Citation

BibTex format

@article{Abe:2022:10.1016/j.astropartphys.2022.102702,
author = {Abe, K and Bronner, C and Hayato, Y and Ikeda, M and Imaizumi, S and Ito, H and Kameda, J and Kataoka, Y and Miura, M and Moriyama, S and Nagao, Y and Nakahata, M and Nakajima, Y and Nakayama, S and Okada, T and Okamoto, K and Orii, A and Pronost, G and Sekiya, H and Shiozawa, M and Sonoda, Y and Suzuki, Y and Takeda, A and Takemoto, Y and Takenaka, A and Tanaka, H and Yano, T and Akutsu, R and Han, S and Kajita, T and Okumura, K and Tashiro, T and Wang, R and Xia, J and Bravo-Berguño, D and Labarga, L and Marti, L and Zaldivar, B and Blaszczyk, FDM and Kearns, E and Raaf, JL and Stone, JL and Wan, L and Wester, T and Pointon, BW and Bian, J and Griskevich, NJ and Kropp, WR and Locke, S and Mine, S and Smy, MB and Sobel, HW and Takhistov, V and Weatherly, P and Hill, J and Kim, JY and Lim, IT and Park, RG and Bodur, B and Scholberg, K and Walter, CW and Bernard, L and Coffani, A and Drapier, O and Hedri, SE and Giampaolo, A and Gonin, M and Mueller, TA and Paganini, P and Quilain, B an},
doi = {10.1016/j.astropartphys.2022.102702},
journal = {Astroparticle Physics},
title = {Search for solar electron anti-neutrinos due to spin-flavor precession in the Sun with Super-Kamiokande-IV},
url = {http://dx.doi.org/10.1016/j.astropartphys.2022.102702},
volume = {139},
year = {2022}
}

RIS format (EndNote, RefMan)

TY  - JOUR
AB - Due to a very low production rate of electron anti-neutrinos (νe) via nuclear fusion in the Sun, a flux of solar νe is unexpected. An appearance of νe 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 (νe→νe) when neutrino has a finite magnetic moment. In this work, we have searched for solar νe in the Super-Kamiokande experiment, using neutron tagging to identify their inverse beta decay signature. We identified 78 νe 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⋅year exposure). The energy spectrum has been consistent with background predictions and we thus derived a 90% confidence level upper limit of 4.7×10−4 on the νe→νe conversion probability in the Sun. We used this result to evaluate the sensitivity of future experiments, notably the Super-Kamiokande Gadolinium (SK-Gd) upgrade.
AU - Abe,K
AU - Bronner,C
AU - Hayato,Y
AU - Ikeda,M
AU - Imaizumi,S
AU - Ito,H
AU - Kameda,J
AU - Kataoka,Y
AU - Miura,M
AU - Moriyama,S
AU - Nagao,Y
AU - Nakahata,M
AU - Nakajima,Y
AU - Nakayama,S
AU - Okada,T
AU - Okamoto,K
AU - Orii,A
AU - Pronost,G
AU - Sekiya,H
AU - Shiozawa,M
AU - Sonoda,Y
AU - Suzuki,Y
AU - Takeda,A
AU - Takemoto,Y
AU - Takenaka,A
AU - Tanaka,H
AU - Yano,T
AU - Akutsu,R
AU - Han,S
AU - Kajita,T
AU - Okumura,K
AU - Tashiro,T
AU - Wang,R
AU - Xia,J
AU - Bravo-Berguño,D
AU - Labarga,L
AU - Marti,L
AU - Zaldivar,B
AU - Blaszczyk,FDM
AU - Kearns,E
AU - Raaf,JL
AU - Stone,JL
AU - Wan,L
AU - Wester,T
AU - Pointon,BW
AU - Bian,J
AU - Griskevich,NJ
AU - Kropp,WR
AU - Locke,S
AU - Mine,S
AU - Smy,MB
AU - Sobel,HW
AU - Takhistov,V
AU - Weatherly,P
AU - Hill,J
AU - Kim,JY
AU - Lim,IT
AU - Park,RG
AU - Bodur,B
AU - Scholberg,K
AU - Walter,CW
AU - Bernard,L
AU - Coffani,A
AU - Drapier,O
AU - Hedri,SE
AU - Giampaolo,A
AU - Gonin,M
AU - Mueller,TA
AU - Paganini,P
AU - Quilain,B
AU - Ishizuka,T
AU - Nakamura,T
AU - Jang,JS
AU - Learned,JG
AU - Anthony,LHV
AU - Sztuc,AA
AU - Uchida,Y
AU - Berardi,V
AU - Catanesi,MG
AU - Radicioni,E
AU - Calabria,NF
AU - Machado,LN
AU - De,Rosa G
AU - Collazuol,G
AU - Iacob,F
AU - Lamoureux,M
AU - Ospina,N
AU - Ludovici,L
AU - Nishimura,Y
AU - Cao,S
AU - Friend,M
AU - Hasegawa,T
AU - Ishida,T
AU - Jakkapu,M
AU - Kobayashi,T
AU - Matsubara,T
AU - Nakadaira,T
AU - Nakamura,K
AU - Oyama,Y
AU - Sakashita,K
DO - 10.1016/j.astropartphys.2022.102702
PY - 2022///
SN - 0927-6505
TI - Search for solar electron anti-neutrinos due to spin-flavor precession in the Sun with Super-Kamiokande-IV
T2 - Astroparticle Physics
UR - http://dx.doi.org/10.1016/j.astropartphys.2022.102702
VL - 139
ER -