4月24日（火）13：30～15：00 太陽系小天体セミナー 第三会議室
Apr 24 Tue Solar System Minor Body Seminar 3rd Conference Room
4月24日（火）13：30～14：30 理論コロキウム 輪講室
Apr 24 Tue DTA colloquium Rinko-room
4月25日（水）10：30～12：00 総研大コロキウム 講義室
Apr 25 Wed SOKENDAI colloquium Lecture Room
4月27日（金）13：30～15：00 太陽天体プラズマセミナー 院生セミナー室
Apr 27 Fri Solar and Space Plasma Seminar Student Seminar Room, Subaru Bldg.
詳細は以下をご覧下さい。
4月24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
- 4月24日（火曜日）13時30分～15時
- 場所
- 第三会議室
- 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
4月24日（火）
- Campus
- Mitaka
- Seminar
- DTA colloquium
- Regularly Scheduled/Sporadic
- Regularly Scheduled
- Date and time
- April 24, 2018,13:30-14:30
- Place
- Rinko room
- Speaker
- Akihiro Suzuki
- Affiliation
- DTA, NAOJ
- Title
- Multi-dimensional modeling of supernova ejecta with a central energy source
- Abstract
- Core-collapse supernova explosions are of fundamental importance in the universe. They are an outcome of massive star formation and evolution and at the same time affect their surrounding environments in various ways. This is the reason why many supernova researches and surveys have been intensively conducted. One of the remarkable successes of modern transient survey programs is the discovery of an extremely bright class of core-collapse supernovae, called superluminous supernovae. Because of their high brightness, we can detect high-z events, potentially making it possible to probe star-forming activity even in the high-z universe. However, the problem is that the energy source of their bright emission is still debated. A promising scenario for superluminous supernovae is the central engine scenario, in which the compact remnant (highly rotating neutron star, black hole accretion disk, or whatever) left in the supernova ejecta play a role in giving rise to bright thermal emission. However, there are many remaining problems, such as, how exactly the additional energy deposition is realized and how the supernova ejecta with a central engine evolve. I’m lately investigating the hydrodynamic evolution of supernova ejecta with such a central energy source by using multi-dimensional numerical simulations. In this talk, after a brief introduction of supernovae, I present results of my recent studies.
- Facilitator
- -Name：Masahiro Ogihara
- Comment
- in English
4月25日（水）
- Campus
- Mitaka
- Seminar
- SOKENDAI colloquium
- Regularly Scheduled/Sporadic
- Regular
- Date and time
- April 25, 2018, 10:30 -12:00
- Place
- Lecture Room
- Speaker
- Kei Ito
- Affiliation
- SOKENDAI 2nd year (M2)(Supervisor: Nobunari Kashikawa,Yuichi Matsuda,Yusei Koyama)
- Title
- Detecting proto-BCG candidates at z~4 by using HSC-SSP
Abstract (if you like): - Speaker
- Nao Fukagawa
- Affiliation
- SOKENDAI 3rd year (D1)(Supervisor: Prof. Tadayuki Kodama,,)
- Title
- Gas inflow and outflow of star forming galaxies at redshift 1.4 as revealed by chemical evolution
Abstract (if you like):Gas inflow and outflow are processes that control star formation history of galaxies. Using chemical evolution models, we attempt to extract information about gas inflow and outflow of star forming galaxies at redshift z~1.4. In this talk, we discuss our results.Please note that the presenter information posted here is not necessarily listed in order of presentation.
- Facilitator
- -Name：Yoshiki Hatta
- Comment
- TV conference system is available connecting from Nobeyama, Hawaii, Mizusawa, and Okayama.
4月27日（金）
- Campus
- Mitaka
- Seminar
- Solar and Space Plasma Seminar
- Regularly Scheduled/Sporadic
- Regular
- Date and time
- 27 April (Fri), 13:30-15:00
- Place
- Student Seminar Room, Subaru Bldg.
- Speaker
- Yikang Wang
- Affiliation
- The University of Tokyo
- Title
- Simulation of Alfven wave propagation in the chromosphere with realistic radiative cooling
- Abstract
-
The chromospheric and coronal heating problem that why the plasma in the chromosphere and the corona could maintain a high temperature is still unclear. Previous researches (e.g. Kudoh & Shibata, 1999; Matsumoto & Shibata 2010) uncover that Alfv’en wave could carry enough energy that contributes to coronal heating. While previous researches usually ignore or treat chromospheric radiative loss crudely, we carry on 1.5D numerical simulation with realistic radiative loss introduced by Carlsson & Leenaarts (2013). In our simulation, Alfv’en wave is initiated by transverse torque artificially added near the lower boundary. We include white noise spectra to investigate the effect of radiation and observational based power spectra in order to mimic the convection motion at the solar surface. We find that under certain geometry setting, the amount of radiative loss as well as spatial distribution of radiative loss profile are consistent with observation.
At the same time, the amount of energy transporting to the corona also meets the requirement of coronal heating. Our study indicates that Alfv’en wave model has the potential to explain chromospheric heating as well as transporting enough energy to the corona for coronal heating simultaneously. - Facilitator
- -Name：Shin Toriumi
- Comment