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2016.12.12-12.18

12月12日(月)13:30~15:00  太陽系小天体セミナー   南棟2階会議室
Dec 12 mon        Solar System Minor Body Seminar  Conference Room, South Bldg.2F

12月14日(水)10:30~11:30   総研大コロキウム     中央棟(北)1F講義室
Dec 14 wed           SOKENDAI Colloquium   Lecture room

12月14日(水)13:30~14:30  理論コロキウム     コスモス会館会議室                        
Dec 14 wed           DTA colloquium   Conference Room, Cosmos Lodge                       

詳細は以下をご覧下さい。

12月12日(月)

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12日(月曜日)13時30分~15時
場所
南棟2階会議室
講演者
寺居剛

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14日(水)

Campus
Mitaka
Seminar
SOKENDAI colloquium
Regularly Scheduled/Sporadic
Regularly
Date and time
10:30-11:30, December 14, 2016
Place
Lecture Room
Speaker
Satoshi Tanioka
Affiliation
SOKENDAI M1 (Supervisor; Yoichi Aso)
Title
Possible indirect confirmation of the existence of Pop III massive stars by gravitational wave (The review of Kinugawa+14
Abstract
(optional)
Facilitator
-Name:Kotomi Taniguchi

Comment
TV conference system is available connecting from Nobeyama, Hawaii, Mizusawa, and Okayama.

12月14日(水)

Campus
Mitaka
Seminar
DTA colloquium
Regularly Scheduled/Sporadic
Regularly Scheduled Date and time:14 December 2016, 13:30-14:30
Place
Conference Room, Cosmos Lodge
Speaker
Shunsuke Hozumi
Affiliation
Shiga University
Title
Intrisic Properties of the Bars Formed by the Bar Instability in Flat Stellar Disks
Abstract
Recent observations have revealed that some properties of galactic bars have been uncovered on a statistically meaningful levels of accuracy using a large sample of galaxies. As a result, it has been found that bars in SB0-SBb galaxies are longer than those in SBc to SBd galaxies. Furthermore, also found are such properties that the longer bars have larger amplitudes, and show more elongated shapes. However, these systematic bar properties have never been explained physically. In this talk, I show the properties of the bars formed by the bar instability for flat stellar disk models which are constructed on the basis of exact equilibrium distribution functions. Then, I demonstrate that the properties of the simulated bars are, in large measure, similar to those of the observed bars, and that the amplitude, length, and axis ratio are strongly correlated to an initial typical Toomre’s Q value. Taking into consideration these results, I discuss what the Hubble sequence represents.
Facilitator
-Name:Tomoya Takiwaki

Comment
in English

以上

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