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Anisotropy and corotation of galactic cosmic rays

Abstract:

The intensity of Galactic cosmic rays is nearly isotropic because of the influence of magnetic fields in the Milky Way. Here, we present two-dimensional high-precision anisotropy measurement for energies from a few to several hundred teraelectronvolts (TeV), using the large data sample of the Tibet Air Shower Arrays. Besides revealing finer details of the known anisotropies, a new component of Galactic cosmic ray anisotropy in sidereal time is uncovered around the Cygnus region direction. For cosmic-ray energies up to a few hundred TeV, all components of anisotropies fade away, showing a corotation of Galactic cosmic rays with the local Galactic magnetic environment. These results have broad implications for a comprehensive understanding of cosmic rays, supernovae, magnetic fields, and heliospheric and Galactic dynamic environments.

Año de publicación:

2006

Keywords:

    Fuente:

    googlegoogle
    scopusscopus

    Tipo de documento:

    Article

    Estado:

    Acceso restringido

    Áreas de conocimiento:

    • Rayo cósmico

    Áreas temáticas:

    • Mecánica clásica

    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.
    Onuma H.Onuma H.
    Amenomori M.Amenomori M.
    Ouchi T.Ouchi T.
    Danzengluobu Danzengluobu
    Zhaxisangzhu Zhaxisangzhu
    Yuan A.F.Yuan A.F.
    Zhou X.X.Zhou X.X.
    Li J.Y.Li J.Y.
    Tsuchiya H.Tsuchiya H.
    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.
    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.
    Hu H.B.Hu H.B.
    T. K. SakoT. K. Sako
    TK SakoTK Sako
    Yang X.C.Yang X.C.
    Guo H.W.Guo H.W.
    Kajino F.Kajino F.
    Takita M.Takita M.
    Hu H.B.Hu H.B.
    Mu J.Mu J.
    Torii S.Torii S.
    Shirai T.Shirai T.
    Sasaki T.Sasaki T.
    He M.He M.
    Ohnishi M.Ohnishi M.
    Ren J.R.Ren J.R.
    Zhang X.Y.Zhang X.Y.
    Wang H.Wang H.
    Mishizawa M.Mishizawa M.
    Yamamoto Y.Yamamoto Y.
    Feng C.F.Feng C.F.
    Feng Z.Y.Feng Z.Y.
    Feng Z.Y.Feng Z.Y.
    Wang X.Wang X.
    Yasue S.Yasue S.
    Kato C.Kato C.
    Zhang J.L.Zhang J.L.
    Yu G.C.Yu G.C.
    Zhang Y.Zhang Y.
    Meng X.R.Meng X.R.
    Lu S.L.Lu S.L.
    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.
    Ayabe S.Ayabe S.
    Tateyama N.Tateyama N.
    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.
    Wang B.S.Wang B.S.
    Munakata K.Munakata K.
    Sugimoto H.Sugimoto H.
    Ohta I.Ohta I.
    Nagai A.Nagai A.
    Kawata K.Kawata K.