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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.

Año de publicación:

2011

Keywords:

  • Galactic cosmic rays
  • Tibet
  • TeV energies
  • anisotropy

Fuente:

googlegoogle
scopusscopus

Tipo de documento:

Conference Object

Estado:

Acceso restringido

Áreas de conocimiento:

  • Ciencia planetaria

Áreas temáticas:

  • Mecánica clásica
  • Cuerpos y fenómenos celestes específicos

Contribuidores:

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