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Heliospheric signatures seen in the sidereal anisotropy of high-energy galactic cosmic ray intensity

Abstract:

Mapping the global heliosphere by detecting energetic neutral atoms (ENAs), IBEX derived the semi-direct information on the structure of the large-scale magnetic field surrounding the heliosphere. Multi-TeV galactic cosmic rays (GCRs) also sense the global structure of the magnetic field within the whole heliosphere as well as the field surrounding the heliosphere, and can provide an additional tool to explore the global structure of these fields. We analyze, in this context, the multi-TeV GCR intensity observed with the Tibet Air Shower (AS) experiment, which clearly shows a midscale component structure observed as the excess intensity along Gurnett's HDP (Hydrogen Deflection Plane), as well as the global component structure. We find that the amplitude of the midscale component is only weakly dependent on GCR energy, while its angular extension along the HDP plane monotonously decreases with increasing energy. On the basis of these results, we discuss the possible origin of the midscale anisotropy. © 2010 American Institute of Physics.

Año de publicación:

2010

Keywords:

  • cosmic rays
  • Extensive air shower

Fuente:

scopusscopus

Tipo de documento:

Conference Object

Estado:

Acceso restringido

Áreas de conocimiento:

  • Rayo cósmico

Áreas temáticas:

  • Cuerpos y fenómenos celestes específicos

Contribuidores:

Shibata M.Shibata M.
Labaciren Labaciren
Hotta N.Hotta N.
Gao X.Y.Gao X.Y.
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.
Li J.Y.Li J.Y.
Tsuchiya H.Tsuchiya H.
Liu C.Liu C.
Ding L.K.Ding L.K.
Huang J.Huang J.
Cui S.W.Cui S.W.
Zhang H.M.Zhang H.M.
Hibino K.Hibino K.
Udo S.Udo S.
Xue L.Xue L.
Lou Y.Q.Lou Y.Q.
Nanjo H.Nanjo H.
Geng Q.X.Geng Q.X.
Huang Q.Huang Q.
Li A.F.Li A.F.
Zhang Y.Zhang Y.
Mizutani K.Mizutani K.
Wu H.R.Wu H.R.
Ding X.H.Ding X.H.
Tan Y.H.Tan Y.H.
Yan C.T.Yan C.T.
Wang Y.Wang Y.
Hu H.B.Hu H.B.
T. K. SakoT. K. Sako
Yang X.C.Yang X.C.
Guo H.W.Guo H.W.
Kajino F.Kajino F.
Kóta J.Kóta J.
Takita M.Takita M.
Hu H.B.Hu H.B.
Mu J.Mu J.
Torii S.Torii S.
Shirai T.Shirai T.
He M.He M.
Ohnishi M.Ohnishi M.
Zhang X.Y.Zhang X.Y.
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.
Yu G.C.Yu G.C.
Meng X.R.Meng X.R.
Zhang Y.Zhang Y.
Yuda T.Yuda T.
He H.H.He H.H.
Shiomi A.Shiomi A.
Chen D.Chen D.
Zhang Y.Zhang Y.
Le G.M.Le G.M.
Tateyama N.Tateyama N.
Li H.C.Li H.C.
Zhang N.J.Zhang N.J.
Saito T.Y.Saito T.Y.
Ye Z.H.Ye Z.H.
Ozawa S.Ozawa S.
Wang Y.G.Wang Y.G.
Katayose Y.Katayose Y.
Saito T.Saito T.
Jiang L.Jiang L.
Wang B.S.Wang B.S.
Munakata K.Munakata K.
Sugimoto H.Sugimoto H.
Ohta I.Ohta I.
Fan C.Fan C.
Kawata K.Kawata K.