Home > 太陽系小天体セミナー | 理論コロキウム > 2019.02.11-02.17

2019.02.11-02.17

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=

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