9月25日（月）13：30～15：00 太陽天体プラズマセミナー 院生セミナー室
Sep 25 Mon Solar and Space Plasma Seminar Student Seminar Room, Subaru Bldg.
9月26日（火）13：30～15：00 太陽系小天体セミナー 南棟２階会議室
Sep 26 tue Solar System Minor Body Seminar Conference Room, South Bldg.2F
9月27日（水）10：30～12：00 総研大コロキウム 中央棟 講義室
Sep 27 Wed SOKENDAI colloquium Lecture Room
詳細は以下をご覧下さい。
9月25日（月）
- Campus
- Mitaka
- Seminar
- Solar and Space Plasma Seminar
- Regularly Scheduled/Sporadic
- Sporadic
- Date and time
- 25 September (Mon), 13:30-15:00
- Place
- Student Seminar Room, Subaru Bldg.
- Speaker
- Antonia Savcheva
- Affiliation
- CfA/Harvard
- Title
- Solar Sigmoidal Active Regions: From Formation to Eruption
- Abstract
- The formation, evolution and eruption of solar active regions is a main theme in solar physics. Ultimately the goal is predicting when, where and how an eruption will occur, which will greatly aid space weather forecasting. S-shaped active regions (sigmoids) facilitate this line of research, since they provide conditions that are easier to disentangle and have a high probability for erupting as flares and/or coronal mass ejections. This talk explores the behaviour of solar sigmoids via both observational and magnetic field modeling studies. Data from the most modern space-based solar observatories are utilized in addition to data-constrained non-linear force-free field (NLFFF) models and MHD simulations to gain insight into the physical processes controlling the evolution and eruption of solar sigmoids. By means of a large comprehensive observational study we investigate the formation and evolution mechanism. Specifically, we show that flux cancellation is a major mechanism for flux rope formation and evolution. We demonstrate how X-ray observations are used to constrain the flux rope insertion method for building NLFFF models over the evolution of such sigmoids and make use of topological analysis to describe the magnetic field structure of the sigmoids. We show that when data-constrained models are used in sync with MHD simulations and observations we can arrive at a consistent picture of the scenario for CME onset, namely the positive feedback between reconnection at a generalized X-line and the torus instability. In addition, we show that topological analysis is of great use in analyzing the (post-)eruption flare- and CME-associated observational features. Such analysis is used to extend the standard 2D flare/CME models to 3D and to find potentially large implications of topology to understanding 3D reconnection and future applications to predictive space weather capabilities. Finally we, we demonstrate that when such NLFFF models are used as initial conditions to global MHD codes, they reproduce very well the observed CME morphology and propagation.
- Facilitator
- -Name：Shin Toriumi
- Comment
-
—
Shin Toriumi, Ph.D.
Solar and Plasma Astrophysics Division
National Astronomical Observatory of Japan
2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan shin.toriumi@nao.ac.jp
9月26日（火）
- キャンパス
- 三鷹
- セミナー名
- 太陽系小天体セミナー
- 定例・臨時の別
- 定例
- 日時
- 9月26日（火曜日）13時30分～15時
- 場所
- 南棟２階会議室
- 講演者
- 藤原康徳
- 連絡先
- 名前：渡部潤一
- 備考
- テレビ会議またはスカイプによる参加も可
9月27日（水）
- Campus
- Mitaka
- Seminar
- SOKENDAI colloquium
- Regularly Scheduled/Sporadic
- Regular
- Date and time
- September 27 2017, 10:30 -12:00
- Place
- Lecture Room
- Speaker1
- Kei Ito
- Affiliation
- SOKENDAI M1 (Supervisor; Nobunari Kashikawa)
- Title
- z~5 HSC Protocluster survey
- Speaker2
- Takafumi Tsukui
- Affiliation
- SOKENDAI M1 (Supervisor; Satoru Iguchi, Hiroshi Nagai, Yuichi Matsuda)
- Title
- Radio Galaxy Formation
- Facilitator
- -Name：Misaki Ando
- Comment
- TV conference system is available connecting from Nobeyama, Hawaii, Mizusawa, and Okayama.
以上