2016.5.23-5.29

5月23日（月）13：30～15：00　 太陽系小天体セミナー　　　 南棟２階会議室
May 23 mon　　　　　　　　　　 Solar System Minor Body Seminar　　 Conference Room, South Bldg.2F

5月25日（水）10:30～11:30　　 総研大コロキウム 中央棟（北）1F講義室
May 25 wed　　　　　　　　　 SOKENDAI colloquium　　 Lecture Room

5月25日（水）13:30～14:30　 理論コロキウム コスモス会館会議室
May 25 wed　　　　　　　　　　 DTA colloquium　　 Conference Room, Cosmos Lodge

詳細は以下をご覧下さい。

5月23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

5月23日（月曜日）13時30分～15時

場所

南棟２階会議室

講演者

佐藤幹哉

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

5月25日（水）

Campus

Mitaka

Seminar

SOKENDAI colloquium

Regularly Scheduled/Sporadic

Regular
Date：10:30-11:30, May25, 2016

Place

Lecture Room

Speaker

Yi Yang

Affiliation

D2, SOKENDAI (supervisor : Saeko Hayashi)

Title

Direct Imaging of Circumstellar Disks and Planets in Binary Systems II

Facilitator

Name : Kotomi Taniguchi

Comment

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

5月25日（水）

Campus

Mitaka

Seminar

DTA colloquium

Regularly Scheduled/Sporadic

Regularly Scheduled Date and time：25 May 2016, 13:30-14:30

Place

Conference Room, Cosmos Lodge

Speaker

Yukari Ohtani

Affiliation

NAOJ CfCA

Title

Study of relation between emission of supernova shock breakout and central engine activity

Abstract

Shock breakout radiation originate as thermal emission from the shock passing through the outer layer of the star. It can provide the first information on how supernova explodes, no matter how relativistic the explosion is. There have been an question about the relativistic jet associated with a hypernova, of which explosion energy is ten times higher than that of an ordinary core-collapse supernova. The question is, how the central engine of the jet works. In order to obtain information on the central engine activity, it might be worth studying the emission properties of ultra-relativistic shock propagating into the dense circumstellar matter (CSM). For example, influence of bulk-Compton scattering on the spectrum can be a powerful indicator of the shock evolution, but there have been no theoretical study on that. In this talk, I will introduce our numerical study on the relationship between the behavior of an ultra-relativistic shock and the spectral properties of shock breakout emission. Using a Monte-Carlo method, we calculate the temporal spectral evolution of ultra-relativistic shock breakout in the CSM. We found that if the shock velocity monotonically decreases with time, photons with relatively high energies tend to appear fast. That is because the bulk kinetic energy of the shocked matter decreases. On the other hand, if the shock velocity increases with time, there are only slight changes in the spectrum. Therefore, in principle, it might be possible to obtain information on the activity of the jet central engine from the observable properties of ultra-relativistic shock breakout.

Facilitator

-Name：Tomoya Takiwaki

Comment

in English