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Time dependence of loss-cone amplitude measured with the tibet air-shower array

Abstract:

The galactic cosmic-ray anisotropy at TeV energies has a large-scale deficit region distributed around 150 to 240 degrees in right ascension, which is called "Loss-Cone". The Milagro experiment in the U.S. detected a significant increase in the Loss-Cone amplitude at 6 TeV from July 2000 to July 2007, and argued that it could be due to variations in the heliosphere in relation to solar activities. In this presentation, we report on the time dependence of the Loss-Cone amplitude from November 1999 through December 2008 measured with the Tibet air-shower array. No time dependence was found in the Loss-Cone amplitude at energies of 4.4, 6.2, and 11 TeV. If the increase in the Loss-Cone amplitude Milagro detected were genuine, the same tendency would be seen at sub-TeV energies where the anisotropy is far more sensitive to solar activities. Matsushiro underground muon observation at 0.6 TeV during the corresponding period, however, reported no significant increase of the Loss-Cone amplitude.

Año de publicación:

2011

Keywords:

  • Sidereal anisotropy
  • Galactic cosmic rays
  • Tibet
  • TeV energies
  • Loss cone

Fuente:

googlegoogle
scopusscopus

Tipo de documento:

Conference Object

Estado:

Acceso restringido

Áreas de conocimiento:

  • Ciencia planetaria

Áreas temáticas:

  • Física
  • Cuerpos y fenómenos celestes específicos
  • Astronomía y ciencias afines

Contribuidores:

Shibata M.Shibata M.
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.
Yuan A.F.Yuan A.F.
Luobu D.Luobu D.
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.
Ngzhu Z.Ngzhu Z.
Yasue S.Yasue S.
Kato C.Kato C.
Zhang J.L.Zhang J.L.
Zhang X.Y.Zhang X.Y.
Baciren L.Baciren L.
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.