Home > Solar and Space Plasma (SSP) Seminar | 国立天文台談話会 | 総研大コロキウム > 2017.9.18-9.24

2017.9.18-9.24

        

9月19日(火)13:30~15:00     太陽天体プラズマセミナー          南棟2階会議室                        
Sep 19 tue               Solar and Space Plasma Seminar    Conference Room, South Bldg.2F

9月20日(水)10:00~12:00      総研大コロキウム              講義室                       
Sep 20 wed               SOKENDAI colloquium           Lecture Room                    

9月22日(金)16:00~17:00      国立天文台談話会             大セミナー室                        
Sep 22 fri                 NAOJ Seminar               Large Seminar Room                    

詳細は以下をご覧下さい。

9月19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
9月19日(火曜日)13時30分~15時
場所
南棟2階会議室
講演者
土屋智恵

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

9月20日(水)

Campus
Mitaka
Seminar
SOKENDAI colloquium
Regularly Scheduled/Sporadic
Irregular
Date and time
September 20 2017, 10:00 -12:00

Place
Lecture Room

Speaker1
Nao Fukagawa
Affiliation
SOKENDAI D1 (Supervisor : Prof. Tadayuki Kodama)
Title
Star formation, gas inflow and outflow of distant star-forming galaxies as revealed by chemical evolution
Abstract
Gas inflow and outflow are physical processes that control star formation histories of galaxies. Using simple chemical evolution model, we attempt to extract information about star formation and gas flows of star-forming galaxies at redshift z~1.4. We find a correlation between star formation efficiency and stellar mass. Mass-loading factor, or the ratio of outflow rate to star formation rate, inflow rate and outflow rate are only weakly related to stellar mass, probably due to limited mass range of the galaxies. Although there is still uncertainty about constraint of the gas inflow, our results support the idea that gas consumption by star formation and outflow is generally dominated compared with gas acquisition by inflow in star-forming galaxies at z~1.4, and they evolve along the main sequence of star-forming galaxies by increasing star formation efficiency while consuming the gas by star formation activities.

Speaker2
Shuichiro Tsuda
Affiliation
SOKENDI M1 (Supervisor; Mareki Honma)
Title
Observation near the Super-Massive Black Holes with the Event Horizon Telescope

Speaker3
Shigeru Namiki
Affiliation
SOKENDAI M1 (Supervisor; Nobunari Kashikawa)
Title
A Spectroscopic Study of a Rich Galaxy Cluster at z~1.52

Facilitator
-Name:Misaki Ando
Comment
TV conference system is available connecting from Nobeyama,
Hawaii, Mizusawa, and Okayama.

9月22日(金)

キャンパス
三鷹
セミナー名
国立天文台談話会
定例・臨時の別
定例
日時
9月22日(金曜日) 16:00-17:00
場所
大セミナー室
講演者
Chat Hull
所属
NAOJフェロー
タイトル
Star formation, polarization, and magnetic fields in the ALMA era
Abstract
The results from the ALMA polarization system have begun both to expand and to confound our understanding of the role of the magnetic field in low-mass star formation. After a brief motivation via CARMA, SMA, and other polarization observations from the prior decade, I will discuss new ALMA results, including the highest resolution and highest sensitivity polarization images made to date of two very young, Class 0 protostellar sources. These new observations achieve ~140 AU resolution, allowing us to probe polarization — and thus magnetic field orientation — in the innermost regions surrounding the protostars. First is a Class 0 protostellar source in Serpens known as Ser-emb 8, where a comparison with cutting-edge, moving-mesh AREPO simulations suggests that cloud-scale turbulence — not a large-scale magnetic field preserved from the source’s natal cloud — is dictating the magnetic field morphology immediately surrounding the protostar. In contrast, in the second source — known as Serpens SMM1 — the magnetic field has clearly been shaped by the bipolar outflow emanating from the central source, a situation that is quite different from the turbulence-dominated morphology of Ser-emb 8. Finally, I will show very recent observations of polarization toward IM Lup, a much more evolved, Class II protoplanetary disk. In the case of IM Lup, consistent with previous observations of other disks, the polarization appears to be due to scattering by dust grains, thus complicating the search for magnetic fields in disks, but opening up a new window into dust grain growth and evolution.

連絡先
-名前:矢野 太平

以上

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