Probe of the Solar Magnetic Field Using the "Cosmic-Ray Shadow" of the Sun

被引：36

作者：

Amenomori, M. ^{[1
]}

Bi, X. J. ^{[2
]}

Chen, D. ^{[3
]}

Chen, T. L. ^{[4
]}

Chen, W. Y. ^{[2
]}

Cui, S. W. ^{[5
]}

Danzengluobu ^{[4
]}

Ding, L. K. ^{[2
]}

Feng, C. F. ^{[6
]}

Feng, Zhaoyang ^{[2
]}

Feng, Z. Y. ^{[7
]}

Gou, Q. B. ^{[2
]}

Guo, Y. Q. ^{[2
]}

Hakamada, K. ^{[8
]}

He, H. H. ^{[2
]}

He, Z. T. ^{[5
]}

Hibino, K. ^{[9
]}

Hotta, N. ^{[10
]}

Hu, Haibing ^{[4
]}

Hu, H. B. ^{[2
]}

Huang, J. ^{[2
]}

Jia, H. Y. ^{[7
]}

Jiang, L. ^{[2
]}

Kajino, F. ^{[11
]}

Kasahara, K. ^{[12
]}

Katayose, Y. ^{[13
]}

Kato, C. ^{[14
]}

Kawata, K. ^{[15
]}

Labaciren ^{[4
]}

Le, G. M. ^{[2
]}

Li, A. F. ^{[2
,6
,16
]}

Li, H. J. ^{[4
]}

Li, W. J. ^{[2
,7
]}

Liu, C. ^{[2
]}

Liu, J. S. ^{[2
]}

Liu, M. Y. ^{[4
]}

Lu, H. ^{[2
]}

Meng, X. R. ^{[4
]}

Mizutani, K. ^{[12
,17
]}

Munakata, K. ^{[14
]}

Nanjo, H. ^{[1
]}

Nishizawa, M. ^{[18
]}

Ohnishi, M. ^{[15
]}

Ohta, I. ^{[19
]}

Onuma, H. ^{[17
]}

Ozawa, S. ^{[12
]}

Qian, X. L. ^{[2
,6
]}

Qu, X. B. ^{[2
]}

Saito, T. ^{[20
]}

Saito, T. Y. ^{[21
]}

机构：

[1] Hirosaki Univ, Dept Phys, Hirosaki, Aomori 0368561, Japan

[2] Chinese Acad Sci, Inst High Energy Phys, Key Lab Particle Astrophys, Beijing 100049, Peoples R China

[3] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China

[4] Tibet Univ, Dept Math & Phys, Lhasa 850000, Peoples R China

[5] Hebei Normal Univ, Dept Phys, Shijiazhuang 050016, Peoples R China

[6] Shandong Univ, Dept Phys, Jinan 250100, Peoples R China

[7] SouthWest Jiaotong Univ, Inst Modern Phys, Chengdu 610031, Peoples R China

[8] Chubu Univ, Dept Nat Sci & Math, Kasugai, Aichi 4878501, Japan

[9] Kanagawa Univ, Fac Engn, Yokohama, Kanagawa 2218686, Japan

[10] Utsunomiya Univ, Fac Educ, Utsunomiya, Tochigi 3218505, Japan

[11] Konan Univ, Dept Phys, Kobe, Hyogo 6588501, Japan

[12] Waseda Univ, Res Inst Sci & Engn, Tokyo 1698555, Japan

[13] Yokohama Natl Univ, Fac Engn, Yokohama, Kanagawa 2408501, Japan

[14] Shinshu Univ, Dept Phys, Matsumoto, Nagano 3908621, Japan

[15] Univ Tokyo, Inst Cosm Ray Res, Kashiwa, Chiba 2778582, Japan

[16] Shandong Agr Univ, Sch Informat Sci & Engn, Tai An 271018, Shandong, Peoples R China

[17] Saitama Univ, Saitama 3388570, Japan

[18] Natl Inst Informat, Tokyo 1018430, Japan

[19] Sakushin Gakuin Univ, Utsunomiya, Tochigi 3213295, Japan

[20] Tokyo Metropolitan Coll Ind Technol, Tokyo 1168523, Japan

[21] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany

[22] Nihon Univ, Coll Ind Technol, Narashino, Chiba 2758576, Japan

[23] Shonan Inst Technol, Fujisawa, Kanagawa 2518511, Japan

[24] Japan Atom Energy Agcy, Tokai, Ibaraki 3191195, Japan

[25] Shinshu Univ, Sch Gen Educ, Matsumoto, Nagano 3908621, Japan

来源：

PHYSICAL REVIEW LETTERS | 2013年 / 111卷 / 01期

基金：

中国国家自然科学基金; 日本学术振兴会;

关键词：

AIR-SHOWER ARRAY; HELIUM SPECTRA; ENERGY-RANGE; DIRECTIONS; PROTON; PHASE;

D O I：

10.1103/PhysRevLett.111.011101

中图分类号：

O4 [物理学];

学科分类号：

0702 ;

摘要：

We report on a clear solar-cycle variation of the Sun's shadow in the 10 TeV cosmic-ray flux observed by the Tibet air shower array during a full solar cycle from 1996 to 2009. In order to clarify the physical implications of the observed solar cycle variation, we develop numerical simulations of the Sun's shadow, using the potential field source surface model and the current sheet source surface (CSSS) model for the coronal magnetic field. We find that the intensity deficit in the simulated Sun's shadow is very sensitive to the coronal magnetic field structure, and the observed variation of the Sun's shadow is better reproduced by the CSSS model. This is the first successful attempt to evaluate the coronal magnetic field models by using the Sun's shadow observed in the TeV cosmic-ray flux.

引用

页数：5

共 21 条

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