Home > ALMA Jセミナー | 太陽系小天体セミナー | 総研大コロキウム > 2014.10.20-10.26

2014.10.20-10.26

10月20日(月)13:30~15:00  太陽系小天体セミナー   南棟2階会議室
Oct 20 Mon   Solar System Minor Body Seminar   Conference Room, South Bldg.2F

10月22日(水)10:30~12:00  総研大コロキウム   中央棟(北)1F講義室
Oct 22 Wed   SOKENDAI colloquium         Lecture Room

10月22日(水)14:00~15:00  ALMAJセミナー     ALMA棟 1F 会議室
Oct 22 Wed   ALMAJ Seminar            Room 109 1F of ALMA Bldg.

詳細は以下をご覧下さい。

10月20日(月)

キャンパス
三鷹
セミナー名
太陽系小天体セミナー
臨時・定例の別
定例
日時
10月20日(月曜日)13時30分~15時
場所
南棟2階会議室
講演者
塚田健
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

10月22日(水)

Campus
Mitaka
Seminar Name
SOKENDAI colloquium
Regular/Irregular
Regular
Date
10:30-12:00,10/22, 2014
Place
Lecture Room
Speaker
Tomoko Suzuki
Affiliation
D1, SOKENDAI, Mitaka(supervisor: Tadayuki Kodama)
Title
GANBA-Subaru: Dissecting high-z star-forming galaxies with NB and AO imaging
Facilitator
-Name:Taiki Suzuki

10月22日(水)

Campus
Mitaka
Seminar
ALMAJ Seminar
Regular/Irregular
Irregular
Date
2pm-3pm 22th October
Place
Room109 (1F) at ALMA Building
Speaker
Patricio Sanhueza
Affiliation
NAOJ Chile Observatory
Title
A Massive, Prestellar Clump hosting no High-Mass Prestellar Cores
Abstract
The Infrared Dark Cloud G028.23-00.19 hosts a massive (~1500 Msun), cold (12 K), and IR dark (from 3.6 to 70 um) clump that has the potential to form high-mass stars. We observed this prestellar clump candidate with the SMA and JVLA in order to characterize the early stages of high-mass star formation and constrain theoretical models. Dust emission at 1.3 mm reveals 4 cores with masses less than 13 Msun. None of the cores currently have the mass reservoir to form a high-mass star in the prestellar phase (assuming 30% star forming efficiency). If this massive clump will ultimately form high-mass stars, its embedded cores must gather a significant amount of mass over time, which is inconsistent with models that claim the existence of high-mass prestellar cores whose mass does not change significantly over their evolution. By using the NH3 (1,1) line, the velocity dispersion of the gas and the virial parameter of the cores are determined. The velocity dispersion is transonic or mildly supersonic (Delta_nt/Delta_th~1.1-1.8). The cores are not highly supersonic as some theories of high-mass star formation predict. Low virial parameters are derived (0.1-0.5), suggesting that the cores are not in virial equilibrium, unless strong magnetic fields of ~1 mG are present.
Facilitator
-Name:Kazuya Saigo

以上

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