\begin{document}$ pp $\end{document}) fusion chain dominates the neutrino production in the Sun. The uncertainty of the predicted \begin{document}$ pp $\end{document} neutrino flux is at the sub-percent level, whereas that of the best measurement is \begin{document}$ {\cal{O}} $\end{document}(10%). In this study, for the first time, we measure solar \begin{document}$ pp $\end{document} neutrinos in the electron recoil energy range from 24 to 144 keV using the PandaX-4T commissioning data with 0.63 tonne \begin{document}$ \times $\end{document} year exposure. The \begin{document}$ pp $\end{document} neutrino flux is determined as \begin{document}$ (8.0 \pm 3.9 \,{\rm{(stat)}} \pm 10.0 \,{\rm{(syst)}} )\times 10^{10}\, $\end{document}\begin{document}$ \rm{s}^{-1} \rm{cm}^{-2} $\end{document}, which is consistent with the Standard Solar Model and existing measurements, corresponding to an upper flux limit of \begin{document}$ 23.3\times 10^{10}\, $\end{document}\begin{document}$ \rm{s}^{-1} \rm{cm}^{-2} $\end{document} at 90% C.L.."> Measurement of solar <i>pp</i> neutrino flux using electron recoil data from PandaX-4T commissioning run -
  • [1]

    E. G. Adelbergeret al., Rev. Mod. Phys.70, 1265 (1998), arXiv:astro-ph/9805121

  • [2]

    S. Turck-Chiezeet al., Astrophys. J. Lett.555, L69 (2001)

  • [3]

    E. G. Adelbergeret al., Rev. Mod. Phys.83, 195 (2011), arXiv:1004.2318 [nucl-ex]

  • [4]

    N. Vinyoles, A. M. Serenelli, F. L. Villanteet al., Astrophys. J.835, 202 (2017), arXiv:1611.09867 [astro-ph.SR]

  • [5]

    P. C. de Holanda and A. Y. Smirnov,LMA MSW solution of the solar neutrino problem and first KamLAND results, JCAP02, 001 (2003), arXiv:hep-ph/0212270

  • [6]

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

  • [7]

    J. N. Abdurashitovet al. (SAGE), Phys. Lett. B328, 234 (1994)

  • [8]

    G. Belliniet al. (BOREXINO), Nature512, 383 (2014)

  • [9]

    M. Agostiniet al. (BOREXINO), Nature562, 505 (2018)

  • [10]

    Y. Menget al. (PandaX-4T), Phys. Rev. Lett.127, 261802 (2021), arXiv:2107.13438 [hep-ex]

  • [11]

    D. S. Akeribet al. (LZ), Phys. Rev. D101, 052002 (2020), arXiv:1802.06039 [astro-ph.IM]

  • [12]

    E. Aprileet al. (XENON),Projected WIMP sensitivity of the XENONnT dark matter experiment, JCAP11, 031 (2020), arXiv:2007.08796[physics.ins-det]

  • [13]

    W. Maet al. (PandaX), Phys. Rev. Lett.130, 021802 (2023), arXiv:2207.04883 [hep-ex]

  • [14]

    E. Aprileet al. (XENON), Phys. Rev. Lett.126, 091301 (2021), arXiv:2012.02846 [hep-ex]

  • [15]

    X. Zhouet al. (PandaX-II), Chin. Phys. Lett.38, 011301 (2021), arXiv:2008.06485 [hep-ex]

  • [16]

    E. Aprileet al. (XENON), Phys. Rev. D102, 072004 (2020), arXiv:2006.09721 [hep-ex]

  • [17]

    J. Billard, L. Strigari, and E. Figueroa-Feliciano, Phys. Rev. D89, 023524 (2014), arXiv:1307.5458 [hep-ph]

  • [18]

    J. W. Chen, H. C. Chi, C. P. Liuet al., Phys. Lett. B774, 656 (2017), arXiv:1610.04177 [hep-ex]

  • [19]

    H. Maet al. (CDEX), J. Phys. Conf. Ser.1342, 012067 (2020), arXiv:1712.06046 [hep-ex]

  • [20]

    J. Li, X. Ji, W. Haxtonet al., Phys. Procedia61, 576 (2015), arXiv:1404.2651 [physics.ins-det]

  • [21]

    X. Yanet al. (PandaX), Phys. Rev. Lett.132, 152502 (2024), arXiv:2312.15632 [nucl-ex]

  • [22]

    L. Siet al. (PandaX), Research2022, 9798721 (2022), arXiv:2205.12809 [nucl-ex]

  • [23]

    D. Zhanget al., Phys. Rev. C105, 014604 (2022), arXiv:2102.02490 [nucl-ex]

  • [24]

    M. Szydagis, N. Barry, K. Kazkazet al.,NEST: A Comprehensive Model for Scintillation Yield in Liquid Xenon, JINST6, P10002 (2011), arXiv:1106.1613[physics.ins-det]

  • [25]

    E. Aprileet al. (XENON), Eur. Phys. J. C80, 785 (2020), arXiv:2003.03825 [physics.ins-det]

  • [26]

    S. J. Haselschwardt, J. Kostensalo, X. Mougeotet al., Phys. Rev. C102, 065501 (2020), arXiv:2007.13686 [hep-ex]

  • [27]

    E. Aprileet al. (XENON), Phys. Rev. C106, 024328 (2022), arXiv:2205.04158 [hep-ex]

  • [28]

    E. Aprileet al. (XENON), Nature568, 532 (2019), arXiv:1904.11002 [nucl-ex]

  • [29]

    W. Verkerke and D. P. Kirkby,The RooFit toolkit for data modeling, eConfC0303241, MOLT007 (2003), arXiv:physics/0306116

  • [30]

    X. Chenet al.,BambooMC — A Geant4-based simulation program for the PandaX experiments, JINST16(09), T09004 (2021), arXiv:2107.05935 [physics.ins-det]

  • [31]

    S. Agostinelliet al. (GEANT4), Nucl. Instrum. Meth. A506, 250 (2003)

  • [32]

    J. B. Albertet al. (EXO-200), Phys. Rev. C89, 015502 (2014), arXiv:1306.6106 [nuclex]

  • [33]

    X. Cuiet al.,Design and commissioning of the PandaX-4T cryogenic distillation system for krypton and radon removal, JINST16(07), P07046 (2021), arXiv:2012.02436 [physics.ins-det]

  • [34]

    J. N. Abdurashitovet al. (SAGE), Phys. Rev. C80, 015807 (2009), arXiv:0901.2200 [nucl-ex]

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