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Colloquium のバックアップ(No.7)


理論コロキウム2016

理論コロキウムは原則として毎週水曜日の午後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
  • 守屋 尭 takashi.moriya_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

Schedule & History

2010年度 2011年度 2012年度 2013年度 2014年度 2015年度

DateSpeakerTitlePlace/Timeremarks
4/6all internal membersself-introductionConference room, Cosmos Lodge / 13:30
4/13Tomoya Takiwaki (NAOJ DTA)A Clockwork Supernova: precision numerical experiments and their applicationsConference room, Cosmos Lodge / 13:30
4/20Yuki Tanaka (NAOJ CfCA)Magnetically Driven Wind from Hot Gaseous PlanetsConference room, Cosmos Lodge / 13:30
4/25Kohei Inayoshi (Columbia University)Hyper-Eddington accretion flows onto massive black holesLecture Room/ 13:30
4/27Tetsuo Taki (NAOJ CfCA)Toward formation of rocky planetesimals: dust and gas density evolution at a local structure of protoplanetary disksConference room, Cosmos Lodge / 13:30
5/11Masahiro Ogihara (NAOJ DTA)TBAConference room, Cosmos Lodge / 13:30
5/18Takashi Moriya (NAOJ DTA)TBALarge seminar room / 13:30
5/25Yukari Ohtani (NAOJ CfCA)TBAConference room, Cosmos Lodge / 13:30
6/1Shogo Tachibana (Hokkaido University)TBAConference room, Cosmos Lodge / 13:30
6/8Alessandro Sonnenfeld (IPMU)TBAConference room, Cosmos Lodge / 13:30
6/15Makoto Takamoto (Tokyo University)TBAConference room, Cosmos Lodge / 13:30
6/22Takahiro Sumi (Osaka University)TBAConference room, Cosmos Lodge / 13:30
7/6Shota Kisaka (Aoyama Gakuin University)TBAConference room, Cosmos Lodge / 13:30

Confirmed speakers

Abstract

4/13 Tomoya Takiwaki (NAOJ DTA) A Clockwork Supernova: precision numerical experiments and their applications
Core-collapse supernovae are flamboyant explosions at death of massive stars. They control the circulation of matter in the universe, and inevitably they affect or are affected by a lot of astrophysical objects, such as supernova remnants, neutron stars, black holes, interplanetary disks and stars. The central engine of the explosion, however, remains in mystery. Elaborate numerical experiments try to uncover that. Stimulated by such precise simulations, phenomenological approaches are recently developed.In this seminar, I introduce the status of the supernova simulations and broaden applications of them.
4/20 Yuki Tanaka (NAOJ CfCA) Magnetically Driven Wind from Hot Gaseous Planets
Several transit observations in the UV band have been suggested that hot Jupiters have high-temperature hydrogen upper atmospheres, and the existence of a large amount of atmospheric escape from the upper atmospheres. For example, a mass-loss rate from the hot Jupiter HD 209458b is estimated to be at least 10^10 g/s. It is thought that heating by the XUV radiation from central stars is the main mechanism to drive the atmospheric escape, but a driving mechanism of atmospheric escape that includes planetary magnetic fields has not been investigated so far. Here I propose a new mechanism in which the atmospheric escape is driven by the dissipation of magnetohydrodynamic (MHD) waves. I performed MHD simulations and show that the dissipation of MHD waves in the upper atmosphere can drive a large amount of atmospheric escape and also can heat up the upper atmosphere. I also discuss parameter dependence of the mass-loss rate and atmospheric structures.
4/25 Kohei Inayoshi (Columbia University) Hyper-Eddington accretion flows onto massive black holes
How fast can black holes (BHs) grow? The existence of bright quasars at high-redshift provides a challenging puzzle about the origin of supermassive BHs. To form such massive objects within a billion year, rapid growth of seed BHs is required. We study very-high rate, spherically symmetric accretion flows onto massive BHs embedded in dense metal-poor clouds. We find solutions from outside the Bondi radius at hyper-Eddington rates, unimpeded by radiation feedback. Accretion rates in this regime are steady, and larger than 5000 L_Edd/c^2. At lower rates, the accretion is episodic due to radiative feedback and the average rate is below the Eddington rate. The hyper-Eddington accretion solution is maintained as long as the emergent luminosity is limited to < (10-30) L_Edd because of photon trapping due to electron scattering. We apply our result to the rapid formation of massive BHs in protogalaxies. Once a seed BH forms at the center of the galaxy, it can grow to a maximum ~ 10^5 Msun via gas accretion independent of the initial BH mass.
4/27 Tetsuo Taki (NAOJ CfCA) Toward formation of rocky planetesimals: dust and gas density evolution at a local structure of protoplanetary disks
The radial drift barrier is one of the most serious problem in the planetesimal formation process. We focus on a local disk structure called "radial pressure bump (Whipple, 1972; Haghighipour & Boss, 2003a, b)”. When a protoplanetary disk has the radial pressure bump, dust particles are trapped at a point where gas pressure is radially maximized. We investigate simultaneous evolution of dust and gas density profiles at a radial pressure bump. We find that the bump structure is flattened by a drag force from dust onto gas when the dust-to-gas mass ratio reaches ~1. Although the pressure bump is a favorable place for streaming instability (SI; Youdin & Goodman, 2005), the flattened bump structure inhibits SI from forming large particle clumps corresponding to 100-1000 km sized bodies, which has been previously proposed. If SI occurs there, the dust clumps formed would be 10-100 times smaller, that is, of about 1 - 100 km.
5/11 Masahiro Ogihara (NAOJ DTA) title
Abstract