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2018.04.23-29


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

Home > Solar and Space Plasma (SSP) Seminar | 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 > 2018.04.23-29

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