7月20日（水）16:00～17:00 国立天文台談話会 大セミナー室
Jul 20 wed NAOJ Seminar Large Seminar Room
7月21日（木）14：30～15：30 ATCセミナー 大セミナー室
Jul 21 thu ATC Seminar Large Seminar Room
7月22日（金）13：30～15：00 太陽天体プラズマセミナー 院生セミナー室
Jul 22 fri Solar and Space Plasma Seminar Student Seminar Room, Subaru Bldg.
詳細は以下をご覧下さい。
7月20日（水）
- キャンパス
- 三鷹
- セミナー名
- 国立天文台談話会
- 定例・臨時の別
- 定例
- 日時
- 7月20日（水） 16:00-17:00
- 場所
- 大セミナー室
- 講演者
- Aleksander Schwarzenberg-Czerny
- 所属
- Nicolaus Copernicus Astronomical Center, Warsaw, Poland
- タイトル
- Astroseismology with BRITE nano-satellites
- Abstract
-
While bright stars are crucial for chemical evolution of the Universe and their structure and evolution are qualitatively understood, quantitative estimates suffer from poor description of convection and chemical mixing in their interiors. Hence opportunity for astroseismic studies based on detection of possibly weakest pulsation modes.
On one hand due to atmosphere, satellites are needed for ultimate precision. On the other hand, visible blue and red giants provide enough light for small telescopes. Hence idea for BRITE constellation of nano-satellites. After description of technical, software and science requirements follows brief description of first science results from BRITE project. - 連絡先
- -名前：久保 雅仁
7月21日（木）
- キャンパス
- 三鷹
- セミナー名
- ATCセミナー
- 定例・臨時の別
- 臨時
- 日時
- 7月21日（木曜日）14時30分～15時30分
- 場所
- 大セミナー室
- 講演者
- 内山 瑞穂 氏
- 所属
- 国立天文台 先端技術センター
- タイトル
- 次世代大型反射光学系の開発・組立
- Abstract
- (optional)
ATC着任以前に担当してきたTAO6.5m望遠鏡用中間赤外線観測装置MIMIZUKUの要素開発について発表いたします。今回はTAO/MIMIZUKUの簡単な紹介と、私が主に担当してきた光学系要素開発・組立について、特に非球面軸外し反射光学系のアライメント作業を中心に今後のTMT/IRISの開発との関連も含めてお話ししたいと思います。 - 連絡先
- -名前：都築 俊宏
- 備考
- 日本語での講演
7月22日（金）
- Campus
- Mitaka
- Seminar
- Solar and Space Plasma Seminar
- Regularly Scheduled/Sporadic
- Regular
- Date and time
- 22 July (Fri), 13:30-15:00
- Place
- Student Seminar Room, Subaru Bldg.
- Speaker
- Takafumi Kaneko
- Affiliation
- The University of Tokyo
- Title
- Numerical study of solar prominence formation by radiative condensation
- Abstract
-
Solar prominences (called as solar filaments on the disk) are cool dense plasma clouds in the hot tenuous corona. The formation mechanism of prominence is still unclear. One possible scenario is the formation of flux rope by converging motion. In this scenario, the flux rope is formed by reconnection of multiple coronal arcade fields, and the prominence mass is assumed to be sustained at the dip of the flux rope.
Although some observations support this scenario, the origin of cool dense plasma is still unclear. We demonstrate that the topological change from the coronal arcade field to the flux rope can trigger the radiative condensation (thermal instability) for prominence formation using three-dimensional MHD simulations including nonlinear anisotropic thermal conduction and optically thin radiative cooling. In our model, the converging and shearing motion at the footpoint of coronal arcade causes the reconnection for the formation of flux rope. When the reconnected loops are sufficiently long, the radiative cooling is not suppressed by thermal conduction, leading to radiative condensation. The critical length roughly matches Field length (Field 1965). Our simulated prominence (filament) satisfies some observed rules between the morphology of filament and the direction of magnetic field. - Facilitator
- -Name：Shin Toriumi
- Comment
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