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2024年10月30日
Chinese Physics C> 2016, Vol. 40> Issue(7) : 073102 DOI: 10.1088/1674-1137/40/7/073102

Detection of supernova neutrinos at spallation neutron sources

  • After considering supernova shock effects, Mikheyev-Smirnov-Wolfenstein effects, neutrino collective effects, and Earth matter effects, the detection of supernova neutrinos at the China Spallation Neutron Source is studied and the expected numbers of different flavor supernova neutrinos observed through various reaction channels are calculated with the neutrino energy spectra described by the Fermi-Dirac distribution and the "beta fit" distribution respectively. Furthermore, the numerical calculation method of supernova neutrino detection on Earth is applied to some other spallation neutron sources, and the total expected numbers of supernova neutrinos observed through different reactions channels are given.
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  • References

    [1] K. Kotake, K. Sato and K. Takahashi, Rept. Prog. Phys., 69:971-1143(2006)
    [2] A. Mirizzi, I. Tamborra, H. T. Janka et al, arXiv:1508. 00785
    [3] X. H. Guo, M. Y. Huang and B. L. Young, Chin. Phys. C, 34(2):257-261(2010)
    [4] K. Hirata, T. Kajita, M. Koshiba et al, Phys. Rev. Lett., 58:1490-1493(1987)
    [5] R. M. Bionta, G. Blewitt, C. B. Bratton et al, Phys. Rev. Lett., 58:1494-1496(1987)
    [6] K. Scholberg, Ann. Rev. Nucl. Part. Sci., 62:81-103(2012)
    [7] CSNS Project Team, China Spallation Neutron Source Feasi-bility Research Report, Institute of High Energy Physics and Institute of Physics, Chinese Academy of Sciences, 2009(in Chinese)
    [8] J. Wei, S. N. Fu, J. Y. Tang et al, Chin. Phys. C, 33(11):1033-1042(2009)
    [9] S. Wang, S. X. Fang, S. N. Fu et al, Chin. Phys. C, 33 (Suppl. II):1-3(2009)
    [10] M. Y. Huang, S. Wang, J. Qiu et al, Chin. Phys. C, 37 (6):067001(2013)
    [11] M. Y. Huang, Chin. Phys. C, 40(6):063002(2016)
    [12] J. R. Wilson, Numerical Astrophysics, edited by J. M. Centrella, J. M. LeBlanc, and R. L. Bowers (Boston:Jones and Bartlett, 1985), p. 422-434
    [13] R. C. Schirato and G. M. Fuller, arXiv:astro-ph/0205390
    [14] L. Hudepohl, B. Muller, H. T. Janka et al, Phys. Rev. Lett., 104:251101(2010)
    [15] S. Sarikas, G. G. Raffelt, L. Hudepohl et al, Phys. Rev. Lett., 108:061101(2012)
    [16] L. Wolfenstein, Phys. Rev. D, 17:2369-2374(1978)
    [17] S. P. Mikheyev and A. Y. Smirnov, Sov. J. Nucl. Phys., 42:913-917(1985)
    [18] T. K. Kuo and J. Pantaleone, Rev. Mod. Phys., 61:937-979(1989)
    [19] M. Blennow and A. Y. Smirnov, Adv. High Energy Phys., 2013:972485(2013)
    [20] B. Dasgupta, A. Dighe and A. Mirizzi, Phys. Rev. Lett., 101:171801(2008)
    [21] H. Y. Duan, G. M. Fuller and J. Carlson, Comp. Scie. Disc., 1:015007(2008)
    [22] H. Y. Duan, G. M. Fuller and Y. Z. Qian, Ann. Rev. Nucl. Part. Sci., 60:569-594(2010)
    [23] A. S. Dighe and A. Y. Smirnov, Phys. Rev. D, 62:033007(2000)
    [24] A. N. Ioannisian and A. Y. Smirnov, Phys. Rev. Lett., 93:241801(2004)
    [25] X. H. Guo, M. Y. Huang and B. L. Young, Phys. Rev. D, 79:113007(2009)
    [26] M. Y. Huang, X. H. Guo and B. L. Young, Phys. Rev. D, 82:033011(2010)
    [27] P. Antonioli, R. T. Fienberg, F. Fleurot et al, New J. Phys., 6:114(2004)
    [28] T. Totani, K. Sato, H. E. Dalhed et al, Astrophys. J., 496, 216-225(1998)
    [29] M. T. Keil, G. G. Raffelt and H. T. Janka, Astrophys. J., 590, 971-991(2003)
    [30] C. Giunti and C. W. Kim, Fundamentals of Neutrino Physics and Astrophysics (New York:Oxford, 2007), p. 511-539
    [31] R. N. Mohapatra and P. B. Pal, Massive Neutrino in Physics and Astrophysics (Singapore:World Scientific, 2004), p. 340-358
    [32] H. T. Janka and W. Hillebrandt, Astron. Astrophys., 224, 49-56(1989)
    [33] H. T. Janka and W. Hillebrandt, Astron. Astrophys. Suppl. Ser., 78:375-397(1989)
    [34] S. Chakraborty, S. Choubey, S. Goswami et al, J. Cosmol. Astropart. Phys., 1006:007(2010)
    [35] L. Cadonati, F. P. Calaprice and M C. Chen, Astropart. Phys., 16:361-372(2002)
    [36] J. Arafune and M. Fukugita, Phys. Rev. Lett., 59:367-369(1987)
    [37] M. Fukugita, Y. Kohyama and K. Kubodera, Phys Lett. B, 212:139-144(1988)
    [38] E. Kolbe, K. Langanke and P. Vogel, Nucl. Phys. A, 652:91-100(1999)
    [39] C. Athanassopulos, L. B. Auerbach, D. A. Bauer et al, Phys. Rev. Lett., 75:2650-2653(1995)
    [40] C. Athanassopulos, L. B. Auerbach, R. L. Burman et al, Phys. Rev. C, 54:2685-2708(1996)
    [41] R. C. Allen, H. H. Chen, P. J. Doe et al, Phys. Rev. D, 47:11-28(1993)
    [42] R. Imlay and G. J. VanDalen, J. Phys. G:Nucl. Part. Phys., 29:2647-2664(2003)
    [43] L. B. Auerbach, R. L. Burman, D. O. Caldwell et al, Phys. Rev. D, 66:015501(2002)
    [44] X. H. Guo et al (Daya Bay Collaboration), arXiv:hep-ex/0701029
    [45] K. Nakazato, Phys. Rev. D, 88:083012(2013)
    [46] H. Zhang, K. Abe, Y. Hayato et al, Astropart. Phys., 60:41-46(2015)
    [47] G. J. VanDalen, arXiv:nucl-ex/0309014
    [48] K. A. Olive, K. Agashe, C. Amsler et al, Chin. Phys. C, 38(9):090001(2014)
    [49] F. Gapozzi, G. L. Fogli, E. Lisi et al, Phys. Rev. D, 89:093018(2014)
    [50] I. Tamborra, G. G. Raffelt, F. Hanke et al, Phys. Rev. D, 90:045032(2014)
    [51] R. L. Burman and W. C. Louis, J. Phys. G:Nucl. Part. Phys., 29:2499-2512(2003)
    [52] C. Athanassopoulos, L. B. Auerbach, D. Bauer et al, Nucl. Instrum. Methods Phys. Res. A, 388:149-172(1997)
    [53] G. Drexlin, V. Eberhard, H. Gemmeke et al, Nucl. Instrum. Methods Phys. Res. A, 289:490-495(1990)
    [54] R. L. Burman, A. C. Dodd and P. Plischke, Nucl. Instrum. Methods Phys. Res. A, 368:416-424(1996)
    [55] B. Boardman, Spallation Neutron Source:Description of Accelerator and Target, RL-82-006, 1982
    [56] SNS Project Team, Spallation Neutron Source Design Manual, June, 1998
    [57] Boardman B. Spallation Neutron Source: Description of Accel-erator and Target. RL-82-006, 1982
    [58] ESS Central Project Team, ESS Technical Design Report, ESS-doc-274-v15, 2015
    [59] SNS Project Team. Spallation Neutron Source Design Manual. June, 1998
    [60] ESS Central Project Team. ESS Technical Design Report. ESS-doc-274-v15, 2015
    [61] M. Elnimr, I. Stancu, M. Yeh et al, arXiv:1307.7097
    [62] E. Baussan, M. Blennow, M. Bogomilov et al, Nucl. Phys. B, 885:127-149(2014)
    [63] Elnimr M, Stancu I, Yeh M et al. The OscSNS White Paper. arXiv:1307.7097 [physics.ins-det]
    [64] Baussan E, Blennow M, Bogomilov M et al. Nucl. Phys. B,2014, 885: 127-149
    [65] E. Kolbe, K. Langanke and P. Vogel, Phys. Rev. D, 66:013007(2002)
    [66] Kolbe E, Langanke K, Vogel P. Phys. Rev. D, 2002, 66: 013007
    [67] K. Langanke, P. Vogel and E. Kolbe, Phys. Rev. Lett., 76:2629-2632(1996)
    [68] Langanke K, Vogel P, Kolbe E. Phys. Rev. Lett., 1996, 76:2629-2632
    [69] S. Nussinov and R. Shrock, Phys. Rev. Lett., 86:2223-2226(2001) 1996, 368: 416-424
    [70] Nussinov S, Shrock R. Phys. Rev. Lett., 2001, 86: 2223-2226

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Ming-Yang Huang, Xin-Heng Guo and Bing-Lin Young. Detection of supernova neutrinos at spallation neutron sources[J]. Chinese Physics C, 2016, 40(7): 073102. doi: 10.1088/1674-1137/40/7/073102
Ming-Yang Huang, Xin-Heng Guo and Bing-Lin Young. Detection of supernova neutrinos at spallation neutron sources[J]. Chinese Physics C, 2016, 40(7): 073102.  doi: 10.1088/1674-1137/40/7/073102 shu
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Received: 2015-11-05
Revised: 2016-02-06
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    Supported by National Natural Science Foundation of China (11205185, 11175020, 11275025, 11575023)

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Detection of supernova neutrinos at spallation neutron sources

    Corresponding author: Ming-Yang Huang,
    Corresponding author: Xin-Heng Guo,
    Corresponding author: Bing-Lin Young,
  • Received Date: 2015-11-05
  • Accepted Date: 2016-02-06
  • Available Online: 2016-07-05
Fund Project:  Supported by National Natural Science Foundation of China (11205185, 11175020, 11275025, 11575023)

Abstract: After considering supernova shock effects, Mikheyev-Smirnov-Wolfenstein effects, neutrino collective effects, and Earth matter effects, the detection of supernova neutrinos at the China Spallation Neutron Source is studied and the expected numbers of different flavor supernova neutrinos observed through various reaction channels are calculated with the neutrino energy spectra described by the Fermi-Dirac distribution and the "beta fit" distribution respectively. Furthermore, the numerical calculation method of supernova neutrino detection on Earth is applied to some other spallation neutron sources, and the total expected numbers of supernova neutrinos observed through different reactions channels are given.

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