×
近期发现有不法分子冒充我刊与作者联系,借此进行欺诈等不法行为,请广大作者加以鉴别,如遇诈骗行为,请第一时间与我刊编辑部联系确认(《中国物理C》(英文)编辑部电话:010-88235947,010-88236950),并作报警处理。
本刊再次郑重声明:
(1)本刊官方网址为cpc.ihep.ac.cn和https://iopscience.iop.org/journal/1674-1137
(2)本刊采编系统作者中心是投稿的唯一路径,该系统为ScholarOne远程稿件采编系统,仅在本刊投稿网网址(https://mc03.manuscriptcentral.com/cpc)设有登录入口。本刊不接受其他方式的投稿,如打印稿投稿、E-mail信箱投稿等,若以此种方式接收投稿均为假冒。
(3)所有投稿均需经过严格的同行评议、编辑加工后方可发表,本刊不存在所谓的“编辑部内部征稿”。如果有人以“编辑部内部人员”名义帮助作者发稿,并收取发表费用,均为假冒。
                  
《中国物理C》(英文)编辑部
2024年10月30日

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.
      PCAS:
  • 加载中
  • [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
  • 加载中

Get Citation
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
Milestone
Received: 2015-11-05
Revised: 2016-02-06
Fund

    Supported by National Natural Science Foundation of China (11205185, 11175020, 11275025, 11575023)

Article Metric

Article Views(1815)
PDF Downloads(615)
Cited by(0)
Policy on re-use
To reuse of Open Access content published by CPC, for content published under the terms of the Creative Commons Attribution 3.0 license (“CC CY”), the users don’t need to request permission to copy, distribute and display the final published version of the article and to create derivative works, subject to appropriate attribution.
通讯作者: 陈斌, bchen63@163.com
  • 1. 

    沈阳化工大学材料科学与工程学院 沈阳 110142

  1. 本站搜索
  2. 百度学术搜索
  3. 万方数据库搜索
  4. CNKI搜索

Email This Article

Title:
Email:

Detection of supernova neutrinos at spallation neutron sources

    Corresponding author: Ming-Yang Huang,
    Corresponding author: Xin-Heng Guo,
    Corresponding author: Bing-Lin Young,
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.

    HTML

Reference (70)

目录

/

DownLoad:  Full-Size Img  PowerPoint
Return
Return