\begin{document}$ ^8 $\end{document}B solar neutrino measurements, such as its low-energy threshold, high energy resolution compared with water Cherenkov detectors, and much larger target mass compared with previous liquid scintillator detectors. In this paper, we present a comprehensive assessment of JUNO's potential for detecting \begin{document}$ ^8 $\end{document}B solar neutrinos via the neutrino-electron elastic scattering process. A reduced 2 MeV threshold for the recoil electron energy is found to be achievable, assuming that the intrinsic radioactive background \begin{document}$ ^{238} $\end{document}U and \begin{document}$ ^{232} $\end{document}Th in the liquid scintillator can be controlled to 10\begin{document}$ ^{-17} $\end{document} g/g. With ten years of data acquisition, approximately 60,000 signal and 30,000 background events are expected. This large sample will enable an examination of the distortion of the recoil electron spectrum that is dominated by the neutrino flavor transformation in the dense solar matter, which will shed new light on the inconsistency between the measured electron spectra and the predictions of the standard three-flavor neutrino oscillation framework. If \begin{document}$ \Delta m^{2}_{21} = 4.8\times10^{-5}\; (7.5\times10^{-5}) $\end{document} eV\begin{document}$ ^{2} $\end{document}, JUNO can provide evidence of neutrino oscillation in the Earth at approximately the 3\begin{document}$ \sigma $\end{document} (2\begin{document}$ \sigma $\end{document}) level by measuring the non-zero signal rate variation with respect to the solar zenith angle. Moreover, JUNO can simultaneously measure \begin{document}$ \Delta m^2_{21} $\end{document} using \begin{document}$ ^8 $\end{document}B solar neutrinos to a precision of 20% or better, depending on the central value, and to sub-percent precision using reactor antineutrinos. A comparison of these two measurements from the same detector will help understand the current mild inconsistency between the value of \begin{document}$ \Delta m^2_{21} $\end{document} reported by solar neutrino experiments and the KamLAND experiment."> Feasibility and physics potential of detecting <sup>8</sup>B solar neutrinos at JUNO -
  • [1]

    Raymond Davis, Don S. Harmer, and Kenneth C. Hoffman, Phys. Rev. Lett.20, 1205-1209 (1968)

  • [2]

    K. S. Hirataet al., Phys. Rev. Lett.63, 16 (1989)

  • [3]

    P. Anselmannet al., Phys. Lett. B285, 376-389 (1992)

  • [4]

    M. Altmannet al., Phys. Lett. B490, 16-26 (2000)

  • [5]

    A. I. Abazovet al., Phys. Rev. Lett.67, 3332-3335 (1991)

  • [6]

    Y. Fukudaet al., Phys. Rev. Lett.81, 1158-1162 (1998)

  • [7]

    Q. R. Ahmadet al., Phys. Rev. Lett.87, 071301 (2001)

  • [8]

    Q. R. Ahmadet al., Phys. Rev. Lett.89, 011301 (2002)

  • [9]

    C. Arpesellaet al., Phys. Lett. B658, 101-108 (2008)

  • [10]

    H. H. Chen, Phys. Rev. Lett.55, 1534-1536 (1985)

  • [11]

    Francesco L. Villante, Aldo M. Serenelli, Franck Delahayeet al., Astrophys. J.787, 13 (2014)

  • [12]

    Maria Bergemann and Aldo Serenelli,Solar Abundance Problem, (Springer International Publishing, Cham, 2014) pages 245–258

  • [13]

    L. Wolfenstein, Phys. Rev. D17, 2369-2374 (1978)

  • [14]

    S. P. Mikheyev and A. Yu. Smirnov, Sov. J. Nucl. Phys.42, 913-917 (1985)

  • [15]

    Michele Maltoni and Alexei Yu. Smirnov, Eur. Phys. J. A52(4), 87 (2016)

  • [16]

    C. Giunti and Y.F. Li, Phys. Rev. D80, 113007 (2009)

  • [17]

    H.W. Long, Y.F. Li, and C. Giunti, JHEP08, 056 (2013)

  • [18]

    S.J. Li, J.J. Ling, N. Raperet al., Nucl. Phys. B944, 114661 (2019)

  • [19]

    K. Abeet al., Phys. Rev. D94(5), 052010 (2016)

  • [20]

    A. Gandoet al., Phys. Rev. D88(3), 033001 (2013)

  • [21]

    Yasuhiro Nakajima, Recent results and future prospects from Super-Kamiokande, Presentation at the XXIX International Conference on Neutrino Physics and Astrophysics (Neutrino 2020), June 2020

  • [22]

    Fengpeng Anet al., J. Phys. G43(3), 030401 (2016)

  • [23]

    M. Agostiniet al., Phys. Rev. D101(6), 062001 (2020)

  • [24]

    Ivan Esteban and M. C. Gonzalez-Garcia, JHEP01, 106 (2019)

  • [25]

    B. Aharmimet al., Phys. Rev. C88, 025501 (2013)

  • [26]

    John N. Bahcall, E. Lisi, D. E. Alburgeret al., Phys. Rev. C54, 411-422 (1996)

  • [27]

    John N. Bahcall, Phys. Rev. C56, 3391-3409 (1997)

  • [28]

    John N. Bahcall, Aldo M. Serenelli, and Sarbani Basu, Astrophys. J.621, L85-L88 (2005)

  • [29]

    Brandon R. Pyephem astronomy library, https://rhodesmill.org/pyephem/index.html

  • [30]

    S. G. Shepherd, Journal of Geophysical Research: Space Physics119(9), 7501-7521 (2014)

  • [31]

    A.N. Ioannisian, A. Yu. Smirnov, and D. Wyler, Phys. Rev. D92(1), 013014 (2015)

  • [32]

    A. M. Dziewonski and D. L. Anderson, Phys. Earth Planet. Interiors25, 297-356 (1981)

  • [33]

    M. Tanabashiet al., Phys. Rev. D98(3), 030001 (2018)

  • [34]

    Carlo Giunti and Chung W. Kim,Fundamentals of Neutrino Physics and Astrophysics,4 2007

  • [35]

    D. Adeyet al., Nucl. Instrum. Meth. A940, 230-242 (2019)

  • [36]

    Monica Sisti,Radioactive background control for the JUNO experimental setup, Poster at the XXVIII International Conference on Neutrino Physics and Astrophysics (Neutrino 2018), June 2018

  • [37]

    S. Agostinelliet al., Nucl. Instrum. Meth. A506, 250-303 (2003)

  • [38]

    Xin-Ying Li, Zi-Yan Deng, Liang-Jian Wenet al., Chin. Phys. C40(2), 026001 (2016)

  • [39]

    Xuantong Zhang, Jie Zhao, Shulin Liuet al., Nucl. Instrum. Meth. A898, 67-71 (2018)

  • [40]

    S. Abeet al., Phys. Rev. C84, 035804 (2011)

  • [41]

    Jie Zhao, Ze-Yuan Yu, Jiang-Lai Liuet al., Chin. Phys. C38(11), 116201 (2014)

  • [42]

    P. Lombardiet al., Nucl. Instrum. Meth. A925, 6-17 (2019)

  • [43]

    Alexandre Göttel, OSIRIS - A 20 ton liquid scintillator detector as a radioactivity monitor for JUNO, poster at Neutrino 2020, July 2020

  • [44]

    C. Arpesellaet al., Phys. Rev. Lett.101, 091302 (2008)

  • [45]

    M. Agostiniet al., Phys. Rev. D100(8), 082004 (2019)

  • [46]

    Table of nuclides, http://atom.kaeri.re.kr/

  • [47]

    Bellato, M. and others, Nucl. Instrum. Meth. A985, 164600 (2021), arXiv:2003.08339

  • [48]

    S. Abeet al., Phys. Rev. C81, 025807 (2010)

  • [49]

    G. Belliniet al., Phys. Rev. D82, 033006 (2010)

  • [50]

    H. Backet al., Phys. Rev. C74, 045805 (2006)

  • [51]

    M. Agostiniet al., Nature562(7728), 505-510 (2018)

  • [52]

    Shirley Weishi Li and John F. Beacom, Phys. Rev. D91(10), 105005 (2015)

  • [53]

    Shirley Weishi Li and John F. Beacom, Phys. Rev. D92(10), 105033 (2015)

  • [54]

    D. Heck, J. Knapp, J. N. Capdevielleet al.,CORSIKA: a Monte Carlo code to simulate extensive air showers. 1998

  • [55]

    V.A. Kudryavtsev, Computer Physics Communications180(3), 339-346 (2009)

  • [56]

    Björn Wonsak, 3D Topological Reconstruction for the JUNO Detector, Poster at the XXVIII International Conference on Neutrino Physics and Astrophysics (Neutrino 2018), June 2018

  • [57]

    Christoph Genster, Michaela Schever, Livia Ludhovaet al., JINST13(03), T03003 (2018)

  • [58]

    Kun Zhang, Miao He, Weidong Liet al., Radiation Detection Technology and Methods2(13), (2018)

  • [59]

    Björn S. Wonsak, Caren I. Hagner, Dominikus A. Hellgartneret al., JINST13(07), P07005 (2018)

  • [60]

    Y. Abeet al., Nucl. Instrum. Meth. A764, 330-339 (2014)

  • [61]

    Fengpeng Anet al., Phys. Rev. D97(5), 052009 (2018)

  • [62]

    G. Belliniet al., JCAP1308, 049 (2013)

  • [63]

    Jie Zhao, Liang-Jian Wen, Yi-Fang Wanget al., Chin. Phys. C41(5), 053001 (2017)

  • [64]

    P. Vogel and John F. Beacom, Phys. Rev. D60, 053003 (1999)

  • [65]

    H. de Kerretet al., Nature Phys.16(5), 558-564 (2020)

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