Author/Authors :
S. Torii، نويسنده , , K. Sakurai، نويسنده , , T. Shirai، نويسنده , , I. Shoji and T. Taira، نويسنده , , T. Tamura، نويسنده , , N. Tateyama، نويسنده , , K. Yoshida، نويسنده , , T. Yamagami، نويسنده , , E. Kamioka، نويسنده , , Y. Saito، نويسنده , , H. Murakami، نويسنده , , T. Kobayashi، نويسنده , , Y. Komori، نويسنده , , K. Kasahara، نويسنده , , T. Yuda، نويسنده , , J. Nishimura، نويسنده ,
Abstract :
The TeV electrons observed in the solar system are considered to be produced in the sources within 1 kpc in distance and in period for the past 100,000 years. The supernova remnants as a candidate of the electron sources are, therefore, very limited in number as Monogem, Loop 1, Geminga and Vela. It is expected that the few sources cause a structural component in the energy spectrum and an anisotropy in the arrival directions. Our calculations show that the direct effects of these nearby sources can be detected by a yearly observation with a detector having a geometrical factor of 0.5 m2 sr. We will present a future plan proposed for the observation of TeV electrons at the Japanese Experiment Module (JEM) in ISS.
