タイトル | Radio science results: Exploration of solar wind acceleration region using interplanetary scintillation of water vapor maser source and quasars |
その他のタイトル | 電波科学の成果:水蒸気メーザソースとクエイサによる惑星間シンチレーションを用いた太陽風加速領域の探索 |
著者(日) | 徳丸 宗利; 山内 洋平; 近藤 哲朗 |
著者(英) | Tokumaru, Munetoshi; Yamauchi, Yohei; Kondo, Tetsuro |
著者所属(日) | 名古屋大学太陽地球環境研究所; NASA, Marshall Space Flight Center; 通信総合研究所 鹿島宇宙通信センター 宇宙電波応用研究室 |
著者所属(英) | Solar-Terrestrial Environment Laboratory, Nagoya University; NASA, Marshall Space Flight Center; Communications Research Laboratory Radio Astronomy Applications Section, Kashima Space Research Center |
発行日 | 2001-03-30 |
発行機関など | Communications Research Laboratory 通信総合研究所 |
刊行物名 | Journal of the Communications Research Laboratory 通信総合研究所英文論文集 |
巻 | 48 |
号 | 1 |
開始ページ | 173 |
終了ページ | 195 |
刊行年月日 | 2001-03-30 |
言語 | eng |
抄録 | Single-station observations of interplanetary scintillation (IPS) at three microwave frequencies; 2 GHz, 8 GHz and 22 GHz have been carried out between 1989 and 1998 using a large (34 m diameter) radio telescope at the Kashima Space Research Center of the Communications Research Laboratory. The aim of these observations is to explore the near-sun solar wind, which is the key region for the study of the solar wind acceleration mechanism. Strong quasars; 3C279 and 3C273B were used for Kashima IPS observations at 2 GHz and 8 GHz, and a water vapor maser source, IRC20431 was used for the IPS observations at 22 GHz. Solar wind velocities derived from Kashima IPS data suggest that the solar wind acceleration takes place at radial distances between 10 and 30 solar radii (Rs) from the sun. Properties of the turbulence spectrum (e.g. anisotropy, spectral index, inner scale) inferred from Kashima data are found to change systematically in the solar wind acceleration region. While the solar wind in the maximum phase appears to be dominated by the slow wind, fast and rarefied winds associated with coronal holes are found to develop significantly at high latitudes as the solar activity declines. Nevertheless, Kashima data suggests that the location of the acceleration region is stable throughout the solar cycle. |
キーワード | solar wind acceleration region; interplanetary scintillation; water maser; quasar; space plasma physics; Kashima 34 m radio telescope; UHF; coronal hole; 太陽風加速領域; 惑星間シンチレーション; 水メーザ; クエイサ; 宇宙プラズマ物理; 鹿島34m電波望遠鏡; UHF; コロナホール |
資料種別 | Technical Report |
ISSN | 0914-9260 |
SHI-NO | AA0029436019 |
URI | https://repository.exst.jaxa.jp/dspace/handle/a-is/37599 |