2月12日（火）13：30～15：00 太陽系小天体セミナー 南棟２階会議室
Feb 12 Tue Solar System Minor Body Seminar Conference Room, South Bldg.2F
2月12日（火）13：30～15：00 理論コロキウム 講義室
Feb 12 Tue DTA colloquium Lecture Room
詳細は以下をご覧下さい。
2月12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
- 2月12日（火曜日）13時30分～15時
- 場所
- 南棟２階会議室
- 講演者
- 土屋智恵
- 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
2月12日（火）
- Campus
- Mitaka
- Seminar
- DTA colloquium
- Regularly Scheduled/Sporadic
- Regularly Scheduled
- Date and time
- February 12, 2019, 13:30-15:00
- Place
- Lecture room
- Speaker
- Kei Tanaka
- Affiliation
- Osaka University
- Title
- Massive Star Formation under Multiple Feedback Processes
- Abstract
- Despite their importance in various fields of astrophysics, the formation of massive stars is not understood well compared to low-mass star formation. Stars with over-100 solar masses have especially been theoretically considered to be hardly formed due to their own radiation feedback even though they do exist. In this talk, I first summarize the concept of “Core Accretion” scenario for massive star formation (e.g., McKee & Tan 2003), which is a scaled-up version of models of low-mass star formation from cores. Then, I present our theoretical works, i.e., the first study of the multiple feedback processes in massive star formation (Tanaka et al. 2017a, 2018). Our model shows that, at solar metallicity, very massive stars with at least 500Msun can be formed by the mass accretion through disks. The MHD disk wind is the most robust feedback rather than the radiative feedback even in massive star formation. We also apply this model to a wide range of metallicities to connect present-day massive star formation and first-star formation in the early universe. At lower metallicity, we find that the star formation efficiency gets lower due to the efficient photo-evaporation. Finally, I introduce our recent observations of massive protostars by SOFIA, VLA, and ALMA (De Buizer et al. 2017, Rosero et al. 2019, Zhang et al. 2019, etc.). We reveal the properties of massive protostars which are deeply embedded in their natal molecular clouds utilizing our theoretical models (Tanaka et al. 2016, 2017b, etc.).
- Facilitator
- -Name：Tomoya Takiwaki
- Comment
- in English=