11月16日（月）13：30～15：00 太陽系小天体セミナー 南棟2階会議室
Nov 16 Mon Solar System Minor Body Seminar Conference Room, South Bldg.2F
11月18日（水）10：30～12：00 総研大コロキウム 中央棟（東）輪講室
Nov 18 Wed SOKENDAI colloquium Rinko-shitsu,Main Bldg.(East)
11月18日（水）14：10～15：10 理論コロキウム コスモス会館 会議室
Nov 18 Wed DTA Colloquium Conference Room, Cosmos Lodge
11月20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
Nov 20 Fri Solar and Space Plasma (SSP) Seminar Student Seminar Room, Subaru bldg.
11月20日（金）16：00～17：00 国立天文台談話会 大セミナー室
Nov 20 Fri NAOJ Seminar Large Seminar Room
詳細は以下をご覧下さい。
11月16日(月)
- キャンパス
- 三鷹
- セミナー名
- 太陽系小天体セミナー
- 臨時・定例の別
- 定例
- 日時
- 11月16日（月曜日）13時30分～15時
- 場所
- 南棟２階会議室
- 講演者
- 蓮尾隆一
- 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
11月18日(水)
- Campus
- Mitaka
- Seminar Name
- SOKENDAI colloquium
- Regular/Irregular
- Regular
- Date
- 10:30-12:00, Nov 18, 2015
- Place
- 輪講室 (IP: 133.40.2.203)
- Speaker 1
- Misaki Ando
- Affiliation
- M1, SOKENDAI(supervisor: Daisuke IONO, Masao SAITO, Daniel ESPADA)
- Title
- The 12CO and 13CO Distribution in Merging Starburst Galaxy NGC 1614
- Speaker 2
- Masaki Yoshida
- Affiliation
- M1, SOKENDAI(supervisor: Suematsu Yoshinori)
- Title
- Estimating a coronal magnetic field in flaring active region using a NLFFF(NonLinear Force-Free Field)
- Organizer
- Name : Ryosuke Nagasawa
- Comment
- TV conference connection is available from Hawaii, Nobeyama, Mizusawa and Okayama.
11月18日(水)
- Campus
- Mitaka
- Seminar
- DTA colloquium
- Regular/Irregular
- Regular
- Date
- 18 Nov 2015, 14:10-15:10
- Place
- Conference Room, Cosmos Lodge
- Speaker
- Kazem Ardaneh (U of Tsukuba)
- Title
- Collisionless Weibel shocks and electron acceleration in gamma-ray bursts
- Abstract
- A study of collisionless external shocks in gamma-ray bursts is presented. The shock structure, electromagnetic fields, and process of electron acceleration are assessed by performing a self-consistent 3D particle-in-cell (PIC) simulation. In accordance with hydrodynamic shock systems, the shock consists of a reverse shock (RS) and forward shock (FS) separated by a contact discontinuity (CD). The development and structure are controlled by the ion Weibel instability. The ion filaments are sources of strong transverse electromagnetic fields at both sides of the double shock structure over a length of 30 – 100 ion skin depths. Electrons are heated up to a maximum energy E_ele = E_b**0.5, where E_ele is the energy normalized tothe total incoming energy. Jet electrons are trapped in the RS transition region due to the presence of an ambipolar electric field and reflection by the strong transverse magnetic fields in the shocked region. In a process similar to shock surfing acceleration (SSA) for ions, electrons experience drift motion and acceleration by ion filament transverse electric fields in the plane perpendicular to the shock propagation direction. Ultimately accelerated jet electrons are convected back into the upstream. The FS region shows the characteristic of a double layer plasma. In this region, acceleration of the electrons by the double layer electric fields creates a power-law distributed population in the electron distribution function. In the present work, the power-law index for the electron distribution function in the precursor region is α =1.8, which can be associated to the radio afterglow emission.
- Contact
- – Name: Seiji Zenitani
11月20日(金)
- キャンパス
- 三鷹
- セミナー名
- 太陽天体プラズマセミナー
- 臨時・定例の別
- 定例
- 日時
- 11月20日（金）13:30-15:00
- 場所
- 院生セミナー室
- 講演者
- David Orozco Suarez
- 所属
- Instituto de Astrofisica de Canarias (IAC)
- タイトル
- Inferring the magnetic field vector in chromospheric
structures: the diagnostic potential of the He 1083nm triplet - Abstract
-
The solar chromosphere is permeated by solar structures such as sunspots, surges, flare ribbons, prominences (filaments) or spicules, where non-local thermodynamic equilibrium effects dominate the state of the plasma and where the magnetic fields are expected to be much lower in intensity than in the photosphere underneath. These solar chromospheric structures are being observed mainly in quasi-monocromatic wavelengths or with spectroscopy. However, imaging and spectroscopic observations do not contain information for allowing the inference of the magnetic field vector, except perhaps through the analysis of waves.
Measuring magnetic fields in the chromosphere requires the observation of spectral lines in polarization. In particular, spectral lines that show the joint action of atomic level polarization and the Hanle and Zeeman effect such as the He 1083nm triplet are of great interest.
Here, a brief overview of the diagnostic potential of the He 10830 nm triplet for measuring chromospheric plasmas and its application to solar chromospheric structures is given, with particular emphasis on the magnetic structure of solar prominences and spicules. - 連絡先
- 名前：鳥海森
11月20日(金)
- キャンパス
- 三鷹
- セミナー名
- 国立天文台談話会
- 臨時・定例の別
- 定例
- 日時
- 11月20日 (金) 16:00-17:00
- 場所
- 大セミナー室
- 講演者
- Andreas Schulze
- 所属
- Kavli IPMU
- タイトル
- The evolution of the mass functions of active SMBHs and their host galaxies out to z～2
- Abstract
-
Understanding the influence of black hole growth on star formation and galaxy evolution over cosmic time scales requires a census of the AGN population, in particular in respect to their black hole masses, accretion rates and host galaxy stellar masses. I will review our current understanding of the demographics of the AGN population in respect to these fundamental quantities.
I first discuss the importance and current observational constraints on the active black hole mass function (BHMF) and the Eddington ratio distribution function (ERDF) for type 1 AGN. Recent work, utilizing both shallow, large area (SDSS) and deep, small area (VVDS, zCOSMOS) optical surveys could reliably disentangle the evolutionary trend seen in the AGN LF into its physical processes of black hole mass downsizing and accretion rate evolution. We are witnessing the shutoff of AGN activity, preferentially in the most massive black holes, from z=2 to z=0, which drives the evolution of the AGN LF.
I will further discuss recent work on establishing the AGN host galaxy stellar mass function of both type 1 and type 2 AGN out to z～2.5, based on the XMM hard X-ray selected AGN sample in the COSMOS field. In contrast to previous studies, we find significant evolution in the shape of the specific accretion rate distribution function out to z～2.5. I will also address implications for the quenching of star formation via AGN feedback. - 連絡先
- 名前：久保 雅仁
以上