دورية أكاديمية
The Anisotropy of Cosmic Ray Arrival Direction around 10^18eV
| العنوان: | The Anisotropy of Cosmic Ray Arrival Direction around 10^18eV |
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| المؤلفون: | Hayashida, N., Honda, K., Inoue, N., Kadota, K., Kakimoto, F., Kakizawa, S., Kamata, K., Kawaguchi, S., Kawasaki, Y., Kawasumi, N., Kusano, E., Matsubara, Y., Mase, K., Minagawa, T., Murakami, K., Nagano, M., Nishikawa, D., Ohoka, H., Osone, S., Sakaki, N., Sasaki, M., Sasano, M., Shinozaki, K., Takeda, M., Teshima, M., Torii, R., Tsushima, I., Uchihori, Y., Yamamoto, T., Yoshida, S., Yoshii, H., Collaboration, The AGASA |
| سنة النشر: | 1999 |
| المجموعة: | ArXiv.org (Cornell University Library) |
| مصطلحات موضوعية: | Astrophysics |
| الوصف: | Anisotropy in the arrival directions of cosmic rays around 10^{18}eV is studied using data from the Akeno 20 km^2 array and the Akeno Giant Air Shower Array (AGASA), using a total of about 216,000 showers observed over 15 years above 10^{17}eV. In the first harmonic analysis, we have found significant anisotropy of $\sim$ 4 % around 10^{18}eV, corresponding to a chance probability of $\sim 10^{-5}$ after taking the number of independent trials into account. With two dimensional analysis in right ascension and declination, this anisotropy is interpreted as an excess of showers near the directions of the Galactic Center and the Cygnus region. This is a clear evidence for the existence of the galactic cosmic ray up to the energy of 10^{18}eV. Primary particle which contribute this anisotropy may be proton or neutron. ; Comment: 4pages, three figures, to appear in Procedings of 26th ICRC(Salt Lake City) |
| نوع الوثيقة: | text |
| اللغة: | unknown |
| العلاقة: | http://arxiv.org/abs/astro-ph/9906056Test |
| DOI: | 10.1016/S0927-6505(98)00064-4 |
| الإتاحة: | https://doi.org/10.1016/S0927-6505Test(98)00064-4 http://arxiv.org/abs/astro-ph/9906056Test |
| رقم الانضمام: | edsbas.695B89C2 |
| قاعدة البيانات: | BASE |
| DOI: | 10.1016/S0927-6505(98)00064-4 |
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