Spatial dependent diffusion of cosmic rays and the excess of primary electrons derived from high precision measurements by AMS-02

Chao Jin; Yi-Qing Guo; Hong-Bo Hu

doi:10.1088/1674-1137/40/1/015101

Chinese Physics C> 2016, Vol. 40> Issue(1) : 015101 DOI: 10.1088/1674-1137/40/1/015101

Spatial dependent diffusion of cosmic rays and the excess of primary electrons derived from high precision measurements by AMS-02

Chao Jin ^1,2,, ,
Yi-Qing Guo ² ,
Hong-Bo Hu ²

1.
School of Physical Engineering, Zhengzhou University, Zhengzhou 450001, China
2.
Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China
3.
Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China

Abstract
HTML
Reference
Related

PDF

Abstract：
The precise spectra of Cosmic Ray (CR) electrons and positrons have been published by the measurement of AMS-02. It is reasonable to regard the difference between the electron and positron spectra (ΔΦ= Φ_e^--Φ_e⁺) as being dominated by primary electrons. The resulting electron spectrum shows no sign of spectral softening above 20 GeV, which is in contrast with the prediction of the standard model of CR propagation. In this work, we generalize the analytic one-dimensional two-halo model of diffusion to a three-dimensional realistic calculation by implementing spatial variant diffusion coefficients in the DRAGON package. As a result, we can reproduce the spectral hardening of protons observed by several experiments, and predict an excess of high energy primary electrons which agrees with the measurement reasonably well. Unlike the break spectrum obtained for protons, the model calculation predicts a smooth electron excess and thus slightly over-predicts the flux from tens of GeV to 100 GeV. To understand this issue, further experimental and theoretical studies are necessary.
- cosmic rays ,
- primary electron ,
- excess ,
- diffusion ,
- propagation ,
- hardening

References

[1]	M. Aguilar, G. Alberti, B. Alpat et al, Phys. Rev. Lett., 110: 141102 (2013)
[2]	O. Adriani, G. C. Barbarino, G. A. Bazilevskaya et al, Nature, 458: 607-609 (2009)
[3]	L. Bergstrm, T. Bringmann, and J. Edsj, Phys. Rev. D, 78: 103520 (2008)
[4]	V. Barger, W. Y. Keung, D. Marfatia et al, Phy. Lett. B, 672: 141-146 (2009)
[5]	D. Hooper, P. Blasi, and P. Dario Serpico. JCAP, 1: 25 (2009)
[6]	H. Yksel, M. D. Kistler, and T. Stanev, Phy. Rev. Lett., 103: 051101 (2009)
[7]	P. Blasi, Phy. Rev. Lett., 103: 051104 (2009)
[8]	M. Ahlers, P. Mertsch, and S. Sarkar, Phy. Rev. D, 80: 123017 (2009)
[9]	H. B. Hu, Q. Yuan, B. Wang et al, ApJ, 700: L170-L173 (2009)
[10]	B. Wang, Q. Yuan, C. Fan et al, Science China Physics, Mechanics, and Astronomy, 53: 842 (2010)
[11]	X. Li, Z. Q. Shen, B. Q. Lu et al, arXiv:1412.1550
[12]	Q. Yuan and X. J. Bi, Phys. Lett. B, 727: 1-7 (2013)
[13]	S. J. Lin, Q. Yuan, and X. J. Bi, Phys. Rev. D, 91: 063508 (2015)
[14]	A. D. Panov, J. H. Adams, H. S. Ahn et al, Bulletin of the Russian Academy of Science, Phys., 73: 564-567 (2009)
[15]	H. S. Ahn, P. S. Allison, M. G. Bagliesi et al, ApJ, 715: 1400-1407 (2010)
[16]	O. Adriani, G. C. Barbarino, G. A. Bazilevskaya et al, Science, 332: 69 (2011)
[17]	N. Tomassetti, ApJ, 752: L13 (2012)
[18]	D. Gaggero, D. Grasso, A. Marinelli et al, arXiv:1504.00227
[19]	P. L. Biermann, J. K. Becker, J. Dreyer et al, ApJ, 725: 184-187 (2010)
[20]	D. C. Ellison, E. G. Berezhko, and M. G. Baring, ApJ, 540: 292 (2000)
[21]	S. Thoudam and J. R. Hrandel, MNRAS, 421: 1209-1214 (2012)
[22]	S. Thoudam and J. R. Hrandel, AA, 567: A33 (2014)
[23]	A. D. Erlykin and A. W. Wolfendale, J. Phys. G: Nucl. Part. Phys., 28: 2329-2348 (2002)
[24]	C. Evoli, D. Gaggero, D. Grasso et al, JCAP, 10: 18 (2008)
[25]	E. S. Seo and V. S. Ptuskin, ApJ, 431: 705 (1994)
[26]	K. M. Ferrire, Reviews of Modern Physics, 73: 1031-1066 (2001)
[27]	C. Consolandi et al (AMS-02 Collaboration), arXiv:1402.0467
[28]	A. D. Panov, J. H. Adams, H. S. Ahn et al, arXiv:0612377
[29]	H. S. Ahn, P. Allison, M. G. Bagliesi et al, ApJ, 714: L89-L93 (2010)
[30]	T. Antoni, W. D. Apel, and A. F. Badea, Astroparticle Physics, 24: 1-25 (2005)
[31]	L. J. Gleeson and W. I. Axford, ApJ, 154: 1011 (1968)
[32]	L. Accardo, M. Aguilar, D. Aisa et al, Phys. Rev. Lett., 113: 121101 (2014)
[33]	M. Aguilar, D. Aisa, B. Alpat et al, Phys. Rev. Lett., 113: 221102 (2014)
[34]	C. S. Shen, ApJ, 162: L181 (1970)
[35]	T. Kobayashi, Y. Komori, K. Yoshida et al, ApJ, 601: 340-351 (2004)
[36]	N. J. Shaviv, E. Nakar, and T. Piran, Phy. Rev. Lett., 103: 111302 (2009)
[37]	Y. Q. Guo, H. B. Hu, and Z. Tian, arXiv:1412.8590

[1]	G.R. Boroun . Non-linear corrections to the derivative of nuclear reduced cross-section at small x at a future electron-ion collider. Chinese Physics C, 2026, 50(2): 1-10.
[2]	Li Tang , Liang Liu , Ying Wu . Null test of cosmic curvature using deep learning method. Chinese Physics C, 2026, 50(2): 1-8.
[3]	Zetian Li , Ning Liu , Bin Zhu . Interplay of 95 GeV Diphoton Excess and Dark Matter in Supersymmetric Triplet Model. Chinese Physics C, 2026, 50(3): 1-11.
[4]	Minghui Ding , Fei Gao , Sebastian M. Schmidt . Anisotropic quark propagation and Zeeman effect in an external magnetic field. Chinese Physics C, 2026, 50(2): 1-19.
[5]	Shi-Qi Ling , Zhao-Huan Yu . Imprints of an early matter-dominated era arising from dark matter dilution mechanism on cosmic string dynamics and gravitational wave signatures. Chinese Physics C, 2025, 49(10): 105105. doi: 10.1088/1674-1137/addcd6
[6]	Fan Yang , Xiangyun Fu , Bing Xu , Kaituo Zhang , Yang Huang , Ying Yang . Testing the cosmic distance duality relation using Type Ia supernovae and radio quasars through model-independent methods. Chinese Physics C, 2025, 49(10): 105108. doi: 10.1088/1674-1137/ade4a3
[7]	HUANG Jiang , XIONG Yong-Qian , CHEN De-Zhi , LIU Kai-Feng , YANG Jun , LI Dong , YU Tiao-Qin , FAN Ming-Wu , YANG Bo . A permanent magnet electron beam spread system used fora low energy electron irradiation accelerator. Chinese Physics C, 2014, 38(10): 107008. doi: 10.1088/1674-1137/38/10/107008
[8]	LIU Chang-Long , LU Yi-Ying , YIN LI . Effects of Additional Vacancy-Like Defects Produced by Ion Impealations on Boron Thermal Diffusion in Silicon. Chinese Physics C, 2005, 29(11): 1107-1111.
[9]	Sa Ben-hao , Zhang Xi-zhen , Li Zhu-xia , Shi Yi-jin . A PRIMARY RESEARCH OF THE PHONON RENORMALIZATION OF NUCLEAR FIELD THEORY. Chinese Physics C, 1980, 4(3): 398-400.
[10]	CHANG KONG-LIANG . DIMENSIONAL METHOD TO SOLVE THE DIFFUSION CONVECTION EQUATION OF SOLAR COSMIC RAYS. Chinese Physics C, 1978, 2(3): 200-210.

Access

Get Citation

Chao Jin, Yi-Qing Guo and Hong-Bo Hu. Spatial dependent diffusion of cosmic rays and the excess of primary electrons derived from high precision measurements by AMS-02[J]. Chinese Physics C, 2016, 40(1): 015101. doi: 10.1088/1674-1137/40/1/015101

RIS(for EndNote,Reference Manager,ProCite)

BibTex

Txt

Milestone

Received: 2015-04-30
Revised: 2015-09-02

Fund

Supported by Natural Sciences Foundation of China (11135010)

Article Metric

Article Views(2998)
PDF Downloads(134)
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

Spatial dependent diffusion of cosmic rays and the excess of primary electrons derived from high precision measurements by AMS-02

Corresponding author: Chao Jin,

1. School of Physical Engineering, Zhengzhou University, Zhengzhou 450001, China

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

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

Received Date: 2015-04-30

Accepted Date: 2015-09-02

Available Online: 2016-01-20

Fund Project: Supported by Natural Sciences Foundation of China (11135010)

Abstract: The precise spectra of Cosmic Ray (CR) electrons and positrons have been published by the measurement of AMS-02. It is reasonable to regard the difference between the electron and positron spectra (ΔΦ= Φ_e^--Φ_e⁺) as being dominated by primary electrons. The resulting electron spectrum shows no sign of spectral softening above 20 GeV, which is in contrast with the prediction of the standard model of CR propagation. In this work, we generalize the analytic one-dimensional two-halo model of diffusion to a three-dimensional realistic calculation by implementing spatial variant diffusion coefficients in the DRAGON package. As a result, we can reproduce the spectral hardening of protons observed by several experiments, and predict an excess of high energy primary electrons which agrees with the measurement reasonably well. Unlike the break spectrum obtained for protons, the model calculation predicts a smooth electron excess and thus slightly over-predicts the flux from tens of GeV to 100 GeV. To understand this issue, further experimental and theoretical studies are necessary.

HTML

Reference (37)

Spatial dependent diffusion of cosmic rays and the excess of primary electrons derived from high precision measurements by AMS-02

Abstract：

References

Access

Article Metrics

Metrics

通讯作者: 陈斌, bchen63@163.com

Email This Article