Home > 太陽系小天体セミナー | 理論コロキウム | 総研大コロキウム > 2016.5.23-5.29

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

Home > 太陽系小天体セミナー | 理論コロキウム | 総研大コロキウム > 2016.5.23-5.29

Return to page top