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Colloquium のバックアップ差分(No.78)


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* DTA Colloquium 2018 [#z407468f]

DTA Colloquium(理論コロキウム)は原則として毎週火曜日の午後13:30から開催しています。~
原則として英語で講演していただきますが、
講師・参加者が日本人だけの場合は日本語に切り替えてくださっても(英語のままでも)結構です。~
台内・台外また分野を問わず広く発表者(台外の方には旅費・謝金あり)を募集しています。~
お問い合わせは以下のコロキウム係までお願いします(_AT_を@に変更してください)。~

- 滝脇知也 takiwaki.tomoya_AT_nao.ac.jp~
- 片岡 章雅 akimasa.kataoka_AT_nao.ac.jp~
- Kenneth Wong ken.wong ATM nao.ac.jp~
- 高橋 博之 takahashi ATM cfca.jp~
- 平居 悠 yutaka.hirai ATM nao.ac.jp

//~理論コロキウムの前には台内の発表者による[[ショートコロキウム>Short]]を行っています。 

** Schedule & History [#j2453518]

[[FY2010:http://th.nao.ac.jp/seminar/colloquium/2010/]]
[[FY2011:http://th.nao.ac.jp/seminar/colloquium/2011/index_2011.html]]
[[FY2012:http://th.nao.ac.jp/seminar/colloquium/2012/]] 
[[FY2013:http://th.nao.ac.jp/seminar/colloquium/2013/]] 
[[FY2014:http://th.nao.ac.jp/seminar/?Colloquium2014]] 
[[FY2015:http://th.nao.ac.jp/seminar/?Colloquium2015]] 
[[FY2016:http://th.nao.ac.jp/seminar/?Colloquium2016]] 
[[FY2017:http://th.nao.ac.jp/seminar/?Colloquium2017]] 

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|Date|Speaker|Title|Place/Time|remarks|h
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|[[04/05>#long0404]]|all internal members|self-introduction|Rinko room, Main Building (East) / 13:30|Thursday|
|[[4/10>#long0410]]|Adriana Pohl (Max-Planck Institute of Astronomy, Heidelberg Germany)|Revealing the evolution of planet-forming disks with polarization observations|Lecture room / 13:30|Tuesday|
|[[04/17>#long0417]]|Yoshiaki Kato (Riken)|TBA|Lecture room / 13:30|Tuesday|
|[[04/24>#long0424]]|TBA||Rinko room, Main Building (East) /  13:30|Tuesday|
|[[05/01>#long0501]]|TBA||Lecture room / 13:30|Tuesday|
|[[05/08>#long0508]]|Yoshiyuki Inoue (Riken)|TBA|Rinko room, Main Building (East) /  13:30|Tuesday|
|[[05/08>#long0508]]|Yoshiyuki Inoue (Riken)|Coronal Magnetic Activity in a Nearby Active Supermassive Black Hole|Rinko room, Main Building (East) /  13:30|Tuesday|
|[[05/15>#long0515]]|TBA||Lecture room / 13:30|Tuesday|
|[[05/22>#long0522]]|Kazumi Kashiyama (University of Tokyo)|TBA|Rinko room, Main Building (East) /  13:30|Tuesday|
|[[05/29>#long0529]]|TBA||Lecture room / 13:30|Tuesday|
|[[06/05>#long0605]]|TBA||Lecture room / 13:30|Tuesday|
|[[06/12>#long0612]]|TBA||Lecture room / 13:30|Tuesday|
|[[06/19>#long0619]]|TBA||Lecture room / 13:30|Tuesday|
|[[06/26>#long0626]]|TBA||Lecture room / 13:30|Tuesday|
|[[07/03>#long0703]]|TBA||Lecture room / 13:30|Tuesday|
|[[07/10>#long0710]]|TBA||Lecture room / 13:30|Tuesday|
|[[07/17>#long0717]]|TBA||Lecture room / 13:30|Tuesday|
|[[07/24>#long0724]]|TBA||Rinko room, Main Building (East) /  13:30|Tuesday|
** Confirmed speakers [#hfb505be]

//|[[02/28>#long0228]]| Takashi Shibata (NAOJ)|TBD|Rinko-room/ 13:30||

** Abstract [#id139640]

//:&aname(long0401){4/01}; Name (affiliation) title|
//Abstract

:&aname(long0410){4/10}; Adriana Pohl (Max-Planck Institute of Astronomy, Heidelberg Germany) Revealing the evolution of planet-forming disks with polarization observations|
Recent observational instruments like VLT/SPHERE and ALMA have reached an unprecedented level of resolution and sensitivity. Meanwhile, even the direct observation of substructures in planet-forming disks is within reach, by which the disk evolution can be traced. Features such as gaps, rings, spiral arms and clumps can be either associated with embedded, but yet unseen forming planets, or be related to other internal, physical disk processes. In this talk, I will compare theoretical predictions of dust evolution models and planet-disk interaction processes with current multi-wavelength observations of planet-forming disks. To this end, detailed radiative transfer calculations are presented, which are employed to model observational signatures in disks. An emphasis is placed on polarization diagnostics, which facilitates the detection of light scattered by dust grains in the disk. The latter is a crucial ingredient to constraining the size and composition of dust grains, which is necessary to understand the earliest stages of planet formation.

//
:&aname(long0508){05/08}; Yoshiyuki Inoue (Riken) Coronal Magnetic Activity in a Nearby Active Supermassive Black Hole|
Black hole coronae are believed to be heated by their magnetic activity like the Sun. However, magnetic fields in the vicinity of active supermassive black holes have never been measured. Recently, we proposed a coronal radio synchrotron emission model for Seyfert galaxies. Here, we report the first detection of coronal radio synchrotron emission from a nearby Seyfert galaxy, which enables us to estimate the coronal magnetic field strength. We also found that coronae are composed of thermal and non-thermal electrons. Our results indicate that magnetic activity cannot sustain X-ray emitting coronae. Existence of non-thermal electrons in coronae implies that Seyfert galaxies may explain not only the cosmic X-ray background radiation but also the cosmic MeV gamma-ray background radiation.
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