P. Paganini, B. Quilain, T. Ishizuka, T. Nakamura, J. S. Jang, J. G. Learned, L. H. V. Anthony, A. A. Sztuc, Y. Uchida, V. Berardi, M. G. Catanesi, E. Radicioni, N. F. Calabria, L. N. Machado, G. De Rosa, G. Collazuol, F. Iacob, M. Lamoureux, N. Ospina, L. Ludovici, Y. Nishimura, S. Cao, M. Friend, T. Hasegawa, T. Ishida, M. Jakkapu, T. Kobayashi, T. Matsubara, T. Nakadaira, K. Nakamura, Y. Oyama, K. Sakashita, T. Sekiguchi, T. Tsukamoto, Y. Nakano, T. Shiozawa, A. T. Suzuki, Y. Takeuchi, S. Yamamoto, A. Ali, Y. Ashida, J. Feng, S. Hirota, A. K. Ichikawa, T. Kikawa, M. Mori, T. Nakaya, R. A. Wendell, Y. Yasutome, P. Fernandez, N. McCauley, P. Mehta, A. Pritchard, K. M. Tsui, Y. Fukuda, Y. Itow, H. Menjo, T. Niwa, K. Sato, M. Tsukada, P. Mijakowski, C. K. Jung, C. Vilela, M. J. Wilking, C. Yanagisawa, M. Harada, K. Hagiwara, T. Horai, H. Ishino, S. Ito, Y. Koshio, W. Ma, N. Piplani, S. Sakai, Y. Kuno, G. Barr, D. Barrow, L. Cook, A. Goldsack, S. Samani, C. Simpson, D. Wark, F. Nova, T. Boschi, F. Di Lodovico, M. Taani, J. Migenda, S. Molina Sedgwick, S. Zsoldos, J. Y. Yang, S. J. Jenkins, M. Malek, J. M. McElwee, O. Stone, M. D. Thiesse, L. F. Thompson, H. Okazawa, S. B. Kim, I. Yu, K. Nishijima, M. Koshiba, K. Iwamoto, N. Ogawa, M. Yokoyama, K. Martens, M. R. Vagins, S. Izumiyama, M. Kuze, M. Tanaka, T. Yoshida, M. Inomoto, M. Ishitsuka, R. Matsumoto, K. Ohta, M. Shinoki, J. F. Martin, H. A. Tanaka, T. Towstego, M. Hartz, A. Konaka, P. de Perio, N. W. Prouse, S. Chen, B. D. Xu, B. Richards, B. Jamieson, J. Walker, A. Minamino, K. Okamoto, G. Pintaudi, R. Sasaki, M. Posiadala-Zezula
Due to a very low production rate of electron anti-neutrinos ($\barν_e$) via nuclear fusion in the Sun, a flux of solar $\barν_e$ is unexpected. An appearance of $\barν_e$ in solar neutrino flux opens a new window for the new physics beyond the standard model. In particular, a spin-flavor precession process is expected to convert an electron neutrino into an electron anti-neutrino (${ν_e\to\barν_e}$) when neutrino has a finite magnetic moment. In this work, we have searched for solar $\barν_e$ in the Super-Kamiokande experiment, using neutron tagging to identify their inverse beta decay signature. We identified 78 $\barν_e$ candidates for neutrino energies of 9.3 to 17.3 MeV in 2970.1 live days with a fiducial volume of 22.5 kiloton water (183.0 kton$\cdot$year exposure). The energy spectrum has been consistent with background predictions and we thus derived a 90% confidence level upper limit of ${4.7\times10^{-4}}$ on the $ν_e\to\barν_e$ conversion probability in the Sun. We used this result to evaluate the sensitivity of future experiments, notably the Super-Kamiokande Gadolinium (SK-Gd) upgrade.
An Indirect Search for WIMPs in the Sun using 3109.6 days of upward-going muons in Super-Kamiokande
我们提出了一个间接搜索的结果，从高能中微子的WIMP湮灭在太阳上使用上行μ子（upmu）事件在超级神冈。使用SKI-SKIII（3109.6天）的数据集进行分析。我们寻找一个多余的中微子信号从太阳相比，预期的大气中微子背景在三个upmu类别：停止，非淋浴，淋浴。未观察到显著过量。90% C. L。由100 GeV/$^2$的WIMP诱导的上行μ子通量的上限对于软和硬湮灭通道分别为6.4 $\times10^{-15}$ cm $^{-2}$ sec $^{-1}$和4.0 $\times10^{-15}$ cm $^{-2}$ sec $^{-1}$。这些极限分别对应于软和硬湮灭通道中自旋相关WIMP-核子散射截面的4.5 $\times10^{-39}$ cm $^{-2}$和2.7 $\times10^{-40}$ cm $^{-2}$的上限。
Search for neutrinos from annihilation of captured low-mass dark matter particles in the Sun by Super-Kamiokande
超级神冈（SK）可以通过探测太阳内部发生的弱相互作用大质量粒子（WIMP）湮灭产生的中微子来寻找WIMP。在这个分析中，我们包括中微子事件的相互作用顶点的检测器除了向上的μ子产生的周围的岩石。与以前的结果相比，它只使用上行的μ子，光（几个GeV/$c^2$ $\sim$ 200-GeV/$c^2$）WIMP的信号接受显着增加。我们拟合了3903天的SK数据，以寻找太阳中WIMP湮灭中微子的贡献。我们发现没有明显超出预期的大气中微子背景和结果解释的上限WIMP核子弹性散射截面在不同的假设下的湮灭通道。我们设置了当前最佳的限制自旋相关（SD）的WIMP质子横截面的WIMP质量低于200 GeV/$c^2$（在10 GeV/$c^2$，1.49 $\times 10^{-39}$ cm $^2$为$χχ\rightarrow b \bar{b}$和1.31 $\times 10^{-40}$ cm $^2$为$χχ\rightarrowτ^+τ^-$湮灭通道），也排除了一些分数的WIMP候选人与自旋无关（SI）耦合在几个GeV/$c^2$质量范围。
A High Sensitivity Search for $\barν_{e}$'s from the Sun and Other Sources at KamLAND
对应于KamLAND探测器0. 28千吨-年曝光量的数据已被用于搜索能量范围为8. 3 MeV $<$ E $_{\barν_e}$ $<$ 14. 8 MeV的$\barν_e$。未发现$1.1{\pm}0.4$事件预期背景的候选事件。该结果可用于获得任何来源的$\barν_{e}$通量的限值。假设所有的$\barν_e$通量都起源于太阳，并具有特征的$^8$ B太阳$ν_e$能谱，我们得到了3.7 \times 10 $^2$ cm $^{-2}$ s $^{-1}$（90% C. L.）在$\barν_e$通量上。我们解释这个限制，对应于$2.8{\times}10^{-4}$的标准太阳模型$^8$ B $ν_e$通量，自旋-味旋进和中微子衰变模型的框架。
GUT monopoles captured by the Sun's gravitation are expected to catalyze proton decays via the Callan-Rubakov process. In this scenario, protons, which initially decay into pions, will ultimately produce ν_{e}, ν_μ and \bar ν_μ. After undergoing neutrino oscillation , all neutrino species appear when they arrive at the Earth, and can be detected by a 50,000 metric ton water Cherenkov detector, Super-Kamiokande (SK). A search for low energy neutrinos in the electron total energy range from 19 to 55 MeV was carried out with SK and gives a monopole flux limit of F_M(σ_0/1 mb) < 6.3 \times 10^{-24…
