| 著者名 | Authors | 所属機関名 | 所属機関名(欧文) | |
| 1 | #宗像/一起 | Munakata/Kazuoki | 信州大学理学部 | Faculty of Science, Shinshu University |
| 3 | 安江/新一 | Tanaka/T. | 信州大学理学部 | Faculty of Science, Shinshu University |
| 4 | 森/覚 | Mori/S. | 信州大学理学部 | Faculty of Science, Shinshu University |
| 5 | 加藤/千尋 | Kato/C. | 信州大学理学部 | Faculty of Science, Shinshu University |
| 6 | 藤井/善次郎 | Fujii/Z. | 名古屋大学太陽地球環境研究所 | STE-lab., Nagoya University |
| 7 | 藤本/和彦 | Fujimoto/K. | 名古屋大学太陽地球環境研究所 | STE-lab., Nagoya University |
| 8 | 鷲見/治一 | Washimi/H. | 湘南工科大学 | Shonan Institute of Technology |
| 9 | 田中/高史 | Shonan Institute of Technology | 通信総合研究所 | Communication Research Laboratory |
| 12 | 両半球観測グループ | two hemisphere observation group | K12 | M |
講演予稿:
宇宙線強度変動の南北両半球観測結果を、「ロスーコーン」と「テールー
イン」異方性を表すガウス関数を用いて解析し、得られたガウス関数の
パラメータから、宇宙線恒星時異方性のモデルを導く。また、この異方性の
起源を調べるため、鷲見ー田中（１９９６）によるMHDシミュレーション
結果を用い、モデル太陽圏内での宇宙線伝播を解析する。
abstract:
We have analyzed the yearly averaged sidereal daily
variations in the count rates of 46 underground muon
telescopes by fitting Gaussian functions to the data.
These functions represent the Loss-cone and Tail-in
anisotropies of the recent sidereal anisotropies model
proposed by Nagashima et al. (1995a, 1995b). The
underground muon telescopes cover the median rigidity
range 143 GV-1400 GV and almost entire celestial
sphere. From the Gaussian amplitudes and positions,
we have confirmed that the Tail-in anisotropy is more
prominent in the southern hemisphere with its
reference axis located at declination (delta) ~ 14 deg.
south, and right ascention (alpha) ~ 4.7 sidereal hours.
The Tail-in anisotropy is asymmetric about its reference
axis and the observed time of maximum intensity depends
on the viewing latitude of the underground muon
telescopes. We also find that the declination of the
reference axis may be related to the rigidity of the
cosmic rays. We show that the Loss-cone anisotropy
is symmetric and has a reference axis located on the
celestial equator (delta ~ 0 deg.) and alpha ~ 13 sidereal
hours. We have used the parameters of the Gaussian fits
to devise an empirical model of the sidereal anisotropies.
We present these results and discuss them in relation
to the model heliosphere obtained from the three
dimensional MHD simulations of the interaction between
the solar wind plasma and the interstellar medium by
Washimi and Tanaka (1996).
キーワード:
銀河宇宙線、恒星時異方性、外部太陽圏
Keywords:
galactic cosmic-rays, sidereal anisotropy, outer heliosphere