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硼ȥ2015

硼ȥΥߥʡǤꡢ§Ȥ轵θ13:30鳫ŤƤޤ ֱϤǤѸǤꤤޤ ܸȯɽƤ⹽ޤ Ԥξ硢饤ɤѸǺäƤȽޤ

硼ȥθˤԤޤ

Schedule & History

2010ǯ 2011ǯ 2012ǯ 2013ǯ 2014ǯ

ȯɽȥ/
4/8ʾҲ⥹ / 13:30
4/15аܥ֥ȿʲȸ⥹ / 13:30
4/22߷饹ȥ󥸥ؤdzƲ⥹ / 13:30
5/13īͺWesterlund 2ʬұߥ졼⥹ / 13:30
5/13ë饹ȿưŻҼø⥹ / 14:10
5/20ϱλƱʬ⥹ / 13:30
5/27ƣ̻ĤΥХꥨε⥹ / 13:30
6/3ʤ٤ߡ3DTAݥŤΤ
6/10ʤ٤ߡ󥰥򣲤ijŤ뤿
6/17ʤ٤ߡ󥰥򣲤ijŤ뤿
6/24ʤ٤ߡʪݥ೫ŤΤ
7/1ʤ٤ߡStar Formation WorkshopŤΤ
7/8̾ϥ󥺶ķ¬ˤ뱧ѥ᡼⥹ / 13:30
7/15빾ΤExoplanetary System Dynamics: Multiplicity and Planetary Mass Effects⥹ / 13:30
7/22ⶶǷ֥åۡ˵Ǥιⲹ⥹ / 13:30
10/07(no talk)
10/14(no talk)(two long-colloquium talks)
10/21Masaomi TanakaExploring Short-Timescale Transients in the UniverseConference Room, Cosmos Lodge / 13:30
10/28(no talk)(workshop of theoretical astronomy)
11/04Hiroshi KobayashiRadiation-MHD Simulation of Clumpy Outflow from Supercritical Accretion FlowLecture room / 13:30
11/11(no talk)(intensive lucture by Prof. Kotake)
11/18Shoichi OshinoTerrestrial Planet Formation around Low-Mass Stars: Effect of the Mass of Central StarsConference Room, Cosmos Lodge / 13:30
11/25Seiji ZenitaniTotal Lagrangian Analysis of Electron Orbits in Collisionless Magnetic ReconnectionLecture room / 13:30
12/02Michiko FujiiThe formation and dynamical evolution of young star clustersLecture room / 13:30
12/09(no talk)(NAOJ project week)
12/16(no talk)
12/23(no talk)(rironkon)
1/13Shota Shibagaki1.5D GRMHD simulation of core-collapse supernovaLecture room / 13:30
1/20Toshitaka KajinoIs the standard cosmology perfect? -- A possible evidence for resonant particle creation during inflation from CMB --Conference Room, Cosmos Lodge / 13:30
1/27(no talk)(CfCA user's meeting)
2/03(no talk)
2/10Ken OhsugaNew GR-RMHD code of post K computer eraLecture room / 13:30
2/17Haruo YoshidaSelf-Similar Natural Boundaries of Non-Integrable Dynamical Systems in the Complex t PlaneConference Room, Cosmos Lodge / 13:30

Abstract

4/15()аܥϤ֥ȿʲȸ
аܤ4Ķ륯θϡ˵ζϤΤΤȰۤʤ뤳ȤΤƤ롣ޤΤ褦ʥˤ̤֥Ȥ¸ߤ뤳ȤǧƤ롣δ¬ϡˤ֥Ȥ®äޤΥȤߤαΤΤȤϰۤʤäƤ뤳Ȥ򼨺롣ܸǤϡȤΥʬۤθ֥ȿʲǥ˴ŤаܥΥ̤ȸοʲˤĤĴ٤η̡̩٤ι⤤ʬұ˭٤¸ߤƤСȾؤνŸǥιȥȤιĹΨŪ˵ꡢǴ¬줿̤ΥȤ¸ߤðۤʸƱǤ뤳Ȥ餫ˤޤΤ褦ʱˤúǼȤϡեȤǤϤʤ󾽼úǤǤ뤳Ȥͤߤ᤿
4/22߷(CfCA)饹ȥ󥸥ؤdzƲ
Ķȯ˷ϡȥ󥸥žǽꡢ˥塼ȥΤ¬ǽǤ뤳ȤԤƤ롣桹ϡήˤϥɥޥ饹ȥ󥸥ޥؤžβ򡢾ܺ٤Ĵ٤ֱܹǤ¿ʪξ̩٤ʤɤž ͿƶˤĤƵ롣
5/13īͺ(CfCA)Westerlund 2ʬұߥ졼
Westerlund 2ľ˱Ӥʬұȱ߸̾ʬұ¬Ƥꡢʬұδ֤ˤTeV¸ߤƤ롣桹ϤʬұåȤǥߺѤˤäƷƤΤǤϤʤȹͤåȤ֥ߺѥߥ졼»ܤޤʬұΰ㤤֥̩ʬۤΰ㤤ǤȹͤǥΥܥ塼ե󥰥եѲ׻Ԥäե󥰥եˤϥåȤǥδ֤ŤǤΤʬұϹä¤ˤʤäե󥰥ե礭ˤϥåȤǥݤʬұηϱ߸̾˶ŤȤ򼨤
5/13ë()饹ȿưŻҼø
ɸ̩٤Ķ뤿ᡢϾ¸ǤΤ褦ʶ˸¾ǤʪΤ뤳Ȥ˺Ǥ롣οưξȿǤΤȤʤ뤿ᡢưָפȤǤ뤫⤷ʤμˡ̳ؤȸƤФƤ롣οưľܤȤ館¬ϤۤȤɤʤǶ𥬥ԡǤĤŪưĤäƤ롣ǡ桹ϤνŪư饹ȤǤοưб뤳Ȥǡ饹Ȥξؤ¤ܻؤƤιֱǤϡäŻҼäθ̤줿ϤԤθ̤ɤٽפȤȤˡǶῷ˸ĤäŪư򤳤ޤǤƱȤߤǤ뤫ͤ롣
5/20(CfCA)ϱλƱʬ
ϵ峰ʪǤФʬϷ̤顢۷ǤϻƱ椬ԶѼǤäǽƤ롣ϱפ¬뤳ȤǤε餫ˤʤȹͤ졢ŪˤϹʬǽALMA˾ɬפǤ롣ALMAˤ븶ϱǤΰúǤδ¬顢۷λƱʬۤβܻؤξҲԤ
5/27ƣ̻()ĤΥХꥨε
ŵŪˤĤϻĤȵĤΣĤ礭ʬव뤬ǯδ¬顢㤤Ĥˤyoung massive clusterembedded clusterleaky clusterȤäХꥨ󤬤뤳Ȥ狼äƤĤΥХꥨϤɤΤ褦ޤ줿Τ餫ˤ뤿ˡήʬұȤķߥ졼Ԥäη̡ŷϤŵŪʬұϸŵŪʻĤOB󤬷졢СȶϤŵṲ̄Ĺ̩٤ʬұyoung massive cluster뤳Ȥ狼ä
7/15빾Τ(/)Exoplanetary System Dynamics: Multiplicity and Planetary Mass Effects
ǯηϳõδ¬ѤθȼʣʤϤ¿ȯƤ롣ܸǤϡ2014ǯ12ޤǤ˻®ˡˤäƴ¬줿375500Ĥȡץ顼˾ˤäȯ줿ʣϤ365899(ޤŷ)Ѥ̤Ϥϳع¤δطŪ餫ˤ뤳ȤǡϷʲǥؤο¤βǽõ롣ϤϡϤ濴μ̤ǵʲ̡濴οʲʳ3ĤΥѥ᡼ʬष줾Ϥι¤ŪĴ٤äϤγѱư̷»(AMD)ȥҥȾ¤ǵʲֵƻֳ֤ܤη̡ϤAMDäȼ뤳Ȥ狼äϷ¿ʤۤɡϤǤ뤿ˤϤ줾εƻߵƻ˶᤯ʤФʤʤȤ̣롣ޤȾεƻΥΨʬۤϰۤʤ뤳Ȥ狼ää0.4礭ƻΥΨϤˤΤ¸ߤ롣ˡξϤǤϡƻֳ֤15-30ϰϤȤδ֤ˤ٤ȿ뤳Ȥǧ줿ޤ濴οʲʤˤĤ졢ƻֳ֤ʤ뷹롣ʣϤϳŪ¤ŪˤĤƤޤȤᡢηŪʰ̣ˤĤƵ롣
7/22ⶶǷ(CfCA)֥åۡ˵Ǥιⲹ
֥åۡŷΤͥ͡ڥȥ/ƥӥƥ¬Ƥꡢϥ֥åۡؤΥ̤ˤäƤ꤬ѤȹͤƤ롣פǤϥեȤX˲ä10keV٤ޤǤΤӤXäƤ뤬ιXεϤ狼äƤʤ桹ϤιXεõ뤿ᡢŪռͼήη׻ѤƣŪߥ졼Ԥäη̡֥åۡ˵(r <10 - 15 rg)ռͤǮʿդˤʤʤⲹ뤳Ȥ狼äιⲹ礭ϼˤäƷޤäƤꡢݥ뼧ͥξˤϤΰ褬깭뤳Ȥ狼äˤιⲹβ٤ϥ֥åۡ륹ԥ˱ƶ뤳Ȥ狼äŪˤϥݥ뼧줬֥åۡ뤬žƤ˹ⲹΤ˸äϥ֥åۡβžͥ륮ΰפؤꡢײǮؤȴͿȹͤ롣ȯɽǤϤιⲹι¤ˤĤȯɽ롣
10/21Masaomi Tanaka(DTA)Exploring Short-Timescale Transients in the Universe
The transient sky has been intensively explored by various surveys in the last decade. One of the important discovery spaces for time-domain astronomy is phenomena with a short timescale, ~< 1 day. To explore this frontier, we have recently started a high-cadence transient survey with Subaru telescope. We have discovered five transients showing the rising timescale shorter than 1 day. We find that the event rate of such transients is not negligible compared with supernova rate. In this talk, I will discuss the nature of these short-timescale transients and their implications.
11/4Hiroshi Kobayashi(SOKENDAI/DTA)Radiation-MHD Simulation of Clumpy Outflow from Supercritical Accretion Flow
Clumpy-shaped outflows from supercritical accretion around a stellar mass black hole are reproduced by a global Radiation-MHD simulation (Takeuchi et al. 2013). However, 2D axis symmetry is assumed in the simulations. Hence, we need to confirm the clumpy structure by 3D simulations. In this talk, I will introduce progress report toward achieving this goal.
11/18Shoichi Oshino(CfCA)Terrestrial Planet Formation around Low-Mass Stars: Effect of the Mass of Central Stars
The Kepler space telescope has detected several thousand planets and candidates. Their central stars are mainly FGK-type stars. It is difficult to observe M-stars by using visible light since M-stars have their peak radiation in the infrared region. However, recently there are several survey projects for planets around M-stars such as the InfraRed Doppler (IRD) survey of the Subaru telescope. Therefore it is expected that the number of planets around M-stars will increase in the near future. The habitable zone of M-stars is closer to the stars than that of G-stars. For this reason, the possibility of finding habitable planets is expected to be higher. Here we study the formation of close-in terrestrial planets by giant impacts of protoplanets around low-mass stars by using N-body simulations. An important parameter that controls formation processes is the ratio between the physical radius of a planet and its Hill radius, which decreases with the stellar mass. We systematically change the mass of the central stars and investigate its effects on terrestrial planet formation. We find that the mass of the maximum planet decreases with the mass of central stars, while the number of planets in the system increases. We also find that the orbital separation of adjacent planets normalized by their Hill radius increases with the stellar mass.
11/25Seiji Zenitani(DTA)Total Lagrangian Analysis of Electron Orbits in Collisionless Magnetic Reconnection
Magnetic reconnection is a fundamental process in many plasma systems, ranging from laboratory and solar-terrestrial environments to extreme astrophysical settings. In a collisionless plasma, the magnetohydrodynamic (MHD) approximation no longer hold true in magnetic reconnection, while plasma kinetic physics plays a vital role. From particle viewpoint, these effects stem from complicated particle trajectories in the reconnection system. In this work, we study electron kinetic motion in magnetic reconnection by using particle-in-cell (PIC) simulations. Although it is technically difficult to track electron trajectories in modern PIC simulations, we overcome this barrier by using a simple but effective method. This allows us to examine full trajectories in the reconnection system. We find that electrons undergo Speiser-type motions, as previously predicted. In addition, we find three new classes of electron orbits that were overlooked in previous researches. Basic properties of these motions as well as their observational signatures will be discussed.
12/02Michiko Fujii(DTA) The formation and dynamical evolution of young star clusters
Star clusters and (OB) associations form from giant molecular clouds via clustering star formations. We perform a series of N-body simulations using initial distributions of stars based on the results of hydrodynamical simulations of turbulent molecular clouds. We find that molecular clouds typical in the Milky Way form classical open clusters and associations, but young massive clusters (super star clusters) form from dense massive molecular clouds typical in starburst galaxies. Our simulations also suggest that associations formed as conglomerates of small clusters and they lost their sub-clustering structures during their dynamical evolution.
01/13Shota Shibagaki(DTA) 1.5D GRMHD simulation of core-collapse supernova
I have extended an open-source spherically-symmetric code for core-collapse supernovae, GR1D, so that it can calculate magnetized stellar collapse. This extension is expected to allow us to systematically explore the long term evolution of magnetorotational supernovae from gravitational collapse to proto-neutron star winds. In this talk, I show some test calculations of this code and report the current status of my magnetized stellar collapse simulation.
01/20Toshitaka Kajino(DTA) Is the standard cosmology perfect? -- A possible evidence for resonant particle creation during inflation from CMB --
The CMB power spectrum from both the Planck and WMAP data exhibits a slight dip for multipoles near 20. We show that such a dip could be the result of the resonant creation of massive particles that couple to the inflaton field. For our best-fit models, the epoch of resonant particle creation reenters the horizon at k = 0.0011 +/- 0.0004 (h Mpc^1). The amplitude and location of this feature corresponds to the creation of a number of degenerate fermion species of appropriate mass and coupling constant between the inflaton field and the created fermion species during inflation. Although the evidence is of marginal statistical significance, this could constitute new observational hints of unexplored physics beyond the Planck scale.
02/10Ken Ohsuga(DTA) New GR-RMHD code of post K computer era
Radiation magnetohydrodynamics (RMHD) simulation is a powerful tool in order to investigate the accretion disks and jets around black holes or neutron stars. Ohsuga et al. (2009) performed for the first time RMHD simulations with using non-relativistic code. Recently, general relativistic (GR) RMHD simulations have been performed by the K computer (Takahashi et al. 2016). Also, ultra large-scale GR-RMHD simulations with using the post K computer have been projected. We introduce current progress for preparation of our new GR-RMHD code.
02/17Haruo Yoshida(DTA) Self-Similar Natural Boundaries of Non-Integrable Dynamical Systems in the Complex t Plane
In September 1983, I gave a talk with the same title above at the 6th Kyoto Summer Institute devoted toChaos and Statistical Mechanics. The original abstract was the following; Self-similar structure of the set of singularities (natural boundary) in the complex t plane is explained by the expansion of solution about singularities. Quite recently I started to work again on this subject, but with use of modern technology, i.e., Mathematica (NDSolve, ListPlot3D, etc.). Since this 1983 talk was an epoch making event for my academic career, I will also comment on my personal life before and after this event. Because of the nature of content, this talk will be given in Japanese.