Impact factor of Chinese Physics C is 3.6 in 2023 Impact factor of Chinese Physics C is 3.6 in 2022 2021 Impact Factor 2.944
Advanced Search
×
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
Chinese Physics C> 2018, Vol. 42> Issue(7) : 075103 DOI: 10.1088/1674-1137/42/7/075103

On the knee of Galactic cosmic rays in light of sub-TeV spectral hardenings

  • 1.

     Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210008, China

  • 2.

     Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China

  • 3.

     School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026, China

  • More than fifty years after the discovery of the knee in the cosmic ray (CR) spectra, its physical origin remains a mystery. This is partly due to the ambiguity of the energy spectra of individual components. Recently, direct measurements from several space experiments found significant spectral hardenings of CR nuclei at ~200 GV. A joint modeling of the direct and indirect measurements may help to understand the experimental systematics and the physics of the knee. In this work, we update the phenomenological "poly-gonato" model to include the spectral hardenings, with a changing spectral index of γ + β·logE. This modification gives a reasonable description of the CR spectra in a wide energy range. However, the fits to different data sets give different results. We find that the fit to the AMS-02 and CREAM data slightly favors a relatively low energy knee of the light components. In such a case, the expected all-particle spectra under-shoot the data, which may require an extra component of CRs. The fits to AMS-02 data and the light component (H+He) data from the Tibet ASγ/ARGO-YBJ/WFCTA and KASCADE experiments give consistent results with the all-particle spectra. We further propose a possible physical realization of such a "modified poly-gonato" model of spectral hardenings by means of spatially-dependent diffusion of CRs. We find reasonably good agreement between the model predictions and the data for CR spectra, the secondary-to-primary ratios, and the amplitude of anisotropies.
      PCAS:
  • 加载中

  • References

    [1] G. V. Kulikov and G. B. Kristiansen, J. Exp. Theor. Phys., 35:635 (1958)
    [2] J. R. Hrandel, Astroparticle Physics, 21: 241265 (2004)
    [3] J. R. Hrandel, Astroparticle Physics, 19: 193220 (2003)
    [4] P. O. Lagage and C. J. Cesarsky, Astron. Astrophys., 125: 249257 (1983)
    [5] H. J. Voelk and P. L. Biermann, Astrophys. J. Lett., 333: L65 L68 (1988)
    [6] V. S. Ptuskin, S. I. Rogovaya, V. N. Zirakashvili et al, Astron. Astrophys., 268: 726735 (1993)
    [7] E. G. Berezhko, Astroparticle Physics, 5: 367378 (1996)
    [8] B. Wiebel-Sooth, P. L. Biermann, and H. Meyer, Astron. Astrophys., 330: 389398 (1998)
    [9] S. Karakula and W. Tkaczyk, Astroparticle Physics, 1: 229237 (1993)
    [10] J. Candia, L. N. Epele, and E. Roulet, Astroparticle Physics, 17: 2333 (2002)
    [11] D. Kazanas and A. Nicolaidis, International Cosmic Ray Conference, 5: 1760 (2001)
    [12] H.-B. Hu, Q. Yuan, B. Wang et al, Astrophys. J. Lett., 700:L170L173 (2009)
    [13] B. Wang, Q. Yuan, C. Fan et al, Science China Physics, Mechanics, and Astronomy, 53: 842847 (2010)
    [14] Y.-Q. Guo, Z.-Y. Feng, Q. Yuan, C. Liu, and H.-B. Hu, New Journal of Physics, 15(1): 013053 (2013)
    [15] J. Huang, Primary proton and helium spectra at energy range from 50 TeV to 1PeV observed with (YAC+Tibet-Ⅲ ) hybrid experiment, International Cosmic Ray Conference, 2013
    [16] W. D. Apel, J. C. Arteaga-Velzquez, K. Bekk et al, Astroparticle Physics, 47: 5466 (2013)
    [17] S. M. Mari, P. Montini, and for the ARGO-YBJ Collaboration, Phys. Rev. D, 91: 112017 (2015)
    [18] B. Bartoli, P. Bernardini, X. J. Bi et al, Phys. Rev. D, 92(9):092005 (2015)
    [19] A. DAmone, I. De Mitri, and A. Surdo, Measurement of the cosmic ray all-particle and light-component energy spectra with the ARGO-YBJ experiment, arXiv:1502.04840
    [20] P. Montini and S. M. Mari, The bending of the proton plus helium flux in primary cosmic rays measured by the ARGOYBJ experiment in the energy range from 20 TeV to 5 PeV, arXiv:1608.01389
    [21] M. Shibata, Y. Katayose, J. Huang, and D. Chen, Astrophys. J., 716: 10761083 (2010)
    [22] Y. Zhao, H.-Y. Jia, and F.-R. Zhu, Chinese Physics C, 39(12):125001 (2015)
    [23] S. Thoudam, J. P. Rachen, A. van Vliet et al, Astron. Astrophys., 595: A33 (2016)
    [24] A. D. Panov, J. H. Adams, Jr., H. S. Ahn et al, Bulletin of the Russian Academy of Science, Phys., 71: 494497 (2007)
    [25] H. S. Ahn, P. Allison, M. G. Bagliesi et al, Astrophys. J. Lett., 714: L89L93 (2010)
    [26] O. Adriani, G. C. Barbarino, G. A. Bazilevskaya et al, Science, 332: 69 (2011)
    [27] M. Aguilar, D. Aisa, B. Alpat et al, Physical Review Letters, 114(17): 171103 (2015)
    [28] M. Aguilar, D. Aisa, B. Alpat et al, Physical Review Letters, 115(21): 211101 (2015)
    [29] V. I. Zatsepin and N. V. Sokolskaya, Astron. Astrophys., 458: 15 (2006)
    [30] Q. Yuan, B. Zhang, and X.-J. Bi, Phys. Rev. D, 84(4): 043002 (2011)
    [31] S. Thoudam and J. R. Hrandel, Mon. Not. Roy. Astron. Soc., 421: 12091214 (2012)
    [32] P. L. Biermann, J. K. Becker, J. Dreyer et al, Astrophys. J., 725: 184187 (2010)
    [33] V. Ptuskin, V. Zirakashvili, and E.-S. Seo, Astrophys. J., 763:47 (2013)
    [34] S. Thoudam and J. R. Hrandel, Astron. Astrophys., 567: A33 (2014)
    [35] N. Tomassetti, Astrophys. J. Lett., 752: L13 (2012)
    [36] D. Gaggero, D. Grasso, A. Marinelli, A. Urbano, and M. Valli, Astrophys. J. Lett., 815: L25 (2015)
    [37] N. Tomassetti, Phys. Rev. D, 92(8): 081301 (2015)
    [38] C. Jin, Y.-Q. Guo, and H.-B. Hu, Chinese Physics C, 40(1):015101 (2016)
    [39] Y. Q. Guo, H. B. Hu, and Z. Tian, Chinese Physics C, 40:115001 (2016)
    [40] Y.-Q. Guo, Z. Tian, and C. Jin, Astrophys. J., 819: 54 (2016)
    [41] J. Feng, N. Tomassetti, and A. Oliva, Phys. Rev. D, 94(12):123007 (2016)
    [42] J. J. Engelmann, P. Ferrando, A. Soutoul, P. Goret, and E. Juliusson, Astron. Astrophys., 233: 96111 (1990)
    [43] Y. S. Yoon, T. Anderson, A. Barrau et al, Astrophys. J., 839:5 (2017)
    [44] M. Ave, P. J. Boyle, F. Gahbauer et al, Astrophys. J., 678: 262273 (2008)
    [45] A. D. Panov, J. H. Adams, H. S. Ahn et al, Bulletin of the Russian Academy of Sciences, Physics, 73: 564567 (2009)
    [46] H. S. Ahn, P. Allison, M. G. Bagliesi et al, Astrophys. J., 707: 593603 (2009)
    [47] M. Amenomori, X. J. Bi, D. Chen et al, Astrophys. J., 678: 11651179 (2008)
    [48] M. Nagano, T. Hara, Y. Hatano et al, Journal of Physics G Nuclear Physics, 10: 12951310 (1984)
    [49] N. Tomassetti, Phys. Rev. D, 92(6): 063001 (2015)
    [50] A. W. Strong, I. V. Moskalenko, and V. S. Ptuskin, Annual Review of Nuclear and Particle Science, 57: 285327 (2007)
    [51] Q. Yuan, S.-J. Lin, K. Fang, and X.-J. Bi, Phys. Rev. D, 95(8):083007 (2017)
    [52] E. S. Seo and V. S. Ptuskin, Astrophys. J., 431: 705714 (1994)
    [53] C. Evoli, D. Gaggero, D. Grasso, and L. Maccione, Journal of Cosmology and Astroparticle Physics, 10: 18 (2008)
    [54] L. J. Gleeson and W. I. Axford, Astrophys. J., 154: 1011 (1968)
    [55] AMS-02 collaboration, Talks at the AMS Days at CERN, 15-17 April, 2015
    [56] O. Adriani, G. C. Barbarino, G. A. Bazilevskaya et al, Physics Reports, 544: 323 (2014)
    [57] A. J. Davis, R. A. Mewaldt, W. R. Binns et al, On the low energy decrease in galactic cosmic ray secondary/primary ratios, In R. A. Mewaldt, J. R. Jokipii, M. A. Lee, E. Mbius, and T. H. Zurbuchen, editors, Acceleration and Transport of Energetic Particles Observed in the Heliosphere, volume 528 of American Institute of Physics Conference Series, pages 421 424, September 2000
    [58] V. A. Derbina, V. I. Galkin, M. Hareyama et al, Astrophys. J. Lett., 628: L41L44 (2005)
    [59] M. Amenomori and et al, International Cosmic Ray Conference, 2015
    [60] M. Ahlers, Deciphering the Dipole Anisotropy of Galactic Cosmic Rays, Physical Review Letters, 117: 151103 (2016)
    [61] T. Thambyahpillai, International Cosmic Ray Conference, 3:383 (1983)
    [62] D. B. Swinson and K. Nagashima, Planet. Space Sci., 33: 10691072 (1985)
    [63] K. Munakata, S. Yasue, S. Mori et al, International Cosmic Ray Conference, 4: 639 (1995)
    [64] K. B. Fenton, A. G. Fenton, and J. E. Humble, International Cosmic Ray Conference, 4: 635 (1995)
    [65] M. Amenomori, S. Ayabe, X. J. Bi et al, Science, 314: 439443 (2006)
    [66] R. Abbasi, Y. Abdou, T. Abu-Zayyad et al, Astrophys. J., 746:33 (2012)
    [67] B. Bartoli, P. Bernardini, X. J. Bi et al, Astrophys. J., 809: 90 (2015)
    [68] T. K. Gaisser, T. Stanev, and S. Tilav, Frontiers of Physics, 8: 748758 (2013)
    [69] CALET Collaboration, Nuclear Physics B Proceedings Supplements, 166: 4349 (2007)
    [70] J. Chang et al, Astropart. Phys., 95: 6 (2017)
    [71] Z. Cao, Chinese Physics C, 34: 249252 (2010)

  • Access

    加载中

Get Citation
Yi-Qing Guo and Qiang Yuan. On the knee of Galactic cosmic rays in light of sub-TeV spectral hardenings[J]. Chinese Physics C, 2018, 42(7): 075103. doi: 10.1088/1674-1137/42/7/075103
Yi-Qing Guo and Qiang Yuan. On the knee of Galactic cosmic rays in light of sub-TeV spectral hardenings[J]. Chinese Physics C, 2018, 42(7): 075103.  doi: 10.1088/1674-1137/42/7/075103 shu
Milestone
Received: 2018-03-14
Fund

    Supported by National Key Research and Development Program of China (2016YFA0400200), the National Natural Science Foundation of China (11635011, 11761141001, 11663006, 11722328) and the 100 Talents program of Chinese Academy of Sciences

Article Metric

Article Views(1738)
PDF Downloads(16)
Cited by(0)
Policy on re-use
To reuse of subscription content published by CPC, the users need to request permission from CPC, unless the content was published under an Open Access license which automatically permits that type of reuse.
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:

On the knee of Galactic cosmic rays in light of sub-TeV spectral hardenings

  • 1. Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210008, China
  • 2. Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China
  • 3. School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026, China
  • Received Date: 2018-03-14
  • Available Online: 2018-07-05
Fund Project:  Supported by National Key Research and Development Program of China (2016YFA0400200), the National Natural Science Foundation of China (11635011, 11761141001, 11663006, 11722328) and the 100 Talents program of Chinese Academy of Sciences

Abstract: More than fifty years after the discovery of the knee in the cosmic ray (CR) spectra, its physical origin remains a mystery. This is partly due to the ambiguity of the energy spectra of individual components. Recently, direct measurements from several space experiments found significant spectral hardenings of CR nuclei at ~200 GV. A joint modeling of the direct and indirect measurements may help to understand the experimental systematics and the physics of the knee. In this work, we update the phenomenological "poly-gonato" model to include the spectral hardenings, with a changing spectral index of γ + β·logE. This modification gives a reasonable description of the CR spectra in a wide energy range. However, the fits to different data sets give different results. We find that the fit to the AMS-02 and CREAM data slightly favors a relatively low energy knee of the light components. In such a case, the expected all-particle spectra under-shoot the data, which may require an extra component of CRs. The fits to AMS-02 data and the light component (H+He) data from the Tibet ASγ/ARGO-YBJ/WFCTA and KASCADE experiments give consistent results with the all-particle spectra. We further propose a possible physical realization of such a "modified poly-gonato" model of spectral hardenings by means of spatially-dependent diffusion of CRs. We find reasonably good agreement between the model predictions and the data for CR spectra, the secondary-to-primary ratios, and the amplitude of anisotropies.

    HTML

Reference (71)

目录

Link
IOPScience
SCOAP3
arXiv
Chinese Physical Society
Journal information
Introduction
Editorial Board
Others
Subscribe
Contact us
QQ: 1307685413
Tel: +86-010-88235947
Fax: +86-010-88233126
E-mail: cpc@ihep.ac.cn

  • CPC Website

  • IOP Website

  • CPC WeChat

Copyright © Institute of High Energy Physics, Chinese Academy of Sciences, 19B Yuquan Road, Beijing 100049, China 京ICP备05002789号-1

Supported by: Beijing Renhe Information Technology Co. Ltd  E-mail: info@rhhz.net

/

DownLoad:  Full-Size Img  PowerPoint
Return
Return