A possible explanation of the knee of cosmic light component spectrum from 100 TeV to 3 PeV

Wen-Hui Lin; Bi-Wen Bao; Ze-Jun Jiang; Li Zhang

doi:10.1088/1674-1137/41/10/105101

Chinese Physics C> 2017, Vol. 41> Issue(10) : 105101 DOI: 10.1088/1674-1137/41/10/105101

A possible explanation of the knee of cosmic light component spectrum from 100 TeV to 3 PeV

1.
Department of Astronomy, Yunnan University, Key Laboratory of Astroparticle physics of Yunnan Province, Kunming 650091, China

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Abstract：
A mixed hydrogen and helium (H+He) spectrum with a clear steepening at 700 TeV has been detected by the ARGO-YBJ experiments. In this paper, we demonstrate that the observed H+He spectrum can be reproduced well with a model of cosmic rays escaping from the supernova remnants (SNRs) in our Galaxy. In this model, particles are accelerated in a SNR through a non-linear diffusive shock acceleration mechanism. Three components of high energy light nuclei escaped from the SNR are considered. It should be noted that the proton spectrum observed by KASCADE can be also explained by this model given a higher acceleration efficiency.
- cosmic Rays ,
- particle acceleration ,
- supernova remnants ,
- amplified magnetic field

References

[1]	W. Baade, F. Zwicky, Physical Review, 46:76-77(1934)
[2]	V. A. Acciari, E. Aliu, T. Arlen et al, Astrophys. J., 730:L20(2011)
[3]	F. Giordano, M. Naumann-Godo, J. Ballet et al, Astrophys. J., 744:L2(2012)
[4]	J. Vink, Astron. Astrophys. Rev., 20:49(2012)
[5]	M. Ackermann, M. Ajello, A. Allafort et al, Science, 339:807(2013)
[6]	P. Blasi, Nuclear Physics B, 256, 36(2014)
[7]	B. Bartoli et al, Phys. Rev. D, 92, 092005(2015)
[8]	G. F. Krymskii, Akademiia Nauk SSSR Doklady, 234:1306-1308(1977)
[9]	R. D. Blandford, J. P. Ostriker, Astrophys. J., 221:L29-L32(1978)
[10]	W. I. Axford, E. Leer, G. Skadron, Proc. 15th. Int. Cosmic. Ray. Conf., 11:132(1977)
[11]	A. R. Bell, MON. Not. R. Astron. Soc., 182:147(1978)
[12]	M. A. Malkov L. Drury, Reports on Progress in Physics, 64:429(2001)
[13]	A. M. Bykov, D. C. Ellison, S. M. Osipov et al, Astrophys. J, 789:137(2014)
[14]	D. Caprioli, H. Kang, A. E. Vladimirov, T. W. Jones, Mon. Not. R. Astron. Soc, 407:1773(2010)
[15]	D. Caprioli, Journal of Cosmology and Astroparticle Physics, Issue 07, id. 038(2012)
[16]	T. Antoni et al, Astrophys. J., 24:1(2005)
[17]	W. D. Apel et al, Astrophys. J., 31:86(2009)
[18]	W. D. Apel et al, Astrophys. J., 47:54(2013)
[19]	D. Caprioli, E. Amato, P. Blasi, Astropart. Phys., 33:160(2010)
[20]	H. Kang, T. Jones U. Giedeler, Astrophys. J., 579:337(2002)
[21]	J. Fang L. Zhang, Chinese Physics Letters, 25:4486(2008)
[22]	J. K. Truelove C. F. McKee, Astrophys. J. Suppl. Ser., 120:299(2009)
[23]	J. R. Hrandel, N. K. Nikilai V. T. Alekesi, Astropart. Phys., 27:119(2007)
[24]	D. Caprioli, E. Amato, P. Blasi, Astropart. Phys., 34:447(2011)
[25]	B. Bartoli et al, Phys. Rev. D, 85:092005(2012)
[26]	B. Bartoli et al, CPC, 38:045001(2014)
[27]	M. Aguilar et al, Phys. Rev. Lett., 114:171103(2015)
[28]	M. Aguilar et al, Phys. Rev. Lett., 115:211101(2015)
[29]	O. Adriani et al, Sci. A, 332:69(2011)
[30]	Y. S. Yoon et al, Astrophys. J., 728:122(2011)
[31]	M. Amenomori et al, ASR, 47:629(2011)
[32]	V. S. Ptuskin, V. N. Zirakashvili E. S. Seo, Astrophys. J., 718:31(2010)
[33]	A. W. Strong I. V. Moskalenko, Astrophys. J., 509:212(1998)

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[12]	GUO Xin-Heng , HUANG Ming-Yang , Young Bing-Lin . Supernova neutrino detection on earth. Chinese Physics C, 2010, 34(2): 257-261. doi: 10.1088/1674-1137/34/2/020
[13]	YUAN Yi , LI Kang , WANG Jian-Hua , CHEN Chi-Yi . Spin-1/2 relativistic particle in a magnetic field in NC phase space. Chinese Physics C, 2010, 34(5): 543-547. doi: 10.1088/1674-1137/34/5/005
[14]	CHANG Zhe , LI Xin . Ultra-high energy cosmic rays threshold in Randers-Finsler space. Chinese Physics C, 2009, 33(8): 626-628. doi: 10.1088/1674-1137/33/8/005
[15]	Ding Linkai , Dai Benzhong , Feng Zhenyong , Huang Qing , Huo Anxiang , Jia Huanyu , Labaciren , Mei Dongming , Meng Lie , Meng Xianru , Mu Jun , Ren Jingru , Shi Zhizheng , Tan Youheng , Wang Hui , Yu Guangce , Zhaxiciren , Zhaxisanzhu , Zhou Wende , Zhang Chunsheng , Zhang Huimin . Search for 10 TeV Gamma-Ray Bursts with the Tibet Air Shower Array. Chinese Physics C, 1997, 21(S3): 9-16.
[16]	Xu Chunxian , Dai Hongyue . Statistic Model for Galactic Cosmic Rays. Chinese Physics C, 1997, 21(S2): 25-32.
[17]	Liu Shaomin , Ding Linkai , Shi Ce , Zhaxiciren , Zhaxisanzhu , Mu Jun , Wnag Hui , Lu Hong , Feng Zhenyong , Ren Jingru , Yu Guangce , Zhou Wende , Labaciren , Meng Xianru , Meng Lie , Zhang Jilong , Zhang Chunsheng , Zhang Huimin , Shi Zhizheng , Jia Huanyiu , Mei Dongming , Huang Qing , Tan Youheng , Huo Anxiang , Dai Benzhong . Correlation Between Sun Shadows of 10 TeV Cosmic Ray and the Solar Activity. Chinese Physics C, 1997, 21(S4): 11-18.
[18]	Luo Guangxuan , Tan Youheng , Zhang Chunsheng , Dong Yuju , Yuan Peng , Zhang Huimin , Wang Hui , Yuang Yukui , Li Jing . Energy Spectrum of Primary Cosmic Rays at the “Knee” Region Observed with the Huairou Air Shower Array. Chinese Physics C, 1995, 19(S4): 325-331.
[19]	Chen Fengzhi , Nie Chuanhui . The Origin of Anomalous Hard Positrons in the Cosmic Rays Above 10 GeV. Chinese Physics C, 1991, 15(S3): 259-264.
[20]	Zhang Naijian , Wang Chengrui , He Mao , Cao Peiyuan , Li Jinyu , Zou Baotangj Wang Guangjun , Wei Chao . High Energy Hadrons in Atmospheric Cosmic Rays Observed with Fe Emulsion Chambers. Chinese Physics C, 1989, 13(S4): 357-362.

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Wen-Hui Lin, Bi-Wen Bao, Ze-Jun Jiang and Li Zhang. A possible explanation of the knee of cosmic light component spectrum from 100 TeV to 3 PeV[J]. Chinese Physics C, 2017, 41(10): 105101. doi: 10.1088/1674-1137/41/10/105101

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Received: 2017-05-04
Revised: 2017-07-03

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Supported by the National Natural Science Foundation of China (11433004, 11363006, 11103016, 11173020), Top Talents Program of Yunnan Province (2015HA030) and the Natural Science Foundation of Yunnan Province(2015FB103)

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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

A possible explanation of the knee of cosmic light component spectrum from 100 TeV to 3 PeV

Corresponding author: Ze-Jun Jiang,

Corresponding author: Li Zhang,

1. Department of Astronomy, Yunnan University, Key Laboratory of Astroparticle physics of Yunnan Province, Kunming 650091, China

Received Date: 2017-05-04

Accepted Date: 2017-07-03

Available Online: 2017-10-05

Fund Project: Supported by the National Natural Science Foundation of China (11433004, 11363006, 11103016, 11173020), Top Talents Program of Yunnan Province (2015HA030) and the Natural Science Foundation of Yunnan Province(2015FB103)

Abstract: A mixed hydrogen and helium (H+He) spectrum with a clear steepening at 700 TeV has been detected by the ARGO-YBJ experiments. In this paper, we demonstrate that the observed H+He spectrum can be reproduced well with a model of cosmic rays escaping from the supernova remnants (SNRs) in our Galaxy. In this model, particles are accelerated in a SNR through a non-linear diffusive shock acceleration mechanism. Three components of high energy light nuclei escaped from the SNR are considered. It should be noted that the proton spectrum observed by KASCADE can be also explained by this model given a higher acceleration efficiency.

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A possible explanation of the knee of cosmic light component spectrum from 100 TeV to 3 PeV

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