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Colloquium のバックアップの現在との差分(No.15)


  • 追加された行はこの色です。
  • 削除された行はこの色です。
#norelated
* 理論コロキウム2016 [#z407468f]
* DTA Colloquium 2018 [#z407468f]

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。~
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結構です。~
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~
- 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
- 荻原正博 masahiro.ogihara_AT_nao.ac.jp~
- 楠根 貴成 takayoshi.kusune_AT_nao.ac.jp~
- 高橋博之 takahashi_AT_cfca.jp~
- 朝比奈雄太 asahina_AT_cfca.jp~
- 佐々木宏和 hiro.sasaki_AT_nao.ac.jp~
//Number of organizer
// Takiwaki 1
// Ogihara 4
// Kusune 2
// Takahashi 2
// Asahina 2
// Sasaki 1


//~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]

[[2010年度:http://th.nao.ac.jp/seminar/colloquium/2010/]]
[[2011年度:http://th.nao.ac.jp/seminar/colloquium/2011/index_2011.html]]
[[2012年度:http://th.nao.ac.jp/seminar/colloquium/2012/]] 
[[2013年度:http://th.nao.ac.jp/seminar/colloquium/2013/]] 
[[2014年度:http://th.nao.ac.jp/seminar/?Colloquium2014]] 
[[2015年度:http://th.nao.ac.jp/seminar/?Colloquium2015]] 
[[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|Organizer|h
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//
//
|[[4/6>#long0406]]|all internal members|self-introduction|Conference room, Cosmos Lodge / 13:30||
|[[4/13>#long0413]]|Tomoya Takiwaki (NAOJ DTA)|A Clockwork Supernova: precision numerical experiments and their applications|Conference room, Cosmos Lodge / 13:30||
|[[4/20>#long0420]]|Yuki Tanaka (NAOJ CfCA)|Magnetically Driven Wind from Hot Gaseous Planets|Conference room, Cosmos Lodge / 13:30||
|[[4/25>#long0425]]|Kohei Inayoshi (Columbia University)|Hyper-Eddington accretion flows onto massive black holes|Lecture Room/ 13:30||
|[[4/27>#long0427]]|Tetsuo Taki (NAOJ CfCA)|Toward formation of rocky planetesimals: dust and gas density evolution at a local structure of protoplanetary disks|Conference room, Cosmos Lodge / 13:30||
|[[5/11>#long0511]]|Masahiro Ogihara (NAOJ DTA)|Formation of close-in super-Earths|Conference room, Cosmos Lodge / 13:30||
|[[5/18>#long0518]]|Takashi Moriya (NAOJ DTA)|Superluminous supernovae and their origins|Large seminar room / 13:30||
|[[5/25>#long0525]]|Yukari Ohtani (NAOJ CfCA)|Study of relation between emission of supernova shock breakout and central engine activity|Conference room, Cosmos Lodge / 13:30||
|[[6/1>#long0601]]|Shogo Tachibana (Hokkaido University)|Timing of gas clearing of the protosolar disk: Constraints from 129I-129Xe ages of solar-wind-rich meteorites|Conference room, Cosmos Lodge / 13:30||
|[[6/8>#long0608]]|Alessandro Sonnenfeld (IPMU)|Dark matter in early-type galaxies: a lensing view|Conference room, Cosmos Lodge / 13:30||
|[[6/15>#long0615]]|Makoto Takamoto (University of Tokyo)|Relativistic Magnetohydrodynamic turbulence in Poynting-Dominated Plasmas and its effects on Current Sheet Dynamics|Conference room, Cosmos Lodge / 13:30||
|[[6/22>#long0622]]|Takahiro Sumi (Osaka University)|Microlensing exoplanet search toward the solar system analog|Conference room, Cosmos Lodge / 13:30||
|[[6/29>#long0629]]|Carmen Adriana Martínez Barbosa (Leiden Observatory, University of Leiden)|Tracing the journey of the Sun and the solar siblings through the Milky Way|Conference room, Cosmos Lodge / 13:30||
|[[7/6>#long0706]]|Shota Kisaka (Aoyama Gakuin University)|Engine-powered macronovae|Conference room, Cosmos Lodge / 13:30||
|[[7/13>#long0713]]|Tomoaki Matsumoto (Hosei University)|Theoretical Models of Protostellar Binary and Multiple Systems with AMR Simulations.|Conference room, Cosmos Lodge / 13:30||
|[[8/24>#long0824]]|Hui Jiang (Shanghai Maritime University)|  Local Nuclear Mass Relations|Conference room, Cosmos Lodge / 10:30||
|[[8/31>#long0831]]|Sherry Suyu (MPA)| Shedding Light on the Dark Cosmos through Gravitational Lensing|Large Seminar Room / 13:30||
|[[9/21>#long0921]]|Kazunori Akiyama (MIT)|Interstellar Scintillation and Radio Counterpart of the FRBs|Conference room, Cosmos Lodge / 13:30||
|[[9/23>#long0923]]|Akimasa Kataoka (Heidelberg University)|Millimeter polarization of protoplanetary disks due to dust scattering|Conference room, Cosmos Lodge / 11:00|Friday|
|[[10/5>#long1005]]|Toshio Fukushima (NAOJ)|Numerical integration of gravitational field for general three-dimensional objects and its application to gravitational study of grand design spiral arm structure|Conference room, Cosmos Lodge / 13:30||
|[[10/12>#long1012]]|Annop Wongwathanarat (RIKEN)|Linking core-collapse simulations with observations |Conference room, Cosmos Lodge / 13:30||
|[[10/14>#long1014]]|Yiping Shu (the National Astronomical Observatories, Chinese Academy of Sciences)|The BOSS Emission-Line Lens Survey: Strong Lensing of Lyα Emitters by Individual Galaxies|Conference room, Cosmos Lodge / 13:30|Friday|
|[[10/19>#long1019]]|Naoki Yamamoto (Keio University)|Chirality and Astrophysics|Conference room, Cosmos Lodge / 13:30||
|[[10/26>#long1026]]|Chit Hong Yam (JAXA)|Space Missions and Modern Astronomy|Conference room, Cosmos Lodge / 13:30||
|[[11/2>#long1102]]|Sergei Blinnikov (ITEP)|Superluminous Supernovae: Current Status of Research|Conference room, Cosmos Lodge / 13:30||
|[[11/9>#long1109]]|Hisasi Hayakawa (Kyoto University)|Historical Solar Activity before Telescopic Observations-- A New Perspective by Historical Documents --|Rinkoh seminar room / 13:30||
|[[12/9>#long1209]]|Manos Chatzopoulos (Louisiana State University)|Pre-supernova Convection in Massive Stars|Conference room, Cosmos Lodge / 13:30|Friday|
|[[12/14>#long1102]]|Shunsuke Hozumi (Shiga University)|Intrisic Properties of the Bars Formed by the Bar Instability in Flat Stellar Disks|Conference room, Cosmos Lodge / 13:30||
|[[1/11>#long0111]]|Federico García (La Plata)|TBA|Conference room, Cosmos Lodge / 13:30||
|[[1/18?>#long0118]]|Alexander Heger (Monash Center for Astrophysics)|TBA |Conference room, Cosmos Lodge / 13:30||
|[[1/25>#long0125]]|Fumi Egusa(NAOJ)|TBA|Conference room, Cosmos Lodge / 13:30||
|[[2/1>#long0201]]|Ryo Tazaki (Tokyo Institute of Technology)|TBA|Conference room, Cosmos Lodge / 13:30|Wednesday|
|[[2/15>#long0215]]|Alexey Tolstov (Kavli IPMU)|TBA|Conference room, Cosmos Lodge / 13:30||
|[[3/1>#long0301]]|Tatsuya Satsuka (Osaka University)|TBA|Conference room, Cosmos Lodge / 13:30|Wednesday|
|[[04/05>#long0404]]|all internal members|self-introduction|Rinko room, Main Building (East) / 13:30|Thursday|Takiwaki|
|[[04/10>#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|Ogihara|
|[[04/17>#long0417]]|Yoshiaki Kato (Riken)|Radiation MHD Simulations of Waves and Vortices on the Sun and beyond|Lecture room / 13:30||Takahashi|
|[[04/24>#long0424]]|Akihiro Suzuki (NAOJ)|Multi-dimensional modeling of supernova ejecta with a central energy source|Rinko room, Main Building (East) /  13:30||Ogihara|
|[[05/08>#long0508]]|Yoshiyuki Inoue (Riken)|Coronal Magnetic Activity in a Nearby Active Supermassive Black Hole|Rinko room, Main Building (East) /  13:30||Asahina|
|[[05/10>#long0510]]|Keiichi Maeda(Kyoto University)|Progenitor Evolutions and Explosion Mechanisms of Type Ia Supernovae|Rinko room, Main Building (East) /  15:00|Thursday|Asahina|
|[[05/15>#long0515]]|Kyohei Kawaguchi (ICRR)|Radiative-transfer simulation for the optical and near-infrared electromagnetic counterparts to GW170817|Lecture room / 13:30||Takahashi|
|[[05/22>#long0522]]|Kazumi Kashiyama (University of Tokyo)|The repeating fast radio burst and the young neutron star model|Rinko room, Main Building (East) /  13:30||Ogihara|
|[[05/29>#long0529]]|ShingChi Leung (IPMU)|Pulsation Pair-instability Supernova: Connection to massive black hole, circumstellar medium and collapsar|Lecture room / 13:30||Sasaki|
|[[06/05>#long0605]]|Doris Arzoumanian (Nagoya University)|Observed properties of nearby molecular filaments|Lecture room / 13:30||Kusune|
|[[06/12>#long0612]]|Teppei Minoda (Nagoya University)|The effect of the primordial magnetic fields on the cosmic microwave background anisotropy|Lecture room / 13:30||Kusune|
|[[06/26>#long0626]]|TBA||Rinko room / 13:30|||
|[[07/03>#long0703]]|Shota Notsu (Kyoto University)|Possibility to locate the position of the H2O snowline in protoplanetary disks through spectroscopic observations|Lecture room / 13:30||Ogihara|
|[[07/10>#long0710]]|Riouhei Nakatani (University of Tokyo)|Radiation Hydrodynamics Simulations of Photoevaporation of Protoplanetary Disks: Metallicity Dependence of UV and X-Ray Photoevaporation|Lecture room / 13:30||Kusune|
|[[07/17>#long0717]]|TBA||Lecture room / 13:30|||
|[[07/24>#long0724]]|Shunsuke Ideguchi (NAOJ)|Basics of Faraday Tomography Technique and Its Applications to Cosmic Magnetism Study|Rinko room, Main Building (East) /13:30||Sasaki|

** Confirmed speakers [#hfb505be]

Masaki Yamaguchi (U Tokyo)
//|[[06/19>#long0619]]|Hirotaka Hohokabe (NAOJ)|TBA|Lecture room / 13:30||Sasaki|
//|[[02/28>#long0228]]| Takashi Shibata (NAOJ)|TBD|Rinko-room/ 13:30||

** Abstract [#id139640]

:&aname(long0413){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.
//:&aname(long0401){4/01}; Name (affiliation) title|
//Abstract

:&aname(long0420){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.
:&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(long0425){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.
//
:&aname(long0417){04/17}; Yoshiaki Kato (Riken) Radiation MHD Simulations of Waves and Vortices on the Sun and beyond|
One of the long-standing problems in solar physics is to understand a
mechanism which maintains the solar atmosphere.  The chromosphere, a
layer between the photosphere and the corona, is a key to unveiling
the mystery of the solar atmosphere.  It is yet to be revealed
entirely by observations because the chromosphere has complex
structure and rapid variability.  Therefore, radiation
magnetohydrodynamic (RMHD) simulations play a major role for
understanding such a complexity, which is difficult to interpret
physical processes.
I introduce my recent publications on the effect of MHD waves
associated with an isolated magnetic flux concentration (or a flux
tube), which is anchored in the photosphere and extended over the
corona.  This is a classical problem which is extensively discussed in
many literatures and probably the best example to understanding MHD
waves.  While all studies so far relied on inflicting driving forces
in the photosphere, only a self-consistent RMHD simulation of the
solar atmospheric layers from the surface convection zone to the
corona can resolve the realistic nature of MHD waves.
First, I present the generation and propagation of mostly slow mode
waves, driven by magneto-convective processes in the deep photosphere
and beneath it.  This is so-called magnetic pumping process which
generates slow modes that propagate upward and develop into shock
waves in the chromosphere.  The magnetic pumping is a robust mechanism
for generating shock waves in the vicinity of strong flux tube at the
chromospheric height and therefore it’s most likely to sustain the
chromosphere.  Second, I present the identification of torsional waves
in the chromosphere and the corona.  Vortical flows in the upper
convection zone and the photosphere force magnetic field structures to
rotate and thus produce so-called solar “magnetic tornadoes”, which
extend into the corona.  Unlike slow modes, large portions of
torsional modes can reach the corona without suffering significant
dissipation and therefore it’s capable of sustaining the corona.
Third, I present the detection of physical phenomena in the flux tube
by magnetic pumping imprinted on the spectral lines.  Thanks to the
rapidly advancing solar observations over the past decades, we will
have an unique opportunity to grasp the quantitative nature of MHD
waves in the near future.  It will enable us to extend our knowledge
of plasma into those of the other astrophysical objects.  Finally, I
will briefly talk about the future perspective on my research in the
next decades.

:&aname(long0427){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.

:&aname(long0511){5/11}; Masahiro Ogihara (NAOJ DTA) Formation of close-in super-Earths|
Recent observations of exoplanets have revealed a large number of
close-in low-mass planets (or close-in super-Earths). As of April
2016, 351 systems harbor 877 close-in super-Earths. We can discuss the
origin of these planets by comparing observed orbital distributions
with results of numerical simulations of planet formation. In this
talk, I will introduce our recent papers on formation of close-in
super-Earths (Ogihara et al. 2015, A&A, 578; Ogihara et al. 2015,
A&AL, 584). I will also show some preliminary results of ongoing
projects.
//
:&aname(long0424){04/24}; Akihiro Suzuki (NAOJ) Multi-dimensional modeling of supernova ejecta with a central energy source|
Core-collapse supernova explosions are of fundamental importance in the universe. They are an outcome of massive star formation and evolution and at the same time affect their surrounding environments in various ways. This is the reason why many supernova researches and surveys have been intensively conducted. One of the remarkable successes of modern transient survey programs is the discovery of an extremely bright class of core-collapse supernovae, called superluminous supernovae. Because of their high brightness, we can detect high-z events, potentially making it possible to probe star-forming activity even in the high-z universe. However, the problem is that the energy source of their bright emission is still debated. A promising scenario for superluminous supernovae is the central engine scenario, in which the compact remnant (highly rotating neutron star, black hole accretion disk, or whatever) left in the supernova ejecta play a role in giving rise to bright thermal emission. However, there are many remaining problems, such as, how exactly the additional energy deposition is realized and how the supernova ejecta with a central engine evolve. I’m lately investigating the hydrodynamic evolution of supernova ejecta with such a central energy source by using multi-dimensional numerical simulations. In this talk, after a brief introduction of supernovae, I present results of my recent studies.

:&aname(long0518){5/18}; Takashi Moriya (NAOJ DTA) Superluminous supernovae and their origins|
Superluminous supernovae (SLSNe) are newly recognized class of core-collapse supernovae (SNe). Their existence is realized only about a decade ago. They are more than 10 times brighter than other core-collapse SNe. The reasons why they can become very bright are still not understood well. It is currently known that there are two distinct spectral types in SLSNe, namely, Type II (those with hydrogen features) and Type I (those without them). Type II SLSNe show narrow spectral features which are likely from dense circumstellar media surrounding the SN ejecta. I will present the numerical modeling of the collision between SN ejecta and dense circumstellar media and show that the interaction between SN ejecta and dense circumstellar media can indeed explain Type II SLSNe. Origins of Type I SLSNe are more mysterious. I will discuss several works of mine related to the luminosity source of Type I SLSNe. I will especially focus on the Type I SLSN iPTF13ehe which did not show hydrogen features at the beginning but started to show them one year after its luminosity peak. I suggest that the delayed hydrogen features may be an evidence of Type I SLSN progenitors evolving in close massive binary systems.
//
:&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.

:&aname(long0525){5/25}; Yukari Ohtani (NAOJ CfCA) Study of relation between emission of supernova shock breakout and central engine activity|
Shock breakout radiation originate as thermal emission from the shock passing through the outer layer of the star. It can provide the first information on how supernova explodes, no matter how relativistic the explosion is. There have been an question about the relativistic jet associated with a hypernova, of which explosion energy is ten times higher than that of an ordinary core-collapse supernova. The question is, how the central engine of the jet works. In order to obtain information on the central engine activity, it might be worth studying the emission properties of ultra-relativistic shock propagating into the dense circumstellar matter (CSM). For example, influence of bulk-Compton scattering on the spectrum can be a powerful indicator of the shock evolution, but there have been no theoretical study on that. In this talk, I will introduce our numerical study on the relationship between the behavior of an ultra-relativistic shock and the spectral properties of shock breakout emission. Using a Monte-Carlo method, we calculate the temporal spectral evolution of ultra-relativistic shock breakout in the CSM. We found that if the shock velocity monotonically decreases with time, photons with relatively high energies tend to appear fast. That is because the bulk kinetic energy of the shocked matter decreases. On the other hand, if the shock velocity increases with time, there are only slight changes in the spectrum. Therefore, in principle, it might be possible to obtain information on the activity of the jet central engine from the observable properties of ultra-relativistic shock breakout.
//
:&aname(long0510){05/10}; Keiichi Maeda(Kyoto University) Progenitor Evolutions and Explosion Mechanisms of Type Ia Supernovae|
I will provide a review on the current status of observational constraints on the progenitor systems and explosion mechanisms of type Ia Supernovae (SNe Ia). Recent development in the field is highlighted by accumulating observational discoveries of diversities found for SNe Ia. An idea is emerging that SNe Ia are perhaps not at all a uniform system as previously believed for many years, and thermonuclear explosions may lead to various outcomes which could correspond to various types of transients. In this talk, I will summarize different observational constraints placed for different sub-types of SNe Ia and related phenomena, and connect these findings to different types of progenitors and modes of explosions which have been theoretically predicted.

//6/1
:&aname(long0601){6/1}; Shogo Tachibana (Hokkaido University) Timing of gas clearing of the protosolar disk: Constraints from 129I-129Xe ages of solar-wind-rich meteorites|
Planets in the solar system and extrasolar planets form in protoplanetary disks, which are the natural outcome of the star formation.  The protosolar gas disk also dispersed after the formation of Jupiter and Saturn, resulting in the insufficient gas accretion onto later-formed Uranus and Neptune cores.  However, there has been no chronological constraint when the gas disk dispersed in the solar system.  Here we found that solar-wind-rich portions of gas-rich chondrite breccias are about 10 million years younger than the oldest solar system solid objects using a 129I-129Xe relative chronometer.  The solar-wind gas implantation into asteroids must have occurred in the absence of disk gas, and thus the disk gas was cleared out completely ~10 million years after the first solid formation.  This could also be the first direct constraint on the timing of the onset of Jupiter and Saturn formation as ~3 million years after the first solid formation.
//
:&aname(long0515){05/15}; Kyohei Kawaguchi (ICRR) Radiative-transfer simulation for the optical and near-infrared electromagnetic counterparts to GW170817|
Recent detection of gravitational waves from a binary-neutron star merger (GW170817) and the subsequent observations of electromagnetic counterparts provide a great opportunity to study the physics of compact binary mergers. The optical and near-infrared counterparts to GW170817 are found to be consistent with a kilonova/macronova scenario with red and blue components. However, in most of previous studies in which contribution from each ejecta component to the lightcurves is separately calculated and composited, the red component is too massive as dynamical ejecta and 
the blue component is too fast as post-merger ejecta. In this talk, I present our recent works performing 2-dimensional radiative-transfer simulations for a kilonova/macronova consistently taking the interplay of multiple ejecta components into account, and show that the lightcurves of optical and near-infrared counterparts can be reproduced naturally by a setup consistent with the prediction of the numerical-relativity simulations.

//6/8
:&aname(long0608){6/8}; Alessandro Sonnenfeld (IPMU) Dark matter in early-type galaxies: a lensing view|
Dark matter halos play a crucial role in the formation and evolution of galaxies but observational constraints on the distribution of dark matter are currently very poor.Gravitational lensing is a very powerful tool for measuring galaxy masses at cosmological distances and provides a unique opportunity for probing the distribution of dark matter in the most massive galaxies.
By statistically combining the lensing signal from a large set of galaxies we explored how the average dark matter distribution correlates with the properties of the baryonic component. Strong lensing constraints reveal an anticorrelation between galaxy size and dark matter mass enclosed within 5kpc. At larger scales, probed by weak lensing, we observe a positive correlation between halo mass and the velocity dispersion of the central galaxy, at fixed stellar mass.
These results could have a significant impact on our understanding of the formation and evolution of massive galaxies.
//
:&aname(long0522){05/22}; Kazumi Kashiyama (University of Tokyo) The repeating fast radio burst and the young neutron star model|
Fast radio bursts (FRBs) are enigmatic radio transients with large dispersion measure. There are ~ 30 of FRBs discovered so far and only one of them, FRB121102, repeats. Recently, the host galaxy and persistent radio counterpart have identified for this repeating FRB. First, I will overview the observational results and the general implications. Then, I will focus on the young neutron star model for FRBs and discuss how one can test the model observationally. In particular, I will discuss the possible connection between FRBs and energetic supernovae.


// 6/15
:&aname(long0615){6/15}; Makoto Takamoto (University of Tokyo) Relativistic Magnetohydrodynamic turbulence in Poynting-Dominated Plasmas and its effects on Current Sheet Dynamics|
Many astrophysical phenomena are considered that the ambient plasma is very high-Reynolds number flows, and should be in a turbulent state. In particular, many high energy astrophysical phenomena are also believed to be in high-sigma state, that is, the plasma is in a Poynting-dominated state. To investigate such phenomena, we need a theory of turbulence of relativistic magnetohydrodynamics (RMHD) with relativistically strong background magnetic field. However, there are very few study of relativistic turbulence, and many properties are still unknown.
In this seminar, we report on our recent findings of the RMHD turbulence in a Poynting-dominated plasma, in particular, effects of compression mode. We performed a series of 3-dimensional RMHD simulations with decaying trans-Alfvenic turbulence. We found that the generation of compressible mode shows different behavior from non-relativistic case, such as an increase of compression mode power with back ground sigma parameter and effects from shock waves. We also discuss the turbulent effects on magnetic reconnection.
//
:&aname(long0605){06/05}; Doris Arzoumanian  (Nagoya Universiry) Observed properties of nearby molecular filaments|
The highly filamentary structure of the interstellar medium is impressively revealed by the unprecedented quality and sky coverage of Herschel and Planck images tracing the Galactic cold dust emission. These observations provide the required data to describe in detail the properties of the filamentary structures observed in both quiescent clouds and in star forming regions, where the densest filaments appear to be the main sites of star formation. 
The omnipresence of filaments in observations as well as in numerical simulations suggests that the formation of filamentary structures is a natural product of the interplay between interstellar shock waves, gravity, and magnetic fields. The detailed description of their observed properties is important to improve our understanding of their formation and evolution process. 
I will present what we have learned about the properties of the filamentary structures derived from Herschel dust continuum and ground based single dish molecular line observations, and I will discuss the observational constraints on the formation and evolution of molecular filaments. 

//6/22
:&aname(long0622){6/22}; Takahiro Sumi (Osaka University) Microlensing exoplanet search toward the solar system analog|
Although thousands of exoplanets have been found by various methods,
not many solar system planets analogs have been detected.
Some Jupiter and Saturn analogs and a few Earth-like plants have been found only very recently.
Gravitational microlensing has an unique sensitivity to exoplanets outside the snow-line
down to the Earth-mass, where the planetary formation is very active. 
The MOA-II and OGLE-IV carries out microlensing exoplanet search toward the
Galactic Bulge in New Zealand and Chile, respectively.
These surveys are detecting various kinds of systems, including the Jupiter-Saturn analog, 
the Neptune analog and the 2-Earth mass planet at 1AU around one of the binary stars.
The Wide Field Infrared Survey Telescope (WFIRST) is the NASA's future large space mission,
which is scheduled to be launched in 2024.
The exoplanet microlensing program is one of the primary science of WFIRST. 
WFIRST will find about 3000 bound planets and 2000 unbound planets by the high
precision continuous survey with 15 min. cadence, which is sensitive to all the solar system 
analogs except the mercury.  WFIRST can complete the statistical census of
planetary systems in the Galaxy, from the outer habitable zone to the outside of the snow-line 
and gravitationally unbound planets &#8211; a discovery space inaccessible to other exoplanet detection techniques.
//
:&aname(long0612){06/12}; Teppei Minoda  (Nagoya University) The effect of the primordial magnetic fields on the cosmic microwave background anisotropy|
The magnetic fields are ubiquitous on the astronomical objects, from asteroids to clusters of galaxies. The origin of these cosmic magnetic fields is unknown, however, while the magnetogenesis in the early universe (such as inflation, the cosmic phase transition, the perturbation evolution, and so on) might be able to explain it. Magnetic fields generated by such cosmological mechanisms are called the primordial magnetic fields (PMFs), and some papers have pointed that the PMFs induce the matter density fluctuation due to their Lorentz force, and also affect the gas temperature distribution through a magnetic dissipation, so-called “ambipolar diffusion”.
We consider these effects and calculate the time evolution of the baryon gas density and temperature before the formation of the first stars and galaxies. And we suggest a method to investigate such primordial gas structure with the cosmic microwave background (CMB) temperature anisotropy.
In this talk, I will briefly introduce the PMFs and its general formalism, and review some basic concepts of the standard cosmology and CMB physics. Next, I will talk about the effect of the PMFs on the baryon gas history, and finally show the calculation method and the results of my recent work (Minoda et al., 2017, Phys. Rev. D, 96, 123525).

//
:&aname(long0703){07/03}; Shota Notsu (Kyoto University) Possibility to locate the position of the H2O snowline in protoplanetary disks through spectroscopic observations|
Observationally locating the position of the H2O snowline in protoplanetary disks is important for understanding the planetesimal and planet formation processes, and the origin of water on Earth. The velocity profiles of emission lines from disks are usually affected by Doppler shift due to Keplerian rotation. Therefore, the line profiles are sensitive to the radial distribution of the line-emitting regions. 
In our studies (Notsu et al. 2016, ApJ, 827, 113; 2017, ApJ, 836, 118; 2018, ApJ, 855, 62), we calculated the chemical composition of the disks around a T Tauri star and a Herbig Ae star using chemical kinetics, and then the H2(16)O and H2(18)O line profiles. We found that lines with small Einstein A coefficients and relatively high upper state energies are dominated by emission from the hot midplane region inside the H2O snowline, and therefore through analyzing their profiles the position of the H2O snowline can be located. 
In addition, we found that H2(18)O lines trace deeper into the disk than H2(16)O lines since the number density of H2(18)O is low (Notsu et al. 2018). Thus these H2(18)O lines are potentially better probes of the position of the H2O snowline at the disk midplane, depending on the dust optical depth. Moreover, H2(18)O and para-H2(16)O lines with relatively lower upper state energies (~a few 100K) can also locate the position of the H2O snowline. There are several candidate water lines that trace the position of the H2O snowline in ALMA Bands 5−10. Finally, we have proposed the water line observations for a Herbig Ae disk HD163296 in ALMA Cycle 3, and partial data were delivered. We constrain the line emitting region (the location of the H2O snowline) and the dust properties from the observations.

//6/29
:&aname(long0629){6/29}; Carmen Adriana Mart&iacute;nez Barbosa (Leiden Observatory, University of Leiden) Tracing the journey of the Sun and the solar siblings through the Milky Way|
The products of radioactive elements found in the meteorite fossil record and the high eccentricities of objects located in the outer regions of the Solar System, suggest that the Sun was born in an open cluster 4.6 Gyr ago. Such an open cluster however, was quickly destroyed by the intense gravitational field of the Galaxy. As a conse- quence, the stars that were born together with the Sun, the so-called solar siblings, might be currently dispersed all over the Galactic disk.~
In this talk I will explain how open cluster simulations can help us in predicting the current phase-space coordinates of the solar siblings. These simulations include the gravitational forces within the cluster, the effects of stellar evolution on the cluster population and the gravitational force due to the Milky Way. The result of these sim- ulations will serve as a guide to search for solar siblings in future surveys such as the Gaia mission and GALAH. The identification of solar siblings is of crucial importance to understand the environment where the Solar system was formed and the place in the Galaxy where the Sun was born.
//
:&aname(long0710){07/10}; Riouhei Nakatani (University of Tokyo) Radiation Hydrodynamics Simulations of Photoevaporation of Protoplanetary Disks: Metallicity Dependence of UV and X-Ray Photoevaporation|
Protoplanetary disks are thought to have lifetimes of several million yr in the solar neighborhood, but recent observations suggest that the disk lifetimes are shorter in a low-metallicity environment. We
perform a suite of radiation hydrodynamics simulations of photoevaporating disks with varying the metallicity to study their long-term evolution and the metallicity dependence of mass-loss rates.
Our simulations follow hydrodynamics, radiative transfer, and nonequilibrium chemistry in a self-consistent manner. Dust-grain temperatures are also calculated consistently by solving the radiative
transfer of the stellar irradiation and grain (re-) emission. In the fiducial case with solar metallicity, including the X-ray effects does not significantly increase the photoevaporation rate when compared to
the case with ultra-violet (UV) radiation only.  At sub-solar metallicities in the range of Z &#8819;  10^{-1.5} Zsun, the photoevaporation rate increases as metallicity decreases owing to the reduced opacity of the disk medium. The result is consistent with the observational trend that disk lifetimes are shorter in low metallicity environments. Contrastingly, the photoevaporation rate decreases at even lower metallicities of Z &#8818; 10^{-1.5} Zsun, because dust-gas collisional cooling remains efficient compared to far UV photoelectric heating whose efficiency depends on metallicity. The net cooling in the interior of the disk suppresses the photoevaporation. However, adding X-ray radiation significantly increases the photoevaporation rate, especially at Z ~ 10^{-2} Zsun. Although the X-ray radiation itself does not drive strong photoevaporative flows, X-rays penetrate deep into the neutral region in the disk, increase the ionization degree there, and reduce positive charges of grains. Consequently, the effect of photoelectric heating by far UV radiation is strengthened by the X-rays and enhances the disk photoevaporation.

:&aname(long0706){7/06}; Shota Kisaka (Aoyama Gakuin University) Engine-powered macronovae|In 2015, a gravitational-wave (GW) signal was directly detected from a merger of a binary black hole (BH) for the first time. GW signals are expected to be generated not only by mergers of binary BHs, but also by mergers of neutron star (NS) binaries (NS-NS and BH-NS binaries). NS binary mergers may also power bright electromagnetic (EM) signals, because the ejection of normal matter during mergers is thought to be responsible. EM counterparts have been focused on to maximize the scientific return from the detection of GWs. One of the most promising EM signatures are macronovae (or kilonovae): approximately isotropic emissions from heated merger ejecta. Although the r-process radioactivity is widely discussed as an energy source, it requires a huge mass of ejecta from a NS binary merger to explain the observed macronova candidates. As an alternative, we propose that macronovae are energized by the central engine, i.e., a BH or NS, and the injected energy is emitted. The engine model allows a wider parameter range, especially smaller ejecta mass than the r-process model. We also discuss the implications for the engine-powered model for the search of EM counterparts to GWs.

// 7/13
:&aname(long0713){7/13}; Tomoaki Matsumoto (Hosei University) Theoretical Models of Protostellar Binary and Multiple Systems with AMR Simulations.|We present theoretical models for protostellar binary and multiple systems based on the high-resolution numerical simulation with an adaptive mesh refinement (AMR) code, SFUMATO.  The recent ALMA observations reveal early phases of the binary and multiple star formation with high spatial resolutions.  The observations should be compared with theoretical models with also high spatial resolutions.  We present two theoretical models for (1) a high density molecular cloud core, MC27, and (2) a protobinary system, L1551 NE.  For the model for MC27, we performed numerical simulations for gravitational collapse of a turbulent cloud core. The cloud core exhibits fragmentation during the collapse, and dynamical interaction between the fragments produces an arc-like structure, which is one of the prominent structures observed by ALMA.  The effects of the magnetic field are also discussed with MHD simulations. For the model for L1551 NE, we performed numerical simulations of gas accretion onto protobinary.  The simulations exhibit asymmetry of circumbinary disks.  Such asymmetry was also found by ALMA in the circumbinary disk of L1551 NE.

// 8/24
:&aname(long0824){8/24}; Hui Jiang (Shanghai Maritime University)  Local Nuclear Mass Relations |The masses are the basic properties of atomic nuclei. In this talk, we will discuss the Garvey-Kelson mass relations as one of the best example schemes of local nuclear mass relations and, report in particular our recent results of researches which we have carried out in the Shanghai Jiao Tong University. The essential point is how to use and improve the Garvey-Kelson relations. We plan to apply our result to explosive nucleosynthesis in SNe.

// 8/31
:&aname(long0831){8/31}; Sherry Suyu (MPA)  Shedding Light on the Dark Cosmos through Gravitational Lensing| Gravitational lensing provides powerful means to study dark energy and dark matter in the Universe.  In particular, strong lens systems with measured time delays between the multiple images can be used to determine the "time-delay distance" to the lens, which is primarily sensitive to the Hubble constant.  Measuring the Hubble constant is crucial for inferring properties of dark energy, spatial curvature of the Universe and neutrino physics.  I will describe the ingredients and newly developed techniques for measuring accurately time-delay distances with a realistic account of systematic uncertainties.  A program initiated to measure the Hubble constant to <3.5% in precision from gravitational lens time delays is in progress, and I will present the latest results and their implications.  Current and upcoming imaging surveys will contain thousands of new time-delay lenses, and I will describe ongoing efforts to find these objects.  An exciting discovery is the first strongly lensed supernova, which has offered a rare opportunity to perform a true blind test of model predictions.  I will describe the bright prospects of using gravitational lens time delays as an independent and competitive cosmological probe.

:&aname(long0921){9/21}; Kazunori Akiyama (MIT) Interstellar Scintillation and Radio Counterpart of the FRBs|
Fast radio bursts (FRBs) are one of the most intriguing sources, not only for astrophysical processes causing one of the most energetic but shortest bursts in the universe but also for their astronomical aspect of a unique probe for the intergalactic medium. Searches for counterparts of FRBs --- for instance, associated aftergrows are of significant importance for their localization. 
Refractive Interstellar scintillation is a critical consideration for searches for identification of associated aftergrows at radio wavelengths. The tenuous ionized interstellar medium along the line of sight can introduce rapid variability of compact radio sources such as active galactic nuclei (AGNs) on timescales comparable to potential aftergrows of the FRBs. Thus, it is quite essential to distinguish between associated aftergrows and rapidly variable scintillating sources close to FRBs.
We have recently demonstrated a fundamental importance of the refractive scintillation for identification of the radio counterpart in a theoretical study on the effect of scintillation of the FRB 150418 (Akiyama & Johnson 2016, ApJL) that Keane et al. 2016 have recently discovered with a promising radio counterpart at 5.5 and 7.5 GHz --- a rapidly decaying source on timescales of ~ 6 days. The analytical theory of refractive scattering and our numerical simulations show that the reported observations on FRB 150418 are consistent with scintillating radio emission from the core of a radio-loud AGN having a brightness temperature of Tb &#8819; 10^9 K, compatible with LLAGN and faint blazars.
In this talk, I introduce FRBs and interstellar scintillation with our recent works on the FRB 150418. I also briefly discuss implications for future surveys of radio counterparts of compact objects such as FRBs and gravitational waves.

// 9/23
:&aname(long0923){9/23}; Akimasa Kataoka (Heidelberg University) Millimeter polarization of protoplanetary disks due to dust scattering |To measure if dust grains have grown to beyond millimeter sizes in protoplanetary disks, usually measurements of the spectral slope are used. However, the interpretation of millimeter spectral slopes in terms of grain size is unreliable. We have found a completely independent way to measure grain sizes in this size and wavelength regime: scattering polarization. If grains are grown to the comparable size of the wavelengths i.e., (sub)mm, dust grains scatter the thermal emission. The scattered emission is polarized by nature. The star itself is dark at millimeter wavelengths, the main source of the radiation is thermal dust emission itself. If a protoplanetary disk has a slight anisotropy such as lopsided or ring-shaped dust density distribution, the residual polarization is up to 2.5 %, which is observable with ALMA. Moreover, it explains measured polarization of emission from e.g. HL Tau. It turns out that this also allows for an independent measurement of the grain sizes; we have constrained the maximum grain sizes to be 150 &#181;m. Also, we report our polarization observations with ALMA toward one of the brightest protoplanetary disks, which show an evidence of the self-scattering.  This allows for a new probe of the grain growth in protoplanetary disks.


//10/5
:&aname(long1005){10/5}; Toshio Fukushima (NAOJ) Numerical integration of gravitational field for general three-dimensional objects and its application to gravitational study of grand design spiral arm structure|
We present a method to integrate the gravitational field for general three-dimensional objects. By adopting the spherical polar coordinates centered at the evaluation point as the integration variables, we numerically compute the volume integral representation of the gravitational potential and of the acceleration vector. The variable transformation completely removes the algebraic singularities of the original integrals. The comparison with exact solutions reveals around 15 digits accuracy of the new method. Meanwhile, the 6 digit accuracy of the integrated gravitational field is realized by around $10^6$ evaluations of the integrand per evaluation point, which costs at most a few seconds at a PC with Intel Core i7-4600U CPU running at 2.10 GHz clock. By using the new method, we show the gravitational field of a grand design spiral arm structure as an example. The computed gravitational field shows not only spiral shaped details but also a global feature composed of a thick oblate spheroid and a thin disc. The developed method is directly applicable to the electromagnetic field computation by means of Coulomb's law, the Biot-Savart law, and their retarded extensions. Sample {\sc fortran} 90 programs and test results are electronically available. (Ref. T. Fukushima 2016, MNRAS, doi:10.1093/mnras/stw2078)

:&aname(long1012){10/12}; Annop Wongwathanarat (RIKEN) Linking core-collapse simulations with observations |
Core-collapse supernovae (CCSNe) are one of the most exciting astrophysical
phenomena. The question of how massive stars die is a long-standing
problem in theoretical astrophysics. Recently observations of young
nearby CCSN remnants provide increasingly great details of the morphology and
chemical composition of the remnants. Such information will help us to decipher
the puzzle of the CCSN explosion mechanism. However, in order to understand
a wide variety of properties of CCSN remnants long-time CCSN simulations
must be performed. There is currently a missing link between simulations and
observations because long-time CCSN simulations are computationally very
demanding. In this talk, I will report results from state-of-the-art 3D long-time
CCSN simulations, and present what we could learn about the explosion mechanism
and the CCSN progenitor star from these results.


:&aname(long1014){10/14}; Yiping Shu (the National Astronomical Observatories, Chinese Academy of Sciences) The BOSS Emission-Line Lens Survey: Strong Lensing of Lyα Emitters by Individual Galaxies|
We present Hubble Space Telescope (HST) F606W-band imaging observations of 21 galaxy-Lyα emitter lens candidates in the Baryon Oscillation Spectroscopic Survey (BOSS) Emission-Line Lens Survey (BELLS) for GALaxy-Lyα EmitteR sYstems (BELLS GALLERY) survey. 17 systems are confirmed to be definite lenses with unambiguous evidence of multiple imaging. The lenses are primarily massive early-type galaxies (ETGs) at redshifts of approximately 0.55, while the lensed sources are Lyα emitters (LAEs) at redshifts from 2 to 3. The HST imaging data are well fit by smooth lens models consisting of singular isothermal ellipsoids in an external shear field. The Einstein radii of the BELLS GALLERY lenses are on average 60% larger than those of the BELLS lenses because of the much higher source redshifts which will allow a detailed investigation of the radius evolution of the mass profile in ETGs. With the aid of the average &#8764; 13× lensing magnification, the LAEs are resolved to comprise individual star-forming knots of a wide range of properties with characteristic sizes from less than 100 pc to several kpc, rest-frame far UV apparent AB magnitudes from 29.6 to 24.2, and typical projected separations of 500 pc to 2 kpc.


:&aname(long1019){10/19}; Naoki Yamamoto (Keio University) Chirality and Astrophysics|
Elementary particles, such as electrons and neutrinos, possess the property of chirality. This microscopic property modifies the macroscopic hydrodynamic behavior and leads to unusual chiral transport phenomena in relativistic systems. We argue that these chiral effects are potentially important for the origin of magnetars and core-collapse supernova explosions.

:&aname(long1026){10/26}; Chit Hong Yam (JAXA) Space Missions and Modern Astronomy|
In the past 50 years, there are over a hundred telescopes and astronomical devices launched to space and they have contributed in modern astronomy in various aspects. Space observation has two main advantages over ground-based telescopes: the absence of atmospheric disturbance and absorption. While the problem of atmospheric disturbance can be partially corrected by optical techniques, the observation of wavelengths absorbed by the atmosphere cannot be performed with ground-based telescopes. This talk presents the opportunities provided by space observatories and the challenges of designing and operating such missions. Basic orbital mechanics and spacecraft systems are introduced to explain how we can plan and operate a space mission to fulfill its scientific objectives. Past and future missions such as the Hubble Space Telescope, WMAP, SOHO, Kepler, LISA will be used as examples. Although space telescopes are much more expensive than ground-based telescopes, their values have been demonstrated in numerous important findings and will continue to help us answer some fundamental questions in astronomy, such as the origin of the universe, the formation and evolution of celestial objects and systems, and the possibility of extraterrestrial life. 

:&aname(long1102){11/2}; Sergei Blinnikov (ITEP) Superluminous Supernovae: Current Status of Research|
Many supernovae are discovered in last decade with peak luminosity
one-two orders of magnitude higher than for normal supernovae of known
types. They are called Superluminous supernovae: SLSNe.
This is a challenge for theory, since even normal supernovae are
not yet completely understood from the first principles.
The models explaining those events with the minimum energy budget
involve multiple ejections of mass in presupernova stars.
The radiative shocks produced in collisions of those shells may
provide the required power of light.
This class of the models is refered to as "interacting'' supernovae.
I concentrate on the non-trivial problems of this scenario for SLSNe:
stability of the shells, on "bumps" in the light curves, and on the
broad lines often observed in their spectra.

:&aname(long1109){11/9}; Hisasi Hayakawa (Kyoto University) Historical Solar Activity before Telescopic Observations -- A New Perspective by Historical Documents --|This presentation provides possibility and importance of historical documents for astronomical studies. Solar Activity is studied both on respects of long-term activity and extreme space events. We have 400-year data for sunspot drawings since Gallillei and 150-year data for flares since Carrington event. However, recent studies for the sun require longer time-scaled finding rare and extreme events such as "superflares", superflares, whose total enery of  about 10^(33-38) erg, 10-10^6 times lager than that of the largest solar foares on the Sun and whose frequency is calculated once hundreds to thousand years. Historical documents can partially cover this shortage, recording low latitude auroras and naked-eye sunspots as proxies for solar activity. Thus, in this presentation, the presenter aims at introducing examples of aurora records in Carrington event in comparison with contemporary magnetic latitude of observational sites and showing further possibility of historical documents for astronomy. This approach casts a new perspectives for extreme events as large as or even larger than the Carrington event in our sun.


:&aname(long1209){12/9}; Manos Chatzopoulos (Louisiana State University) Pre-supernova Convection in Massive Stars|
The interior of a massive star in the final years prior to core-collapse supernova is in a state of violent unrest.
Vigorous convective shell burning of silicon, oxygen and carbon drives large scale plume motions that can
interact with each other and significantly alter the structure of the progenitor star. Under such conditions
the star departs from perfect hydrostatic equilibrium and spherical symmetry and may experience dynamical pulses
that, in some cases, can lead to episodic mass-loss. I will present preliminary results from
multidimensional simulations of convection in massive stars in the few seconds to hours preceding the supernova
explosion. The proper, dynamical multidimensional treatment of convection will be bench-marked against
parametrized one-dimensional mixing length theory predictions and the implications for realistic
core-collapse supernova progenitor models will be discussed. I will also present a new method
to characterize pre-supernova convection, the method of Vector Spherical Harmonics decomposition, and
discuss how it can be used to make realizations of core-collapse models in future simulations.


:&aname(long1214){12/14}; Shunsuke Hozumi (Shiga University) Intrisic Properties of the Bars Formed by the Bar Instability in Flat Stellar Disks|
Recent observations have revealed that some properties of galactic
bars have been uncovered on a statistically meaningful levels of
accuracy using a large sample of galaxies.  As a result, it has
been found that bars in SB0-SBb galaxies are longer than those in
SBc to SBd galaxies.  Furthermore, also found are such properties
that the longer bars have larger amplitudes, and show more elongated
shapes.  However, these systematic bar properties have never been
explained physically. In this talk, I show the properties of the bars formed by the
bar instability for flat stellar disk models which are constructed
on the basis of exact equilibrium distribution functions.  Then, 
I demonstrate that the properties of the simulated bars are, in
large measure, similar to those of the observed bars, and that
the amplitude, length, and axis ratio are strongly correlated to
an initial typical Toomre's Q value.  Taking into consideration
these results, I discuss what the Hubble sequence represents.

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