12月18日（火）13：30～15：00 太陽系小天体セミナー 南棟２階会議室
Dec 18 Tue Solar System Minor Body Seminar Conference Room, South Bldg.2F
12月19日（水）10：30～12：00 総研大コロキウム 講義室
Dec 19 Wed SOKENDAI colloquium Lecture Room
12月21日（金）16:00～17：00 国立天文台談話会 大セミナー室
Dec 21 Fri NAOJ Seminar Large Seminar Room
詳細は以下をご覧下さい。
12月18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
- 12月18日（火曜日）13時30分～15時
- 場所
- 南棟２階会議室
- 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
12月19日（水）
- Campus
- Mitaka
- Seminar
- SOKENDAI colloquium
- Regularly Scheduled/Sporadic
- Regular
- Date and time
- December 19, 2018, 10:30 -12:00
- Place
- Lecture Room
- Speaker
- Masaki Yoshida
- Affiliation
- SOKENDAI 4th year (D2)(Supervisor: Yoshinori Suematsu,Hirohisa Hara,Ryohko Ishikawa)
- Title
- MHD wave propagation along spicules observed by CLASP
- Abstract
- (optional)
Please note that the presenter information posted here is not necessarily listed in order of presentation.
- Facilitator
- -Name：Yoshiki Hatta
- Comment
- TV conference system is available connecting from Nobeyama, Hawaii, Mizusawa, and Okayama.
12月21日（金）
- Campus
- Mitaka
- Seminar
- NAOJ seminar
- Regularly Scheduled/Sporadic
- Scheduled
- Date and time
- Fri 21 Dec. 16:00~17:00
- Place
- Large Seminar Room
- Speaker
- Kengo Tachihara (立原研悟)
- Affiliation
- Nagoya University (名古屋大学)
- Title
- “Synthetic observations of clumpy ISM: Implications on the seed CO clouds and CO-dark molecular gas”
- Abstract
-
We carried out synthetic observations of a theoretical model of interstellar carbon in CO, C I and C II including
H2 formation. The theoretical model based on numerical simulations of H I gas converging at a velocity of
20km/s by Inoue & Inutsuka (2012) is employed in the present study. The gas model, which is fairy realistic
and consistent with the observations of the local gas located at high b, is turbulent and inhomogeneous
with magnetic field. We focus on the evolution of the rare species, CO, C I and C II from 0.3 Myr to
9 Myr since the converging flows collided. In the early phase within 1 Myr, the Cold Neutral Medium (CNM)
clumps of sub-pc scales are the formation sites of H2, CO and C I, and in the late phase from 3 Myr to 9 Myr
the CNM clumps merge together to form pc-scale molecular clouds. The results show that C I and CO
are well mixed at pc scales, and mark a significant disagreement with the classic picture which predicts
layered C I and CO distributions according to Av. The total mass budget of the local ISM indicates
the fraction of H I is about 70% and the CO-dark H2 is small, less than a few percent, contrary to the usual
assumption. The results of high resolution CO observations by the Nobeyama 45m telescope, ASTE, and
ALMA obtained at a cloud edge are consistent with this picture, and future high resolution CI observations
by ALMA/ACA will reveal small-scale structures of molecular clouds and PDRs. - Facilitator
- -Name：Nakaya, Hidehiko