Search for solar electron anti-neutrinos due to spin-flavor precession in the Sun with Super-Kamiokande-IV

Abe, K.; Bronner, C.; Hayato, Y.; Ikeda, M.; Imaizumi, S.; Itô, Hiroshi; Kameda, J.; Kataoka, Y.; Miura, M.; Moriyama, S.; Nagao, Y.; Nakahata, M.; Nakajima, Yasuhiro; Nakayama, S.; Okada, Taku; Orii, A.; Pronost, G.; Sekiya, H.; Shiozawa, M.; Sonoda, Y.; Suzuki, Y.; Takeda, Atsushi; Takemoto, Y.; Takenaka, A.; Yano, T.; Akutsu, R.; Han, S.; Kajita, T.; Okumura, K.; Tashiro, T.; Wang, R.; Xia, J.; Bravo-Berguño, D.; Labarga, L.; Marti, Ll.; Zaldívar, Bryan; Blaszczyk, F. d. M.; Kearns, E.; Raaf, J. L.; Stone, James L.; Wan, L.; Wester, T.; Pointon, B. W.; Bian, J. G.; Griskevich, N. J.; Kropp, W. R.; Locke, S.; Mine, S.; Smy, M. B.; Sobel, H. W.; Takhistov, Volodymyr; Weatherly, P.; Hill, J.; Kim, J.Y.; Lim, I. T.; Park, R.G.; Bodur, B.; Scholberg, K.; Walter, C. W.; Bernard, L.; Coffani, A.; Drapier, O.; Hedri, Sonia El; Giampaolo, A.; Gonin, M.; Mueller, Th A.; Paganini, P.; Quilain, B.; Ishizuka, T.; Nakamura, T.; Jang, J. S.; Learned, J. G.; Anthony, L. H. V.; Sztuc, A. A.; Uchida, Y.; Berardi, V.; Catanesi, M. G.; Radicioni, E.; Calabria, N. F.; Machado, L. N.; Rosa, G. De; Collazuol, G.; Iacob, F.; Lamoureux, Mathieu; Ospina, N.; Ludovici, L.; Nishimura, Y.; Cao, S.; Friend, M.; Hasegawa, T.; Ishida, Toru; Jakkapu, M.; Kobayashi, T.; Matsubara, T.; Nakadaira, T.; Nakamura, K.; Oyama, Y.; Sakashita, K.; Sekiguchi, T.; Tsukamoto, T.; Nakano, Y.; Shiozawa, T.; Suzuki, A.; Takeuchi, Y.; Yamamoto, Shuji; Ali, Ahmed Farag; Ashida, Yosuke; Feng, J.; Hirota, S.; Ichikawa, A. K.; Kikawa, T.; Mori, Masao; Nakaya, T.; Wendell, R.; Yasutome, Y.; Fernández, P.; McCauley, N.; Mehta, Poonam; Pritchard, A.; Tsui, K. M.; Fukuda, Y.; Itow, Y.; Menjo, H.; Niwa, T.; Sato, K.; Tsukada, M.; Mijakowski, P.; Jung, C. K.; Vilela, C.; Wilking, M. J.; Yanagisawa, C.; Harada, Masayuki; Hagiwara, Kaoru; Horai, T.; Ishino, H.; Ito, S.; Koshio, Y.; Ma, W.; Piplani, N.; Sakai, S.; Kuno, Y.; Barr, G.; Barrow, D.; Cook, L.; Goldsack, A.; Samani, S.; Simpson, C.; Wark, D.; Nova, F.; Boschi, T.; Lodovico, F. Di; Taani, M.; Migenda, J.; Sedgwick, S. Molina; Zsoldos, S.; Yang, J.; Jenkins, S. J.; Malek, M.; McElwee, J.; Stone, O.; Thiesse, M.; Thompson, L.F.; Okazawa, H.; Kim, S.B.; Yu, I.; Nishijima, K.; Koshiba, M.; Iwamoto, K.; Ogawa, Naoyuki; Yokoyama, M.; Martens, K.; Vagins, M. R.; Izumiyama, S.; Kuze, M.; Tanaka, M.; Yoshida, Tadashi; Inomoto, M.; Ishitsuka, M.; Matsumoto, R.; Ohta, Kouji; Shinoki, M.; Martin, J. F.; Tanaka, Hirohisa; Towstego, T.; Hartz, M.; Konaka, A.; Perio, P. de; Prouse, N. W.; Chen, S.; Xu, B. D.; Richards, B.; Jamieson, B.; Walker, John M.; Minamino, A.; Okamoto, Ken‐ichi; Pintaudi, G.; Sasaki, R.; Posiadała-Zezula, M.

doi:10.1016/j.astropartphys.2022.102702

Cited by 9 publications

(16 citation statements)

References 36 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…For the Super-Kamiokande experiment, the limit found in [23], µB ⊥ (r 0 ) < 1.5 × 10 −8 µ B kG, is approximately a factor 2 weaker than our limit (3.11). This difference is probably due to the fact that Super-Kamiokande looked for electron antineutrinos in the energy range 9.3 to 17.3 MeV but used in their analysis the same simplified energyindependent νe appearance probability that was derived in [15] for smaller energies.…”

Section: Jhep10(2022)144contrasting

confidence: 84%

“…High-energy experimental bounds may, however, be relevant for constraining the flux of νe from supernovae. [20], Borexino [22] and Super-Kamiokande [23,30]. For comparison, we show the expected solar νe flux for µ 12 B ⊥ (r 0 ) = 2.5 × 10 −9 µ B kG for the AGSS09 SSM, from our analytical and numerical calculations.…”

Section: Existing Limits From Astrophysical νE Fluxes Revisitedmentioning

confidence: 97%

“…Electron antineutrinos from the Sun have been searched for experimentally by Kam-LAND [17][18][19][20], Borexino [21,22] and Super-Kamiokande [23] collaborations. No excess over the expected backgrounds was found, which allowed the collaborations to establish upper bounds on the product of the transition neutrino magnetic moment and the solar magnetic field strength.…”

Section: Jhep10(2022)144mentioning

confidence: 99%

“…We then re-analyze the results of refs. [17][18][19][20][21][22][23] using our formalism. For reference, we also present a compilation of bounds on neutrino magnetic moments obtained from other experiments and astrophysical observations and express the effective neutrino magnetic moments to which they are sensitive through the fundamental neutrino magnetic moments and leptonic mixing parameters.…”

Section: Jhep10(2022)144mentioning

confidence: 99%

“…We will revisit here the existing limits on neutrino magnetic moments and solar magnetic fields coming from the upper bounds on astrophysical νe fluxes and compare them with our results. At present, the most stringent limits come from the KamLAND experiment [20], although Borexino and Super-Kamiokande set comparable bounds [22,23,30]. In all these experiments the detection channel was inverse beta decay on protons.…”

Section: Existing Limits From Astrophysical νE Fluxes Revisitedmentioning

confidence: 99%

See 4 more Smart Citations

Solar $$ {\overline{\nu}}_e $$ flux: revisiting bounds on neutrino magnetic moments and solar magnetic field

Akhmedov

Martínez-Miravé

2022

J. High Energ. Phys.

View full text Add to dashboard Cite

The interaction of neutrino transition magnetic dipole moments with magnetic fields can give rise to the phenomenon of neutrino spin-flavour precession (SFP). For Majorana neutrinos, the combined action of SFP of solar neutrinos and flavour oscillations would manifest itself as a small, yet potentially detectable, flux of electron antineutrinos coming from the Sun. Non-observation of such a flux constrains the product of the neutrino magnetic moment μ and the strength of the solar magnetic field B. We derive a simple analytical expression for the expected $$ {\overline{\nu}}_e $$ ν ¯ e appearance probability in the three-flavour framework and we use it to revisit the existing experimental bounds on μB. A full numerical calculation has also been performed to check the validity of the analytical result. We also present our numerical results in energy-binned form, convenient for analyses of the data of the current and future experiments searching for the solar $$ {\overline{\nu}}_e $$ ν ¯ e flux. In addition, we give a comprehensive compilation of other existing limits on neutrino magnetic moments and of the expressions for the probed effective magnetic moments in terms of the fundamental neutrino magnetic moments and leptonic mixing parameters.

show abstract

Section: Jhep10(2022)144contrasting

confidence: 84%

Section: Existing Limits From Astrophysical νE Fluxes Revisitedmentioning

confidence: 97%

Section: Jhep10(2022)144mentioning

confidence: 99%

Section: Jhep10(2022)144mentioning

confidence: 99%

Section: Existing Limits From Astrophysical νE Fluxes Revisitedmentioning

confidence: 99%

See 3 more Smart Citations

Solar $$ {\overline{\nu}}_e $$ flux: revisiting bounds on neutrino magnetic moments and solar magnetic field

Akhmedov

Martínez-Miravé

2022

J. High Energ. Phys.

View full text Add to dashboard Cite

show abstract

Solar neutrino physics

Wang

Chen

2023

Progress in Particle and Nuclear Physics

View full text Add to dashboard Cite

Shedding light on neutrino self-interactions with solar antineutrino searches

Wu,

2024

J. Cosmol. Astropart. Phys.

View full text Add to dashboard Cite

Solar antineutrinos are absent in the standard solar model prediction. Consequently, solar antineutrino searches emerge as a powerful tool to probe new physics capable of converting neutrinos into antineutrinos. In this study, we highlight that neutrino self-interactions, recently gaining considerable attention due to their cosmological and astrophysical implications, can lead to significant solar antineutrino production. We systematically explore various types of four-fermion effective operators and light scalar mediators for neutrino self-interactions. By estimating the energy spectra and event rates of solar antineutrinos at prospective neutrino detectors such as JUNO, Hyper-Kamiokande, and THEIA, we reveal that solar antineutrino searches can impose stringent constraints on neutrino self-interactions and probe the parameter space favored by the Hubble tension.

show abstract

Search for solar electron anti-neutrinos due to spin-flavor precession in the Sun with Super-Kamiokande-IV

Cited by 9 publications

References 36 publications

Solar $$ {\overline{\nu}}_e $$ flux: revisiting bounds on neutrino magnetic moments and solar magnetic field

Solar $$ {\overline{\nu}}_e $$ flux: revisiting bounds on neutrino magnetic moments and solar magnetic field

Solar neutrino physics

Shedding light on neutrino self-interactions with solar antineutrino searches

Contact Info

Product

Resources

About