Modeling of the galactic cosmic-ray anisotropy at TeV energies

M. Amenomori; X. J. Bi; D. Chen; W. Y. Chen; S. W. Cui; Danzengluobu; L. K. Ding; X. H. Ding; C. F. Feng; Zhaoyang Feng; Z. Y. Feng; Q. B. Gou; H. W. Guo; Y. Q. Guo; H. H. He; Z. T. He; K. Hibino; N. Hotta; Haibing Hu; H. B. Hu; J. Huang; W. J. Li; H. Y. Jia; L. Jiang; F. Kajino; K. Kasahara; Y. Katayose; C. Kato; K. Kawata; Labaciren; G. M. Le; A. F. Li; C. Liu; J. S. Liu; H. Lu; X. R. Meng; K. Mizutani; K. Munakata; H. Nanjo; M. Nishizawa; M. Ohnishi; I. Ohta; Shunsuke Ozawa; X. L. Qian; X. B. Qu; T. Saito; T. Y. Saito; M. Sakata; T. K. Sako; J. Shao; M. Shibata; A. Shiomi; T. Shirai; H. Sugimoto; M. Takita; Y. H. Tan; N. Tateyama; Shoji Torii; H. Tsuchiya; S. Udo; H. Wang; H. R. Wu; L. Xue; Y. Yamamoto; Z. Yang; S. Yasue; A. F. Yuan; T. Yuda; L. M. Zhai; H. M. Zhang; J. L. Zhang; X. Y. Zhang; Y. Zhang; Yi Zhang; Ying Zhang; Zhaxisangzhu; X. X. Zhou

doi:10.7529/ICRC2011/V02/0361

Modeling of the galactic cosmic-ray anisotropy at TeV energies

M. Amenomori, X. J. Bi, D. Chen, W. Y. Chen, S. W. Cui, Danzengluobu, L. K. Ding, X. H. Ding, C. F. Feng, Zhaoyang Feng, Z. Y. Feng, Q. B. Gou, H. W. Guo, Y. Q. Guo, H. H. He, Z. T. He, K. Hibino, N. Hotta, Haibing Hu, H. B. HuJ. Huang, W. J. Li, H. Y. Jia, L. Jiang, F. Kajino, K. Kasahara, Y. Katayose, C. Kato, K. Kawata, Labaciren, G. M. Le, A. F. Li, C. Liu, J. S. Liu, H. Lu, X. R. Meng, K. Mizutani, K. Munakata, H. Nanjo, M. Nishizawa, M. Ohnishi, I. Ohta, Shunsuke Ozawa, X. L. Qian, X. B. Qu, T. Saito, T. Y. Saito, M. Sakata, T. K. Sako^*, J. Shao, M. Shibata, A. Shiomi, T. Shirai, H. Sugimoto, M. Takita, Y. H. Tan, N. Tateyama, Shoji Torii, H. Tsuchiya, S. Udo, H. Wang, H. R. Wu, L. Xue, Y. Yamamoto, Z. Yang, S. Yasue, A. F. Yuan, T. Yuda, L. M. Zhai, H. M. Zhang, J. L. Zhang, X. Y. Zhang, Y. Zhang, Yi Zhang, Ying Zhang, Zhaxisangzhu, X. X. Zhou

^*この研究の対応する著者

理工学術院総合研究所

研究成果: Conference contribution

2 被引用数 (Scopus)

抄録

A possible origin of the large-scale anisotropy of TeV galactic cosmic rays is discussed. It can be well modeled by a superposition of the Global Anisotropy and the Midscale Anisotropy. The Global Anisotropy would be generated by galactic cosmic rays interacting with the magnetic field in the local interstellar space of a few parsec scale surrounding the heliosphere. On the other hand, the Midscale Anisotropy would be caused by the modulation of galactic cosmic rays in the heliotail. The Midscale Anisotropy can be expressed as two intensity enhancements placed along the Hydrogen Deflection Plane, each symmetrically centered away from the heliotail direction. It is found that the separation angle between the heliotail direction and each of the two intensity enhancements monotonously decreases as energy increases from 4 TeV to 30 TeV.

本文言語	English
ホスト出版物のタイトル	Proceedings of the 32nd International Cosmic Ray Conference, ICRC 2011
出版社	Institute of High Energy Physics
ページ	103-106
ページ数	4
巻	11
DOI	https://doi.org/10.7529/ICRC2011/V02/0361
出版ステータス	Published - 2011
イベント	32nd International Cosmic Ray Conference, ICRC 2011 - Beijing 継続期間: 2011 8月 11 → 2011 8月 18

Other

Other	32nd International Cosmic Ray Conference, ICRC 2011
City	Beijing
Period	11/8/11 → 11/8/18

ASJC Scopus subject areas

核物理学および高エネルギー物理学

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10.7529/ICRC2011/V02/0361

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引用スタイル

Amenomori, M., Bi, X. J., Chen, D., Chen, W. Y., Cui, S. W., Danzengluobu, Ding, L. K., Ding, X. H., Feng, C. F., Feng, Z., Feng, Z. Y., Gou, Q. B., Guo, H. W., Guo, Y. Q., He, H. H., He, Z. T., Hibino, K., Hotta, N., Hu, H., ... Zhou, X. X. (2011). Modeling of the galactic cosmic-ray anisotropy at TeV energies. In Proceedings of the 32nd International Cosmic Ray Conference, ICRC 2011 (Vol. 11, pp. 103-106). Institute of High Energy Physics. https://doi.org/10.7529/ICRC2011/V02/0361

Amenomori, M, Bi, XJ, Chen, D, Chen, WY, Cui, SW, Danzengluobu, Ding, LK, Ding, XH, Feng, CF, Feng, Z, Feng, ZY, Gou, QB, Guo, HW, Guo, YQ, He, HH, He, ZT, Hibino, K, Hotta, N, Hu, H, Hu, HB, Huang, J, Li, WJ, Jia, HY, Jiang, L, Kajino, F, Kasahara, K, Katayose, Y, Kato, C, Kawata, K, Labaciren, Le, GM, Li, AF, Liu, C, Liu, JS, Lu, H, Meng, XR, Mizutani, K, Munakata, K, Nanjo, H, Nishizawa, M, Ohnishi, M, Ohta, I, Ozawa, S, Qian, XL, Qu, XB, Saito, T, Saito, TY, Sakata, M, Sako, TK, Shao, J, Shibata, M, Shiomi, A, Shirai, T, Sugimoto, H, Takita, M, Tan, YH, Tateyama, N, Torii, S, Tsuchiya, H, Udo, S, Wang, H, Wu, HR, Xue, L, Yamamoto, Y, Yang, Z, Yasue, S, Yuan, AF, Yuda, T, Zhai, LM, Zhang, HM, Zhang, JL, Zhang, XY, Zhang, Y, Zhang, Y, Zhang, Y, Zhaxisangzhu & Zhou, XX 2011, Modeling of the galactic cosmic-ray anisotropy at TeV energies. in Proceedings of the 32nd International Cosmic Ray Conference, ICRC 2011. vol. 11, Institute of High Energy Physics, pp. 103-106, 32nd International Cosmic Ray Conference, ICRC 2011, Beijing, 11/8/11. https://doi.org/10.7529/ICRC2011/V02/0361

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title = "Modeling of the galactic cosmic-ray anisotropy at TeV energies",

abstract = "A possible origin of the large-scale anisotropy of TeV galactic cosmic rays is discussed. It can be well modeled by a superposition of the Global Anisotropy and the Midscale Anisotropy. The Global Anisotropy would be generated by galactic cosmic rays interacting with the magnetic field in the local interstellar space of a few parsec scale surrounding the heliosphere. On the other hand, the Midscale Anisotropy would be caused by the modulation of galactic cosmic rays in the heliotail. The Midscale Anisotropy can be expressed as two intensity enhancements placed along the Hydrogen Deflection Plane, each symmetrically centered away from the heliotail direction. It is found that the separation angle between the heliotail direction and each of the two intensity enhancements monotonously decreases as energy increases from 4 TeV to 30 TeV.",

keywords = "Anisotropy, Galactic cosmic rays, TeV energies, Tibet",

author = "M. Amenomori and Bi, {X. J.} and D. Chen and Chen, {W. Y.} and Cui, {S. W.} and Danzengluobu and Ding, {L. K.} and Ding, {X. H.} and Feng, {C. F.} and Zhaoyang Feng and Feng, {Z. Y.} and Gou, {Q. B.} and Guo, {H. W.} and Guo, {Y. Q.} and He, {H. H.} and He, {Z. T.} and K. Hibino and N. Hotta and Haibing Hu and Hu, {H. B.} and J. Huang and Li, {W. J.} and Jia, {H. Y.} and L. Jiang and F. Kajino and K. Kasahara and Y. Katayose and C. Kato and K. Kawata and Labaciren and Le, {G. M.} and Li, {A. F.} and C. Liu and Liu, {J. S.} and H. Lu and Meng, {X. R.} and K. Mizutani and K. Munakata and H. Nanjo and M. Nishizawa and M. Ohnishi and I. Ohta and Shunsuke Ozawa and Qian, {X. L.} and Qu, {X. B.} and T. Saito and Saito, {T. Y.} and M. Sakata and Sako, {T. K.} and J. Shao and M. Shibata and A. Shiomi and T. Shirai and H. Sugimoto and M. Takita and Tan, {Y. H.} and N. Tateyama and Shoji Torii and H. Tsuchiya and S. Udo and H. Wang and Wu, {H. R.} and L. Xue and Y. Yamamoto and Z. Yang and S. Yasue and Yuan, {A. F.} and T. Yuda and Zhai, {L. M.} and Zhang, {H. M.} and Zhang, {J. L.} and Zhang, {X. Y.} and Y. Zhang and Yi Zhang and Ying Zhang and Zhaxisangzhu and Zhou, {X. X.}",

year = "2011",

doi = "10.7529/ICRC2011/V02/0361",

language = "English",

volume = "11",

pages = "103--106",

booktitle = "Proceedings of the 32nd International Cosmic Ray Conference, ICRC 2011",

publisher = "Institute of High Energy Physics",

note = "32nd International Cosmic Ray Conference, ICRC 2011 ; Conference date: 11-08-2011 Through 18-08-2011",

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T1 - Modeling of the galactic cosmic-ray anisotropy at TeV energies

AU - Amenomori, M.

AU - Bi, X. J.

AU - Chen, D.

AU - Chen, W. Y.

AU - Cui, S. W.

AU - Danzengluobu,

AU - Ding, L. K.

AU - Ding, X. H.

AU - Feng, C. F.

AU - Feng, Zhaoyang

AU - Feng, Z. Y.

AU - Gou, Q. B.

AU - Guo, H. W.

AU - Guo, Y. Q.

AU - He, H. H.

AU - He, Z. T.

AU - Hibino, K.

AU - Hotta, N.

AU - Hu, Haibing

AU - Hu, H. B.

AU - Huang, J.

AU - Li, W. J.

AU - Jia, H. Y.

AU - Jiang, L.

AU - Kajino, F.

AU - Kasahara, K.

AU - Katayose, Y.

AU - Kato, C.

AU - Kawata, K.

AU - Labaciren,

AU - Le, G. M.

AU - Li, A. F.

AU - Liu, C.

AU - Liu, J. S.

AU - Lu, H.

AU - Meng, X. R.

AU - Mizutani, K.

AU - Munakata, K.

AU - Nanjo, H.

AU - Nishizawa, M.

AU - Ohnishi, M.

AU - Ohta, I.

AU - Ozawa, Shunsuke

AU - Qian, X. L.

AU - Qu, X. B.

AU - Saito, T.

AU - Saito, T. Y.

AU - Sakata, M.

AU - Sako, T. K.

AU - Shao, J.

AU - Shibata, M.

AU - Shiomi, A.

AU - Shirai, T.

AU - Sugimoto, H.

AU - Takita, M.

AU - Tan, Y. H.

AU - Tateyama, N.

AU - Torii, Shoji

AU - Tsuchiya, H.

AU - Udo, S.

AU - Wang, H.

AU - Wu, H. R.

AU - Xue, L.

AU - Yamamoto, Y.

AU - Yang, Z.

AU - Yasue, S.

AU - Yuan, A. F.

AU - Yuda, T.

AU - Zhai, L. M.

AU - Zhang, H. M.

AU - Zhang, J. L.

AU - Zhang, X. Y.

AU - Zhang, Y.

AU - Zhang, Yi

AU - Zhang, Ying

AU - Zhaxisangzhu,

AU - Zhou, X. X.

PY - 2011

Y1 - 2011

N2 - A possible origin of the large-scale anisotropy of TeV galactic cosmic rays is discussed. It can be well modeled by a superposition of the Global Anisotropy and the Midscale Anisotropy. The Global Anisotropy would be generated by galactic cosmic rays interacting with the magnetic field in the local interstellar space of a few parsec scale surrounding the heliosphere. On the other hand, the Midscale Anisotropy would be caused by the modulation of galactic cosmic rays in the heliotail. The Midscale Anisotropy can be expressed as two intensity enhancements placed along the Hydrogen Deflection Plane, each symmetrically centered away from the heliotail direction. It is found that the separation angle between the heliotail direction and each of the two intensity enhancements monotonously decreases as energy increases from 4 TeV to 30 TeV.

AB - A possible origin of the large-scale anisotropy of TeV galactic cosmic rays is discussed. It can be well modeled by a superposition of the Global Anisotropy and the Midscale Anisotropy. The Global Anisotropy would be generated by galactic cosmic rays interacting with the magnetic field in the local interstellar space of a few parsec scale surrounding the heliosphere. On the other hand, the Midscale Anisotropy would be caused by the modulation of galactic cosmic rays in the heliotail. The Midscale Anisotropy can be expressed as two intensity enhancements placed along the Hydrogen Deflection Plane, each symmetrically centered away from the heliotail direction. It is found that the separation angle between the heliotail direction and each of the two intensity enhancements monotonously decreases as energy increases from 4 TeV to 30 TeV.

KW - Anisotropy

KW - Galactic cosmic rays

KW - TeV energies

KW - Tibet

UR - http://www.scopus.com/inward/record.url?scp=84899517613&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=84899517613&partnerID=8YFLogxK

U2 - 10.7529/ICRC2011/V02/0361

DO - 10.7529/ICRC2011/V02/0361

M3 - Conference contribution

AN - SCOPUS:84899517613

VL - 11

SP - 103

EP - 106

BT - Proceedings of the 32nd International Cosmic Ray Conference, ICRC 2011

PB - Institute of High Energy Physics

T2 - 32nd International Cosmic Ray Conference, ICRC 2011

Y2 - 11 August 2011 through 18 August 2011

ER -

Modeling of the galactic cosmic-ray anisotropy at TeV energies

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