Colloquium ¤Î¥Ð¥Ã¥¯¥¢¥Ã¥×¤Î¸½ºß¤È¤Îº¹Ê¬(No.50)

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* DTA Colloquium 2018 [#z407468f]

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- ÂìÏÆÃÎÌé takiwaki.tomoya_AT_nao.ac.jp~
- ÊÒ²¬ ¾Ï²í akimasa.kataoka_AT_nao.ac.jp~
- Kenneth Wong ken.wong ATM nao.ac.jp~
- ¹â¶¶ ÇîÇ· takahashi ATM cfca.jp~
- Ê¿µï Íª yutaka.hirai ATM nao.ac.jp
- ²®¸¶ÀµÇî masahiro.ogihara_AT_nao.ac.jp~
- Æïº¬ µ®À® takayoshi.kusune_AT_nao.ac.jp~
- ¹â¶¶ÇîÇ· takahashi_AT_cfca.jp~
- Ä«ÈæÆàÍºÂÀ asahina_AT_cfca.jp~
- º´¡¹ÌÚ¹¨ÏÂ hiro.sasaki_AT_nao.ac.jp~
//Number of organizer
// Takiwaki 1
// Ogihara 4
// Kusune 2
// Takahashi 2
// Asahina 2
// Sasaki 1

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** Schedule & History [#j2453518]

[[2010Ç¯ÅÙ:http://th.nao.ac.jp/seminar/colloquium/2010/]]
[[2011Ç¯ÅÙ:http://th.nao.ac.jp/seminar/colloquium/2011/index_2011.html]]
[[2012Ç¯ÅÙ:http://th.nao.ac.jp/seminar/colloquium/2012/]]
[[2013Ç¯ÅÙ:http://th.nao.ac.jp/seminar/colloquium/2013/]]
[[2014Ç¯ÅÙ:http://th.nao.ac.jp/seminar/?Colloquium2014]]
[[2015Ç¯ÅÙ:http://th.nao.ac.jp/seminar/?Colloquium2015]]
[[2016Ç¯ÅÙ:http://th.nao.ac.jp/seminar/?Colloquium2016]]
[[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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//
//
|[[4/5>#long0405]]|all internal members|self-introduction|Conference room, Cosmos Lodge / 13:30||
|[[4/12>#long0412]]|Shing Chi Leung (Kavli IPMU)|Nucleosynthesis of Type Ia supernovae|Conference room, Cosmos Lodge / 13:30||
|[[4/17>#long0417]]|Toshihiko Kawano (LANL/Tokyo Tech)|beta-delayed neutron emission and fission for r-process nucleosynthesis|Conference room, Cosmos Lodge / 13:30||
|[[4/19>#long0419]]|Masaki Yamaguchi (U. Tokyo)|The number of black hole-star binaries discovered by the astrometric satellite, Gaia|Conference room, Cosmos Lodge / 13:30||
|[[4/26>#long0426]]| Tomohisa Kawashima (NAOJ DTA)|Radiation hydrodynamic simulations of super-critical accretion columns onto neutron stars in ULX-pulsars|Conference room, Cosmos Lodge / 13:30||
|[[5/08>#long0508]]| Jonathan C. Tan (University of Florida)| Inside-Out Planet Formation |Conference room, Cosmos Lodge / 13:30||
|[[5/10>#long0510]]| Shinpei Shibata (Yamagata University)| Physics of The Rotation Powered Pulsar |Conference room, Cosmos Lodge / 13:30||
|[[5/17>#long0517]]| Tomohiro Ono (Kyoto University)| Large-scale Gas Vortex Formed by the Rossby Wave Instability |Rinkoh room / 13:30||
|[[5/24>#long0524]]| Naonori Sugiyama (IPMU)| Kinematic Sunyaev-Zel'dovich effect|Conference room, Cosmos Lodge / 13:30||
|[[5/31>#long0531]]| Shogo Ishikawa (NAOJ CfCA)|The Galaxy-Halo Connection in High-redshift Universe|Conference room, Cosmos Lodge / 13:30||
|[[6/7>#long0607]]| Tomoya Kinugawa (U. Tokyo)|Compact binary remnants from first stars for the gravitational wave source|Conference room, Cosmos Lodge / 13:30||
|[[6/12>#long0612]]|Yama&#231; Pehlivan (Mimar Sinan University)|Stars as extreme laboratories for neutrino physics|Conference room, Cosmos Lodge / 13:30||
|[[6/14>#long0614]]|Cemsinan Deliduman (Mimar Sinan University)|Astrophysics with Weyl Gravity|Rinkoh room / 13:30||
|[[6/21>#long0621]]|Hiroyuki Kurokawa (ELSI, Tokyo Tech)|Hydrodynamics of first atmospheres of planets embedded in protoplanetary disk|Conference room, Cosmos Lodge/ 13:30||
|[[6/28>#long0628]]| Masanobu Kunitomo (Nagoya University)|Revisiting the pre-main sequence evolution of low-mass stars: Importance of accretion and deuterium abundance|Conference room, Cosmos Lodge / 13:30||
|[[7/5>#long0705]]| Yuta Asahina (NAOJ CfCA)| MHD Simulations of the Feedback via an AGN outflow to the inhomogenious interstellr medium |Conference room, Cosmos Lodge / 13:30||
|[[7/12>#long0712]]| Shoko Oshigami (NAOJ CfCA)|Mare volcanism: Reinterpretation based on Kaguya Lunar Radar Sounder data|Conference room, Cosmos Lodge / 13:30||
|[[7/19>#long0719]]| Shinsuke Takasao (Nagoya University)| MHD Simulations of Accretion onto Star from Surrounding Disk|Conference room, Cosmos Lodge / 13:30||
|[[7/26>#long0726]]| Jean Coupon (University of Geneva)|Probing the galaxy-mass connection in TeraByte-scale imaging surveys|Conference room, Cosmos Lodge / 13:30||
|[[9/27>#long0927]]| Takayoshi Kusune (NAOJ)|Magnetic field of the bright-rimmed cloud SFO 74|Conference room, Cosmos Lodge / 13:30||
|[[10/03>#long1003]]| Matthew Kenworthy (Leiden Observatory)|Looking for exorings towards Beta Pictoris, J1407 and PDS 110 |Conference room, Cosmos Lodge / 13:30||
|[[10/04>#long1004]]| Yuri Aikawa (University of Tokyo)|Deuterium Fractionation in Protoplanetary Disks|Conference room, Cosmos Lodge / 13:30||
|[[10/10>#long1010]]| Peter Behroozi (University of Arizona)|Maximizing Inference from Galaxy Observations|Conference room, Cosmos Lodge / 13:30|Tuesday|
|[[10/18>#long1018]]| Ryosuke Hirai (Waseda University)|Understanding core-collapse supernovae in binaries with various numerical approaches|Conference room, Cosmos Lodge / 13:30||
|[[10/19>#long1019]]| Sergey Blinnikov (Institute for Theoretical and Experimental Physics )|GRB Central Engines within Superluminous Supernovae and their environment|Conference room, Cosmos Lodge / 13:30|Thursday|
|[[10/25>#long1025]]| Sho Fujibayashi (Kyoto University)|The evolution and mass ejection from the remnant of the binary neutron star merger|Conference room, Cosmos Lodge / 13:30||
|[[11/01>#long1101]]|No colloquium|NAOJ decadal workshop |||
|[[11/02>#long1102]]|Wanggi Lim (NAOJ)|Dust in Infrared Dark Clouds|Conference room, Cosmos Lodge / 13:30|Thursday|
|[[11/08>#long1108]]|No colloquium|DTA workshop 2017 |||
|[[11/15>#long1115]]| Sanemichi Takahashi (Kogakuin University)| Early evolution of protoplanetary disks: a ring-gap structure formation |Conference room, Cosmos Lodge / 13:30||
|[[11/22>#long1122]]| Wolfgang Loeffler (Heidelberg ARI)|Gaia Sky: A 3D visualisation of the Gaia Catalogues|Conference room, Cosmos Lodge / 13:30||
|[[11/29>#long1129]]|No colloquium|CfCA UM |||
|[[12/06>#long1206]]| Kazuyuki Sugimura (Tohoku University)| Accretion onto seed BHs: the impacts of anisotropic radiation and gas angular momentum|Conference room, Cosmos Lodge / 13:30||
|[[12/20>#long1220]]| Yutaka Hirai (NAOJ)|The role of enrichment of heavy elements in the chemodynamical evolution of dwarf galaxies|Conference room, Cosmos Lodge / 13:30||
|[[01/17>#long0117]]| Kohei Hayashi (NAOJ)|The universal dark halo scaling relation for the dwarf spheroidal galaxies in the Local Group|Conference room, Cosmos Lodge / 13:30||
|[[01/24>#long0124]]| Hiroshi Kobayashi (NAOJ)|Three-Dimensional Radiation-Hydrodynamic Simulation of Clumpy Outflow and Its Application to Supercritical Accretors around Black Holes *practice for the PhD defence. *in Japanese  |TBD / 13:30||
|[[01/31>#long0131]]| Misako Tatsuuma (UTokyo)|Gravitational Instability of a Dust Layer Composed of Porous Silicate Dust Aggregates in a Protoplanetary Disk *practice for the master thesis defence. *in Japanese  |Rinko-room/ 13:30||
|[[01/31>#long0131]]| Kanji Mori (UTokyo)|Quantum Mechanical Constraint on Carbon Fusion Reaction and Its Impact on Type Ia Supernovae  *practice for the master thesis defence. *in Japanese  |Rinko-room/ 14:15||
|[[02/21>#long0221]]| Kaiki Inoue (Kinki University)|TBD|Rinko-room / 13:30||
|[[03/28>#long0328]]| Tomoyuki Hanawa (Chiba University)|Conservation of Total Energy Including Gravity in Hydrodynamical Simulations|Lecture-room/ 13:30||

|[[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|
|[[07/24>#long0724]]|Shunsuke Ideguchi (NAOJ)|Basics of Faraday Tomography Technique and Its Applications to Cosmic Magnetism Study|Rinko room, Main Building (East) /13:30||Sasaki|
|[[10/02>#long1002]]|Richard Teague (University of Michigan) |Observing the Kinematics of Planet-Disk Interactions with ALMA|Lecture room / 13:30||Kusune|
|[[10/11>#long1011]]| Hector O. Silva (Montana State University)|Illuminating the strong-field regime of gravity|Conference room, N6 3F / 14:00|Thursday|Kusune|
|[[10/11>#long1011]]| George Papas (Sapienza University of Rome)|Testing the Kerr hypothesis with QNMs and ring downs |Conference room, N6 3F / 14:00|Thursday|Kusune|
|[[10/16>#long1016]]|Kazunari Iwasaki (Osaka University) |The formation of molecular clouds by compression of atomic gases|Lecture room /14:30||Kusune|
|[[10/30>#long1030]]|Yen-Chen Pan (NAOJ) |Understanding Type Ia Supernova with UV Spectroscopy|Lecture room /13:30||Takiwaki|
|[[11/12>#long1112]]|Sylvain Bontemps(Bordeaux University)|NAOJ Seminar|Large Seminar Room/16:00|||
|[[11/20>#long1120]]|Yuri Fujii (Nagoya University) |Formation of Circumplanetary Disks and Regular Moons|Lecture room /13:30||Ogihara|
|[[12/04>#long1204]]|DTA workshop |||||
|[[12/11>#long1211]]|Daisuke Nakauchi (Tohoku University) |Ionization degree and magnetic diffusivities in the low-metallicity star-formation|Lecture room /13:30||Asahina|
|[[01/08>#long0108]]|Hiroshi Kobayashi (Nagoya University) |From Dust to Planet via Collisional Growth|Large seminar room /13:30||Ogihara|
|[[01/15>#long0115]]|CfCA UM |||||
|[[01/22>#long0122]]|Jun Kumamoto (University of Tokyo) |Gravitational-Wave Emission from Binary Black Holes Formed in Open Clusters|Conference room, N6 3F /13:30||Asahina|
|[[02/07>#long0207]]|Hiroshi Kimura (Chiba Institute of Technology)| The Evolution of Organic Matter in the Universe |Large Seminar Room/13:00||Sasaki|
|[[02/12>#long0212]]|Kei Tanaka (Osaka University/ NAOJ)| Massive Star Formation under Multiple Feedback Processes|Lecture room/13:30||Sasaki|
|[[02/18>#long0218]]|Takashi Shibata (NAOJ)|Coalescence condition of planetesimals|Lecture room/ 13:30||Takiwaki|
|[[02/26>#long0226]]|Hirotaka Hohokabe (NAOJ)|Flow structures around growing protoplanets with hydrodynamic simulations|Lecture room / 13:30||Takiwaki|
|[[03/05>#long0305]]|Scott Suriano (University of Tokyo)|The Formation of Rings and Gaps in Magnetized Wind-Launching Disks|Lecture room / 13:30||Ogihara|
|[[03/12>#long0312]]|Shingo Hirano (Kyusyu University)|Environmental dependence of the first star formation|Conference room, N6 3F / 13:30 ||Asahina|
** Confirmed speakers [#hfb505be]

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

** Abstract [#id139640]

:&aname(long0412){4/12}; Shing Chi Leung (Kavli IPMU) Nucleosynthesis of Type Ia supernovae|
Type Ia supernovae (SNe Ia) are an important class of astrophysical objects. They are the standard candles of the universe and the major sources of iron-peak elements. It is known to be the explosion of a carbon-oxygen white dwarf by thermonuclear runaways. However, many theoretical uncertainties still persist, for example whether the progenitor of SNe Ia belongs to single degenerate or double degenerate scenario. Furthermore, the diversity in observations, such as the subclasses of Type Iax or super-luminous SNe Ia, suggests that the standard picture using the explosion of a Chandrasekhar mass white dwarf is insufficient to explain the variety of the observed SNe Ia. To resolve these, a systematic understanding in SNe Ia nucleosynthesis becomes necessary. In this present, I shall present hydrodynamics and nucleosynthesis results of multi-dimensional models for the explosion phase of SNe Ia. We explore the effects of model parameters on the explosion energetic and its chemical production. The influences of our SNe Ia models to galactic chemical evolution are discussed. I also present constraints on the progenitor properties of some recently observed SNe Ia and their remnants.
//:&aname(long0401){4/01}; Name (affiliation) title|
//Abstract

:&aname(long0417){4/17}; Toshihiko Kawano (LANL/Tokyo Tech) beta-delayed neutron emission and fission for r-process nucleosynthesis|
We give a brief summary of our recent development of nuclear reaction
theories with a particular focus on nuclear data production for the
r-process nucleosynthesis. The topics include calculations of the
beta-delayed process for neutron-rich nuclei, where several neutrons
can be emitted, and eventually fission may take place as well.
Our recent studies on fission itself are also given.
:&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(long0419){4/19}; Masaki Yamaguchi (U. Tokyo) The number of black hole-star binaries discovered by the astrometric satellite, Gaia|
Although it is believed that there are 10^8-9 stellar mass black holes (BH) in Milky Way, until now only ~60 BHs have been discovered. Moreover, masses of only a dozen BHs of them are constrained. By discovering more BHs and estimating their masses, we would obtain the mass distribution of BHs with a higher confidence level. This distribution is expected to constrain a theoretical model of the supernova explosion in which a BH is produced as a remnant.
Gaia is now operated and have a capability to detect binaries with an unseen companion, such as a BH or a neutron star. Gaia performs a high-precision astrometry with the optical band (0.3-1.0um), and surveys a whole sky, where main observational targets are stars. If a target star has an unseen companion, it should show an elliptical motion on the celestial sphere. Gaia can confirm the companion by detecting such motion. Moreover, this elliptical motion leads to all orbital elements, which enables us to estimate the mass of companion. If this mass is larger than 3 solar masses, we can confirm the companion as a BH.
In my talk, I will show how many BHs can be detected by such method with Gaia. Considering the binary evolution, we obtain the number of detectable BHs, ~600, for main sequence targets. This means that Gaia can discover the order of one thousand BHs whose masses can be found, although we know only a dozen such BHs now. We conclude that the astrometric observation for binaries is very powerful method for finding BHs.
//
:&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¡Çs 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 ¡Èmagnetic tornadoes¡É, which
extend into the corona.  Unlike slow modes, large portions of
torsional modes can reach the corona without suffering significant
dissipation and therefore it¡Çs 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(long0426){4/26}; Tomohisa Kawashima (NAOJ) Radiation hydrodynamic simulations of super-critical accretion columns onto neutron stars in ULX-pulsars|
Ultraluminous X-ray sources are off-centered, extragalactic X-ray sources with luminosities exceeding the Eddington limit for stellar-mass black holes. After the recent discovery of pulsed X-ray emissions in three ULXs, it is widely thought that some ULXs are powered by super-critical column accretion onto neutron stars. The mechanism of super-critical column accretion is, however, still poorly understood. We have, therefore, carried out two-dimensional radiation hydrodynamic simulations of super-critical accretion columns onto neutron stars, and have found that the super-critical accretion can be realized because the most photons escape from the side wall of accretion columns (i.e., the radiation field is anisotropic in the accretion columns). The simulated accretion columns are luminous enough to be consistent with the observed ULX-pulsars.

:&aname(long0508){5/08}; Jonathan C. Tan (University of Florida) Inside-Out Planet Formation |
The Kepler-discovered systems with tightly-packed inner planets (STIPs), typically with several planets of Earth to super-Earth masses on well-aligned, sub-AU orbits may host the most common type of planets in the Galaxy. They pose a great challenge for planet formation theories, which fall into two broad classes: (1) formation further out followed by migration; (2) formation in situ from a disk of gas and planetesimals. I review the pros and cons of these classes, before focusing on a new theory of sequential in situ formation from the inside-out via creation of successive gravitationally unstable rings fed from a continuous stream of small (~cm-m size) "pebbles," drifting inward via gas drag. Pebbles first collect at the pressure trap associated with the transition from a magnetorotational instability (MRI)-inactive ("dead zone") region to an inner MRI-active zone. A pebble ring builds up until it either becomes gravitationally unstable to form an Earth to super-Earth-mass planet directly or induces gradual planet formation via core accretion. The planet continues to accrete until it becomes massive enough to isolate itself from the accretion flow via gap opening. The process repeats with a new pebble ring gathering at the new pressure maximum associated with the retreating dead-zone boundary. I discuss the theory¡Çs predictions for planetary masses, relative mass scalings with orbital radius, and minimum orbital separations, and their comparison with observed systems. Finally I speculate about potential causes of diversity of planetary system architectures, i.e. STIPs versus Solar System analogs.
//
:&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¡Çm 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(long0510){5/10}; Shinpei Shibata (Yamagata University) Physics of The Rotation Powered Pulsar|
I review physics of the rotation powered pulsars with special interest of how the energy and angular momentum are emitted from the system. I will mention briefly an recent observational result that torque on the neutron stars varies with various time scales. This talk is given in Japanese.
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:&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(long0517){5/17}; Tomohiro Ono (Kyoto University) Large-scale Gas Vortex Formed by the Rossby Wave Instability|
Large-scale gas vortexes induced by the Rossby wave instability (RWI) are one of the plausible explanations of the lopsided structures recently observed in several protoplanetary disks. For comparison with the observations, it is important to investigate quantitatively the properties of the vortexes formed by the RWI. However, our knowledge on the properties and outcomes of the RWI has been limited until recent years. We have studied the RWI with linear stability analyses and hydrodynamical simulations using the Athena++ code. As a result of the linear stability analyses, we show that the RWI is one of the shear instabilities which are explained by the interaction between two Rossby waves. We also derive the critical condition for the onset of the RWI in semi-analytic form. From the numerical simulations, we investigate the properties of the vortexes formed by the RWI and discuss possible observational predictions. In my talk, I will present our three results on the RWI: (1) the physical mechanism, (2) the critical condition for the onset and (3) the properties of the vortexes.
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:&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.

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:&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.

:&aname(long0524){5/24}; Naonori Sugiyama (IPMU) Kinematic Sunyaev-Zel'dovich effect|
Over the past few years, cosmologists have been able to make the first detections of the kinematic Snuyaev-Zel'dovich (kSZ) effect by combining galaxy data with measurements from CMB experiments.¡¡ The kSZ effect is well-suited for studying properties of the optical depth of halos hosting galaxies or galaxy clusters. As the measured optical depth via the kSZ effect is insensitive to gas temperature and redshift, the kSZ effect can be used to detect ionized gas that is difficult to observe through its emission, so-called "missing baryons".  This work presents the first measurement of the kSZ effect in Fourier space.  While the current analysis results in the kSZ signals with only evidence for a detection, the combination of future CMB and spectroscopic galaxy surveys should enable precision measurements. This talk emphasizes the potential scientific return from these future measurements.
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:&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.

:&aname(long0531){5/31}; Shogo Ishikawa (NAOJ CfCA) The Galaxy-Halo Connection in High-redshift Universe |
We present the results of clustering analyses of Lyman break galaxies
(LBGs) at z~3, 4, and 5 using the final data release of the
Canada&#8211;France&#8211;Hawaii Telescope Legacy Survey (CFHTLS). Deep- and
wide-field images of the CFHTLS Deep Survey enable us to obtain
sufficiently accurate two-point angular correlation functions to apply
a halo occupation distribution analysis. The mean halo masses increase
with the stellar-mass limit of LBGs. Satellite fractions of dropout
galaxies, even at less massive halos, are found to drop sharply, from
z=2 down to less than 0.04, at z=3-5, suggesting that satellite
galaxies form inefficiently even for less massive satellites. We
compute stellar-to-halo mass ratios (SHMRs) assuming a main sequence
of galaxies, which is found to provide SHMRs consistent with those
derived from a spectral energy distribution fitting method. The
observed SHMRs are in good agreement with model predictions based on
the abundance-matching method, within 1sigma confidence intervals. We
derive observationally, for the first time, the pivot halo mass, which
is the halo mass at a peak in the star-formation efficiency, at 3<z<5,
and it shows a small increasing trend with cosmic time at z>3. In
addition, the pivot halo mass and its normalization are found to be
almost unchanged during 0<z<5. Our study provides observational
evidence that galaxy formation is ubiquitously most efficient near a
halo mass of 10^12Msun over cosmic time.

:&aname(long0607){6/7}; Tomoya Kinugawa (U. Tokyo) compact binary remnants from first stars for the gravitational wave source|
Using our population synthesis code, we found that the typical chirp mass of binary black holes (BH-BHs) whose origin is the first star (Pop III) is ~30 Msun. This result predicted the gravitational wave events like GW150914 and LIGO paper said "recently predicted BBH total masses agree astonishingly well with GW150914 and can have sufficiently long merger times to occur in the nearby universe (Kinugawa et al. 2014)" (Abbot et al. ApJL 818,22 (2016)). Thus, the compact binary remnants of the first stars are interesting targets of LIGO,VIRGO and KAGRA.Nakano, Tanaka & Nakamura 2015 show that if S/N of QNM is larger than 35, we can confirm or refute the General Relativity more than 5 sigma level. In our standard model, the detection rate of Pop III BH-BHs whose S/N is larger than 35 is 3.2 events/yr (SFR_p/(10^{-2.5}Msun/yr/Mpc^3))*([f_b/(1+f_b)]/0.33)* Err_sys. Thus, there is a good chance to check whether GR is correct or not in the strong gravity region. Furthermore, the Pop III binaries become not only BH-BH but also NS-BH. We found Pop III NS-BH merger rate is ~ 1 events/Gpc^3 and the chirp mass of Pop III NS-BH is more massive than that of Pop I and II. Therefore, we might get information of Pop III stars from massive BH-BHs and NS-BHs.
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:&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.

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:&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 ¡Èambipolar diffusion¡É.
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(long0612){6/12}; Yama&#231; Pehlivan  (Mimar Sinan University)	 Stars as extreme laboratories for neutrino physics|
Neutrinos are the second most abundant particle species in the universe after
the photons. Due to their small cross sections, their last point of scattering
(and hence their memory) lies deep within dense astrophysical objects. As a new
observational window to the Universe, neutrinos hold a great potential. But, an
equally exciting possibility is to use these observations as a probe to their
minuscule properties under the Universe's most extreme conditions.In this talk, I will focus on the neutrinos emitted by core collapse supernova
where, in the deep regions, neutrino-neutrino interactions turn their flavor
oscillations into a nonlinear many-body phenomenon. Various tiny neutrino
properties can be amplified by these nonlinear effects with detectable
consequences. These can show themselves directly in a future galactic supernova
signal detected by Super-Kamiokande, or indirectly (through their effect on
nucleosynthesis) in elemental abundance surveys by Subaru and TMT.
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:&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¡Ý10. 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.

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:&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(long0614){6/14}; Cemsinan Deliduman (Mimar Sinan University) Astrophysics with Weyl Gravity|
This talk will introduce an attempt to describe the diverse astrophysical phenomena via Weyl gravity. In the first part I will review my work on the resolution of the flat galactic rotation curve problem via geometry instead of assuming the existence of dark matter. Motivation for this work came from the observation that the scale independence of the rotational velocity in the outer region of galaxies could point out to a possible existence of local scale symmetry and therefore the gravitational phenomena inside such regions should be described by the unique local scale symmetric theory, namely Weyl¡Çs theory of gravity. Solution to field equations of Weyl gravity will determine the special geometry of the outer region of galaxies. In the second part of the talk it will be conjectured that this special geometry could be valid up to the scale of galaxy clusters. Then one challenge of this approach will be to explain gravitational lens characteristics of galaxy clusters by Weyl geometry without assuming existence of dark matter. Research in this direction will be summarized.
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:&aname(long0724){07/24}; Shunsuke  Ideguchi (NAOJ) Basics of Faraday Tomography Technique and Its Applications to Cosmic Magnetism Study|
The synchrotron radiations from various astronomical objects and their Faraday rotation allow us to obtain the information about magnetic fields of the objects and of the media between them and us. The low-frequency, wide-band polarization observations made with the next-generation telescopes represented by Square Kilometer Array (SKA) and its precursors/pathfinders make it possible to use Faraday rotation to create a tomographic reconstruction of magnetized structures along the line of sight, a technique known as Faraday tomography. In this talk, I will introduce the basics of the technique and overview the cosmic magnetism studies using the technique so far.

:&aname(long0621){6/21}; Hiroyuki Kurokawa (ELSI, Tokyo Tech) Hydrodynamics of first atmospheres of planets embedded in protoplanetary disk|
Exoplanet observations revealed that a significant fraction of Sun-like stars harbor super-Earths, here defined as those objects having masses between a few to ~20 Earth masses. Though their masses overlap with the range of core masses believed to trigger runaway accretion of disk gas, these super-Earths retain only small amounts of gas: ~1%-10% by mass. How did super-Earths avoid becoming gas giants? One possible solution is late-stage core formation; super-Earths were formed by the final assembly of proto-cores during disk dispersal (Lee et al. 2014). Another solution is rapid recycling of envelope gas. Ormel et al. (2015) conducted hydrodynamical simulations of isothermal flow past a low-mass planet embedded in disk gas. They found that the atmosphere (inside the Bondi sphere) is an open system where disk gas enters from high latitude (inflow) and leaves through midplane region (outflow). They argued that the recycling is faster than the cooling (namely, the contraction) of the envelope gas, and so that further accretion of disk gas is prevented. To evaluate the influence of the cooling process on the recycling process, we performed non-isothermal hydrodynamical simulations of the flow around an embedded planet, where radiative cooling was approximated by the beta cooling model. We found that the recycling is limited in the non-isothermal cases because of the difference in entropy between the inflow (high entropy) and the atmosphere (low entropy). The high entropy flow cannot penetrate the low-entropy atmosphere, and therefore the recycling is limited to the upper region of the Bondi sphere. Our results suggest that the recycling process may not be able to explain the ubiquity of super-Earths. Nevertheless, the midplane outflow induced by the recycling may prevent or reduce the accretion of pebbles onto proto-cores. This would delay the growth of these cores and help us to explain the ubiquity of super-Earths in the context of the late-stage core-formation scenario.
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:&aname(long1002){10/02}; Richard Teague  (University of Michigan)¡¡Observing the Kinematics of Planet-Disk Interactions with ALMA|
ALMA has undoubtedly revolutionised our understanding of planet formation. It has demonstrated that substructures in the both the gas and dust distributions are ubiquitous, indicative of on-going, unseen planet formation. However, our ability to recreate these substructures with a myriad of mechanisms and perturbers, ranging from multiple-planet systems to planet free ones, leaves us unable to distinguish between scenarios. I will present recent work in which we use the motions of the gas to provide a unique view of planet-disk interactions. I will show how we can measure velocities to a sub-percent level precision, allowing us to infer accurate pressure and density profiles for these disks. With these constraints to hand we are able beginning to be able to differentiate between these scenarios and understand the connections between the dust substructures we see, both at the midplane and in the disk atmosphere, and unseen planets.

:&aname(long0628){6/28}; Masanobu Kunitomo (Nagoya University) Revisiting the pre-main sequence evolution of low-mass stars: Importance of accretion and deuterium|
Recent theoretical work has shown that the pre-main sequence (PMS) evolution of stars is much more complex than previously envisioned: Instead of the traditional one-dimensional solution of the contraction of a spherically symmetric gaseous envelope, protostars grow from the first formation of a small seed and subsequent accretion of material. This material is shocked, accretion may be episodic and not necessarily symmetrical, thereby affecting the energy deposited inside the star and its interior structure. Given this new framework, we confirm the findings of previous works (e.g., Baraffe et al. 2009, 2012, Hosokawa et al. 2011) that the evolution changes significantly with the amount of energy that is lost during accretion. We find that deuterium burning also regulates the PMS evolution. In the low-entropy accretion, the evolutionary tracks in the Hertzsprung-Russell diagram are significantly different from the classical ones and sensitive to the deuterium content. Our results agree with previous work that the variation of heat injection can be the solution of luminosity spread problem of PMS stars and show the importance of the deuterium content. We also discuss the internal structure evolution of young stars and the impact on the stellar surface composition.
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:&aname(long1011){10/11}; Hector O. Silva (Montana State University) Illuminating the strong-field regime of gravity|
Observation of the x-ray pulse profile emitted by hotspots on the surface of neutron stars offers a unique tool to measure the properties of these objects, including their masses and radii. The x-ray emission takes place at the star¡Çs surface, where the gravitational field is strong, making these observations an incise probe into the spacetime curvature generated by these stars. In this presentation, I will discuss how general relativity plays a key role in the accurate modelling of pulse profiles and the prospects for testing Einstein's theory - and some of its contenders - using these observations.

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:&aname(long1011){10/11}; George Pappas (Sapienza University of Rome) Testing the Kerr hypothesis with QNMs and ringdowns|
The Kerr spacetime that describes all rotating black holes is one of the most important solutions of general relativity. The theoretical and astrophysical significance of this solution cannot be underestimated. For this reason it is of analogous importance to thoroughly test whether the objects that we have identified as the astrophysical incarnations of Kerr black holes are actually that or some alternative exotic compact object that simply mimics aspects of their behaviour. With the advent of gravitational wave astronomy, this is possible by observing the inspiral, merger, and ringdown of binary systems. This talk will discuss some ways that we can use to test for these impostors.

:&aname(long0705){7/5}; Yuta Asahina (NAOJ CfCA) MHD Simulations of the Feedback via an AGN outflow to the inhomogenious interstellr medium|
Co-evolution between central supermassive black holes and host galaxies is a hotly debated issue in astrophysics. Outflows are thought to have an impact of the interstellar medium (ISM), and probably be responsible for the establishment of a widely known correlation between black hole mass (M) and the stellar velocity dispersion in galactic bulge (¦Ò), so-called M-¦Ò relation. Feedback by the quasar wind has been investigated by Silk & Rees (1998),  Fabian (1999), and King (2003). However the quasar winds are assumed to be spherical symmetric outflows.  Wagner et al. (2012) studied the feedback via AGN jets. They revealed that the feedback via the AGN jet can be origin of M-¦Ò relation. Magnetic fields are not included in their simulations, although magnetic fields of 0.01-1 mG have been reported to exist in the galactic center. In order to study the effect of the magnetic field to the feedback via the AGN jet, we carry out 3D MHD simulations. Our simulations reveal that the magnetic tension force promotes the acceleration of the ISM and enhances the feedback efficiency.
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:&aname(long1016){10/16}; Kazunari Iwasaki  (Osaka University)¡¡The formation of molecular clouds by compression of atomic gases|
The formation of molecular clouds is one of the fundamental building blocks in star formation. In order to determine the initial condition of the star formation,it is crucial to reveal the formation and evolution processes of molecular clouds. We investigate the formation of molecular clouds from atomic gas by using three-dimensional magnetohydrodynamical simulations including non-equilibrium chemical reactions and heating/cooling processes. We consider super-Alfvenic head-on colliding flows of the atomic gas possessing the two-phase structure. We examine how the molecular cloud formation changes depending on the angle between the upstream flow and mean magnetic field. If the atomic gas is compressed almost along the mean magnetic field, the accretion of the highly inhomogeneous upstream atomic gas drives a super-Alfvenic velocity dispersion which decreases the mean density of the post-shock layer. Even a small obliqueness of the magnetic field weakens the post-shock turbulence. As a result, the post-shock layer becomes denser than that formed by a colliding flow almost aligned to the magnetic field. If the magnetic field is further inclined to the upstream flow, the shock-amplified magnetic pressure suppresses gas compression, leading to an extended post-shock layer. Our results, therefore, show that there is a critical angle which maximizes the mean density of the post-shock layers. Developing an analytic model and performing a parameter survey, we derive an analytic formula of the critical angle as a function of the mean density, collision speed, and field strength of the upstream atomic gas. We also found that the dependence of the post-shock layers on the angle causes a diversity of the physical properties of dense clumps.

:&aname(long1030){10/30}; Yen-Chen Pan (NAOJ) Understanding Type Ia Supernova with UV Spectroscopy|
Ultraviolet (UV) observations of Type Ia supernovae (SNe Ia) are useful tools for understanding progenitor systems and explosion physics. In particular, UV spectra of SNe Ia, which probe the outermost layers, are strongly affected by the progenitor metallicity. Theory suggests that SN Ia progenitor metallicity is correlated with its peak luminosity, but not its light-curve shape. This effect should lead to an increased Hubble scatter, reducing the precision with which we measure distances. If the mean progenitor metallicity changes with redshift, cosmological measurements could be biased. Models also indicate that changing progenitor metallicity will have little effect on the appearance of optical SN data, but significantly alter UV spectra. To address this problem, we reduced and published the largest UV spectroscopic sample of SNe Ia to date. With this sample, we confirm theoretical predictions that SN Ia UV spectra are strong metallicity indicators. Our findings show that UV spectra are promising tools to further our understanding of SN Ia while directly improving the utility of SN Ia for cosmology.

:&aname(long0712){7/12}; Shoko Oshigami (NAOJ CfCA) Mare volcanism: Reinterpretation based on Kaguya Lunar Radar Sounder data|
The Lunar Radar Sounder (LRS) onboard Kaguya (SELENE) detected widespread horizontal reflectors under some nearside maria. Previous studies estimated that the depths of the subsurface reflectors were up to several hundreds of meters and suggested that the reflectors were interfaces between mare basalt units. The comparison between the reflectors detected in the LRS data and surface age maps indicating the formation age of each basalt unit allows us to discuss the lower limit volume of each basalt unit and its space and time variation. We estimated volumes of basalt units in the ages of 2.7 to 3.8 Ga in the
nearside maria. The lower limit volumes of the geologic units estimated in this study were on the order of 10^3 to 10^4 km^3. This volume range is consistent with the total amount of erupted lava flows derived from numerical simulations of thermal erosion models of lunar sinuous rille formation and is also comparable to the average flow volumes of continental flood basalt units formed after the Paleozoic and calculated flow volumes of Archean komatiite flows on the Earth. The lower limits of average eruption rates estimated from the unit volumes were on the order of 10 ^5 to 10^ 3 km^3/yr. The estimated volumes of the geologic mare units and average eruption rate showed clear positive correlations with their ages within the same mare basin, while they vary among different maria compared within the same age range. This talk is given in Japanese.

:&aname(long1120){11/20}; Yuri Fujii (Nagoya University) Formation of Circumplanetary Disks and Regular Moons|
During the formation phase of gas giants, circumplanetary gaseous disk form around the planets. Circumplanetary disks are important not only for mass supply to gas giants but also for formation of regular satellites. Because of the comparatively small size-scale of the sub-disk, quick magnetic diffusion prevents the magnetorotational instability (MRI) from being well-developed at ionization levels that would allow MRI in the parent protoplanetary disk. In the absence of significant angular momentum transport, continuous mass supply from the parental protoplanetary disk leads to the formation of a massive circumplanetary disk. We have developed an evolutionary model for this scenario and have estimated the orbital evolution of satellites within the disk. In a certain temperature range, we find that inward migration of a satellite can be stopped by a disk structure due to the opacity transitions. We also find that the second and third migrating satellites can be captured in mean motion resonances. In this way, a compact system in Laplace resonance, which are similar to inner three bodies of Galilean satellites, can be formed in our disk models.

:&aname(long0726){7/26}; Jean Coupon (University of Geneva): Probing the galaxy-mass connection in TeraByte-scale imaging surveys|
The past decade has seen the emergence of new techniques and exciting discoveries powered by wide-field imaging surveys from the UV to the near-IR domain. Owing to gravitational lensing, galaxy clustering and abundance matching (to name but a few), coupled with advanced statistical interpretation, the informative power of astronomical imaging surveys has significantly increased. In particular, the connection between galaxies and dark matter, a keystone in cosmology and the study of galaxy evolution, has widely gained from this "scale revolution" and the future is bright, as the next experiments such as HSC, LSST, Euclid or WFIRST are dedicated "survey" machines that will further increase imaging data by orders of magnitude (without mentioning the tremendous gain in image resolution, time domain and deep near-IR imaging). I will focus my talk on reviewing the main techniques to connect galaxies and dark matter in the context of wide-field surveys and I will show some concrete examples of applied data analysis in the CFHTLenS and COSMOS projects, showing that these techniques are now well proven, although the challenges in reducing some critical systematic uncertainties are ahead of us.
:&aname(long1211){12/11}; Daisuke Nakauchi (Tohoku University) Ionization degree and magnetic diffusivities in the low-metallicity star-formation|
Magnetic fields change the mass and angular momentum of a star-forming
cloud and affect the formation of a protostar disk and binary system by
driving an outflow and braking the cloud core rotation. The coupling
between the gas and magnetic field is, however, generally weak, owing to
the low fractional ionization of the cloud. Therefore, accurate
calculation of the ionization degree is needed to consider the magnetic
fields. Here, we calculate the chemical and thermal evolution of a
low-metallicity cloud by using a chemical network in which reverse
reactions are considered for all the forward reactions. Considering
reverse reactions only for 1/10 of the forward reactions, previous studies
can not calculate the ionization degree accurately until the protostar
formation. We find that at ~ 10^{14}-10^{19} cm^{-3}, the ionization
degree becomes 10-100 times higher than that obtained in the previous
studies. This is due to the ionization of alkali metals, like lithium,
sodium, and potassium, which are missed in the previous studies. We also
calculate the magnetic diffusivities and discuss the implication of our
results.

:&aname(long0927){9/27};  Takayoshi Kusune (NAOJ): Magnetic field of the bright-rimmed cloud SFO 74|
Magnetic fields are believed to play an important role in the formation and evolution of molecular cloud. In this talk, I will present the results of near-infrared polarimetric observations toward a bright-rimmed cloud (SFO 74). Bright-rimmed clouds, which are small molecular clouds located at the periphery of the HII regions, are considered to be potential sites for induced star formation by UV radiation from nearby OB stars. The obtained polarization vector maps clearly show that the plane-of-sky (POS) magnetic field structure inside the cloud is quite different from its ambient POS magnetic field direction. By applying the Chandrasekhar-Fermi method, I estimate the POS magnetic field strength toward the two regions inside the cloud. Our results indicate that the magnetic field (configuration and strength) of SFO 74 is affected by the UV-radiation-induced shock. I will discuss the relationship between the POS magnetic field and the cloud structure.
:&aname(long0108){1/8}; Hiroshi Kobayashi (Nagoya University) From Dust to Planet via Collisional Growth|
Planets are believed to be formed in a protoplanetary disk. The mass ratio of a planet to a dust grain is on the order of 10^42. In collisional history of solid bodies across such a large dynamic range of mass, we need to care various physics controlling relative velocity between bodies and collisional cross sections, which determines the collisional growth of bodies. To tackle this problem, we develop impact simulation, N-body simulation, and statistical simulation. We construct a collisional model based on the results of impact simulation. We investigate the growth of bodies via N-body or statistical simulations based on the collisional model. The statistical simulation is good at the treatment of the large dynamic range of mass, while chaotic orbital evolution in the late stage of terrestrial planet formation should be treated by N-body simulation. Accordingly, we show the growth of dust aggregates to be planetesimals (Okuzumi et al. 2012), the formation of gas giant planets (Kobayashi et al. 2011, 2012), minor bodies such as main-belt asteroids (Kobayashi et al. 2016), and the formation terrestrial planets (Kobayashi & Dauphas 2013). I will introduce the collisional history from dust to planet based on these results.

:&aname(long0122){1/22}; Jun Kumamoto (University of Tokyo) Gravitational-Wave Emission from Binary Black Holes Formed in Open Clusters|
In February 2016, the first gravitational wave was directed by LIGO. This detection suggests that there are many black-hole binaries of ~30 solar mass. In order to investigate the formation rate of binary black holes (BBHs) in stellar clusters with a mass comparable to open clusters, we performed a series of direct N-body simulations of open clusters with a mass of 2500 and 10000 solar mass. Since such low-mass clusters would have been more populous than globular clusters when they were born, low-mass clusters are also candidates as the origin of BBHs which are the source of the gravitational waves. In our model, most of BBHs merged within 10 Gyr formed via dynamically formed main-sequence binary stars and stable and unstable mass transfer between them since open clusters collapse within the main-sequence life-time of massive stars. Our simulation shows that the contribution of BBHs originated from open clusters is not negligible.

:&aname(long1003){10/03};  Matthew Kenworthy (Leiden Observatory) : Looking for exorings towards Beta Pictoris, J1407 and PDS 110|
Circumplanetary disks are part of the planet and moon formation
process, passing from an optically thick regime of gas and dust
through to a planet with retinue of moons and Roche lobe rings formed
from the accreted material. There should therefore be a transitional
phase where moons are beginning to form and these will clear out lanes
in the circumplanetary disk, producing Hill sphere filling 'rings'
hundreds of times larger than Saturn's rings.
We have seen evidence of these objects transiting their young star -
with J1407, and more recently, with the young star PDS 110. This star
shows periodic eclipses lasting over two weeks of up to 30% in depth,
and the next eclipse is predicted to occur in September this year. The
star is 10th magnitude in the belt of Orion, and can be followed in
the early morning skies from most places on Earth.
We are also following the Hill sphere transit of Beta Pictoris b, a
gas giant planet around a nearby bright star, and I will also present
the latest light curves from this experiment.
:&aname(long0207){2/7}; Hiroshi Kimura (Chiba Institute of Technology) The Evolution of Organic Matter in the Universe|
&#8212; Genesis 3:19: For dust you are and to dust you will return
This is the essence of cosmic dust research at PERC (Planetary Exploration Research Center) in Chiba Institute of Technology. The questions we aim to answer are: Where do we come from? What are we? Where are we going?
Primitive cosmic dust consists of C, H, O, and N, owing to the cosmic abundance constraints. The evolution of matter in the Universe is inevitably associated with stellar evolution, and its consequence is enrichment of C, H, O, and N in primitive dust. No doubt, C, H, O, and N are the major elements to comprise organic matter as well as life on Earth. Therefore, we, dust researchers at PERC, aim to seek evidence for a link of organic matter to the origin of life as well as the ubiquity of life in planetary systems through a comprehensive study on organic matter in primitive dust particles. In this talk, I will present recent advances in our understanding of the evolution of organic matter in interstellar dust and cometary dust based on in-situ dust measurements and theoretical modelings.

:&aname(long1004){10/04};  Yuri Aikawa (University of Tokyo): Deuterium Fractionation in Protoplanetary Disks|
Deuterium enrichments in molecules are found in star-forming regions, as well as in Earth¡Çs ocean. Asrtrochemical models show that the enrichment originates in exothermic exchange reactions at low temperatures, which could proceed not only in molecular clouds, but also in the cold regions of protoplanetary disks. In recent years, several groups observed deuterated molecules in disks using ALMA, in order to investigate the significance and spatial distribution of the fractionation. Brightness distributions of deuterated molecular lines vary with species and objects. In TW Hya, DCN is centrally peaked, while DCO+ is offset from the center, which suggests that they are formed via different deuteration paths. In AS 209, on the other hand, DCO+ and DCN emissions show similar distribution. Motivated by these observations, we calculate the reaction network model of deuterium chemistry in protoplanetary disks. Our model includes various deuterated molecules, exchange reactions, and nuclear spin-state chemistry of H2 and H3+, which affects the efficiency of deuterium enrichment. We found that the exchange reaction responsible for the fractionation varies among regions. While the exchange reactions of HD with H3+ and CH3+ are effective, as expected, the exchange reaction of D atom with HCO+ is also found to be important in warm regions and disk surface. As long as cosmic rays penetrate the disk, ortho/para ratio of H2 is found to be almost thermal, which lowers the efficiency of fractionation via CH2D+ compared with previous models which assume that H2 is all in para state. We also discuss the effects of grain size and turbulent mixing on deuterium chemistry.
:&aname(long0207){2/12}; Kei Tanaka (Osaka University/ NAOJ) Massive Star Formation under Multiple Feedback Processes|
Despite their importance in various fields of astrophysics, the formation of massive stars is not understood well compared to low-mass star formation. Stars with over-100 solar masses have especially been theoretically considered to be hardly formed due to their own radiation feedback even though they do exist. In this talk, I first summarize the concept of "Core Accretion" scenario for massive star formation (e.g., McKee & Tan 2003), which is a scaled-up version of models of low-mass star formation from cores. Then, I present our theoretical works, i.e., the first study of the multiple feedback processes in massive star formation (Tanaka et al. 2017a, 2018). Our model shows that, at solar metallicity, very massive stars with at least 500Msun can be formed by the mass accretion through disks. The MHD disk wind is the most robust feedback rather than the radiative feedback even in massive star formation. We also apply this model to a wide range of metallicities to connect present-day massive star formation and first-star formation in the early universe. At lower metallicity, we find that the star formation efficiency gets lower due to the efficient photo-evaporation. Finally, I introduce our recent observations of massive protostars by SOFIA, VLA, and ALMA (De Buizer et al. 2017, Rosero et al. 2019, Zhang et al. 2019, etc.).  We reveal the properties of massive protostars which are deeply embedded in their natal molecular clouds utilizing our theoretical models (Tanaka et al. 2016, 2017b, etc.).

:&aname(long1010){10/10}; Peter Behroozi (University of Arizona): Maximizing Inference from Galaxy Observations|
I discuss new methods to combine multiple datasets to maximally constrain galaxy evolution and the galaxy¡½dark matter halo connection, and show how these methods have already changed our understanding of galaxy formation physics (including why galaxies stop forming stars).  Basic extensions to the same techniques allow constraining internal galaxy processes, including coevolution between galaxies and supermassive black holes as well as time delays for supernova / GRB progenitors.  Finally, I discuss how these methods will benefit from the enormous amount of upcoming data in widefield (HETDEX, LSST, Euclid, WFIRST) and targeted (JWST, GMT) observations, as well as ways they can benefit observers, including making predictions for future telescopes (especially JWST) and testing which of many possible targeted observations would best constrain galaxy formation physics.
:&aname(long0218){2/18}; Takashi Shibata (NAOJ) Coalescence condition of planetesimals|
Terrestrial planets and ice giants are thought to be born by the accumulation of planetesimals. The process of planetesimal accumulation has thus far been studied by methods such as N-body simulations, and the process of detailed accumulation such as the runaway growth and oligarchic growth of planetesimals is becoming apparent. However, there has been no research on accumulation correctly evaluating the rebound at the time of planetesimal collision, while recent studies used conditions of protoplanet coalescence only provisionally. Merging that does not consider rebounding or destruction is called perfect coalescence. By accounting for merging planetesimals that bounce off in reality, there is a possibility that the accumulation time has previously been underestimated. It also affects the accumulation of the angular momentum accompanying the accumulation of planetesimals. In a perfect coalescence, even a grazing collision is judged to be coalesced, so accumulation of excessive angular momentum can occur. In order to properly evaluate the accumulation time and the rotation angular momentum, it is necessary to clarify the coalescence conditions of the planetesimal and to consider the rebound when studying planetesimal accretion. In this study, we investigated conditions that determine coalescence vs. rebound by numerically colliding undifferentiated rocky planetesimals, undifferentiated icy planetesimals, and differentiated icy planetesimals using Smoothed Particle Hydrodynamics (SPH). We vary the total mass, mass ratio, collision speed, and collision angle of the colliding planetesimals, and define the impact velocity at which the planetesimal bounces as the critical impact velocity. The critical impact velocity was examined for each mass ratio and collision angle, revealing a clear dependence on each parameter. In addition, the critical impact velocity normalized by the escape velocity was independent of the total mass of the planetesimals. From the above results, we can formulate the critical impact velocity as a variable for the planetesimals¡Ç mass ratio and collision angle. This equation can be used as a condition for determining the rebound and coalescence at the time of the collision in the numerical calculation of the accumulation process of the planetesimals. Moreover, this condition has small dependence on the composition and internal structure of the planetesimals, and it can be used as a coalescence condition for various planetesimals.

:&aname(long1018){10/18}; Ryosuke Hirai (Waseda University ): Understanding core-collapse supernovae in binaries with various numerical approaches|
Compact binaries have rapidly attracted attention since the recent detection of gravitational waves from a binary black hole merger event. The two components should have originated from massive stars which experience core-collapse at the end of their lives. However, the evolution of massive stars are extremely uncertain and the presence of a close-by companion complicates it even more. A close binary can undergo mass transfer by overflowing its Roche lobe, or dynamical evolution called common envelope phases when a star plunges into the envelope of the other. Another possible effect is the direct impact of supernova ejecta colliding with its companion when one of the star explodes.
In this talk I will discuss the consequence of the "ejecta-companion interaction", using hydrodynamical simulations and stellar evolution calculations. Our results have coincidentally helped us understand the nature of the progenitor system of a supernova called iPTF13bvn. I will also discuss the overall evolution of this progenitor system. If I have time, I will also introduce some of my latest works on numerical techniques.
:&aname(long0305){3/4}; Scott Suriano (University of Tokyo) The Formation of Rings and Gaps in Magnetized Wind-Launching Disks|
Radial substructures in circumstellar disks are now routinely detected by state-of-the-art observational facilities. There is also growing evidence that large-scale magnetic fields threading disks are responsible for launching disk winds and driving accretion. We investigate how rings and gaps form in magnetized disks through non-ideal MHD simulations. In axisymmetric 2D simulations including either Ohmic resistivity or ambipolar diffusion (AD), prominent features form in the disk surface density with a strong radial variation of the poloidal magnetic flux relative to the mass. Regions with low mass-to-flux ratios accrete quickly and lead to the development of gaps, whereas regions with higher mass-to-flux ratios accrete more slowly, allowing matter to accumulate and form dense rings. Specifically, in the AD-dominated disks, the radial variation of the magnetic flux is set by the reconnection of a highly elongated poloidal magnetic field across a thin midplane current sheet, through which fast laminar accretion occurs. We extend the simulations of AD-dominated disks to 3D and find that rings and gaps still develop naturally from the same basic mechanism that was identified in 2D. The rings and gaps remain stable in 3D for a few thousand orbital periods at the inner edge of the simulated disks, making them attractive sites for trapping large grains that would otherwise be lost to rapid inward radial migration.

:&aname(long1019){10/19}; Sergey Blinnikov (Institute for Theoretical and Experimental Physics ): GRB Central Engines within Superluminous Supernovae and their environment|
Large amounts of mass may be expelled by a star  a few years before a supernova explosion. The collisions of SN-ejecta and the dense CSM  may provide the required power of light to make the supernova much more luminous. This class of models is referred to as "interacting SNe¡É. Many SLSNe-I have photospheric velocity of order 10&#8308; km/s which is hard to explain in interacting scenario with modest energy of explosion. A strong "hypernova" explosion improves the situation and the properties of  SLSNe near maximum light are explained by a GRB-like central engine, embedded in a dense envelope and shells ejected prior the final collapse/explosion of a massive star. In this case velocity up to 1.5x10&#8308; km/s is no problem. The problem remains with the nature of the central engine and evolution scenarios leading to double explosions. In view of new LIGO/VIRGO detections of gravitational waves and accompanying events, a few comments and historical remarks will be given.
:&aname(long0312){3/12}; Shingo Hirano (Kyusyu University) Environmental dependence of the first star formation|First stars play vital roles in the early cosmic evolution by initiating cosmic reionization and chemical enrichment of the intergalactic medium. The characteristic mass of first stars (or initial mass function) is thus essential to understand the observational counterparts and formation and evolution of the first galaxies. We perform a set of cosmological simulations of early structure formation incorporating baryonic streaming motions, which are intrinsically generated in the early universe according to the standard model of structure formation. We find different first star formation depending on the initial streaming velocities: massive star, massive star cluster, and supermassive star. Interestingly, the latter two cases leave (1) a massive black hole binary, which can be a progenitor of strong gravitational wave sources similar to those recently detected by LIGO, and (2) a intermediate mass black hole, which can be a promising seed for the formation of observed high-z quasars, respectively.

:&aname(long1025){10/25}; Sho Fujibayashi (Kyoto University ): The evolution and mass ejection from the remnant of the binary neutron star merger|
We perform general relativistic, long-term, axisymmetric neutrino
radiation hydrodynamics simulations for a remnant massive neutron star
(MNS) surrounded by a torus, which is a canonical remnant formed after
the binary neutron star merger.
In this work, we take into account effects of viscosity which is
likely to arise in the merger remnant due to magnetohydrodynamical
turbulence.
We find that two viscous effects play a key role for the evolution of
the remnant system and resulting mass ejection.
In the first ~10 ms, the structure of the MNS is changed due to the
viscous angular momentum transport. As a result, a sound wave, which
subsequently becomes a shock wave, is formed in the vicinity of the
MNS and the shock wave leads to significant mass ejection.
For the longer-term evolution with ~ 0.1--10 s, viscous effects on the
torus surrounding the MNS play an important role for mass ejection.
The mass ejection rate depends on the viscous parameter for both mass
ejection mechanisms, but even for the conservative alpha viscous
parameter $\alpha_{\rm vis}\sim0.01$, total ejecta mass is $\sim 5\times 10^{-3}\ M_\odot$ and for $\alpha_{\rm vis}\sim0.04$, it could
be $0.02\ M_\odot$.
In this talk, I will explain the viscosity-driven mass ejection
processes and discuss the electromagnetic signal from the ejecta.

:&aname(long1102){11/02}; Wanggi Lim (NAOJ): Dust in Infrared Dark Clouds|
The dust grains play key roles to determine physical properties of
dense molecular structures. Despite of their importance, our knowledge
toward dust properties is mostly dependent on experimental tests and
theoretical models due to observational limits on high extinction
regions. Here we introduce Mid, Far and Spectroscopic infrared
extinction (MIREX, FIREX & SIREX) mapping methods that show the first
observational evidence of grain growth in extremely high density
regions, i.e. Infrared Dark Clouds. We utilize archival image data of
Spitzer-IRAC band 1-4 (3.5 - 8¦Ìm), WISE band 3 (12¦Ìm), Spitzer-MIPS
(24¦Ìm) and Herschel-PACS (70¦Ìm) in order to make MIREX & FIREX maps of
an IRDC, G028.07+00.07. Spectroscopic data of Spitzer-IRS Long-Low
slit (15 to 38¦Ìm) is analyzed to produce a SIREX map of same IRDC. The
pixel by pixel relative extinction laws of the IRDC show the tentative
evidence of dust grain growth via coagulation and ice mantle formation
in the region of Av~10-100mag. We then compare mass surface density
probability distribution functions (¦²-PDFs) of the IRDC and
surrounding giant molecular cloud (GMC) that are derived from MIREX
map (8¦Ìm) and sub-mm (Herschel 160-500¦Ìm) dust emission based ¦² map
(via grey-body fit). The PDFs can be well fit by a single log-normal
distribution, with only a small mass fraction (0.03-0.08) in a high ¦²
power-law tail, even though gas kinematics indicate the IRDC and GMC
are self-gravitating with virial parameter ¦Á~1. We also show the
effect of spectral index ¦Â variation against the mass fraction of
high-¦² power-law tails.

:&aname(long1115){11/15}; Sanemichi Takahashi (Kogakuin University): Early evolution of protoplanetary disks: a ring-gap structure formation |Planets are formed in protoplanetary disks, which are formed around
protostars simultaneously with them. Investigation of the early stages
of evolution of the protoplanetary disks is important to understand
how the star formation and the planet formation processes are
connected.
Recent observations with ALMA reveal the detailed structures of the
protoplanetary disk at the early evolutionary stage. Sheehan and
Eisner 2017 found that the gap structure is formed in the
protoplanetary disk the protostar WL 17 within about 10 au. Such a
structure is thought to be the feature of the old disks (>10^6 yr)
called by transition disks. However, the age of WL 17 is estimated to
be a few times 10^5 yr. The mechanisms of the gap formation in such
young disks have not been investigated well.
Sheehan and Eisner 2017 mentioned that the gap structure is formed by
the planet. However, the planets forming the gap have not been
observed, and it seems difficult to form the planet in the young
protoplanetary disks. Thus, it is important to investigate another
mechanism for the gap formation in the young disk. In this talk, we
discuss the gap formation by the disk wind in the young disks like WL
17 using 1D disk model for the formation and evolution of
protoplanetary disks.

:&aname(long1122){11/22}; Wolfgang Loeffler (Heidelberg ARI): Gaia Sky: A 3D visualisation of the Gaia Catalogues|
The aim of the ESA Gaia mission is to chart the three-dimensional
positions and motions of about 1 billion stars in our Milky Way. Gaia
Sky is an open-source, multi-platform, real-time, 3D, astronomy
software being developed in the Gaia group of the Astronomisches
Rechen-Institut (ZAH, Universit&#228;t Heidelberg) to visualise these
positions and motions. We will give an overview of the software
features and catalogues which have already been released for the Gaia
Data Release 1 and which are under current development for the Gaia
Data Relase 2. After briefly touching some technical aspects of the
Gaia Sky implementation, we will present some educational and
scientific use cases.

:&aname(long1206){12/06}; Kazuyuki Sugimura (Tohoku University): Accretion onto seed BHs: the impacts of anisotropic radiation and gas angular momentum|
Seed black hole (BH) growth by gas accretion is supposed to play a crucial role in the formation of supermassive BHs. In this talk, I will present the results of our simulations of accretion onto seed BHs under radiation feedback and explain the impact of anisotropic radiation and gas angular momentum on the accretion flow. Then, I will shortly discuss the growth of Pop III remnant BHs based on our findings.

:&aname(long1220){12/20}; Yutaka Hirai (NAOJ): The role of enrichment of heavy elements in the chemodynamical evolution of dwarf galaxies|
Recent astronomical observations have shown that there are large star-to-star scatters in the abundances of r-process elements and increasing trend of Zn in extremely metal-poor stars. However, it is not yet clear how the early chemo-dynamical evolution of the building blocks of the Milky Way halo affect the abundances of heavy elements. In this talk, we show that high-resolution N-body/smoothed particle hydrodynamics simulations of dwarf galaxies. We find that galaxies with star formation rates less than 0.001 Msun per year reproduce the observed abundances of r-process elements. On the other hand, r-process elements appear at a higher metallicity in galaxies with star formation rates greater than 0.01 Msun per year. We also find that the ejecta from electron-capture supernovae contribute to stars with [Zn/Fe] > 0.5. The scatters of heavy elements mainly come from the inhomogeneity of the metals in the interstellar medium. We find that timescale of metal mixing is less than 40 Myr. This timescale is lower than that of typical dynamical times of dwarf galaxies. Our results demonstrate that the future observations of r-process elements in extremely metal-poor stars will be able to constrain the early chemo-dynamical evolution of the Local Group galaxies.

:&aname(long0117){1/17}; Kohei Hayashi (NAOJ): The universal dark halo scaling relation for the dwarf spheroidal galaxies in the Local Group|
Dwarf spheroidal galaxies (dSphs) are are excellent laboratories to shed light on fundamental
properties of dark matter because these galaxies are the most dark matter dominated systems.
In this talk, we propose the universal  dark halo scaling relation for the dSphs in the Milky Way
and M31.
We calculate the dark halo surface density within a radius, r_max, giving the maximum circular
velocity, V_max, with respect to observed dSphs and simulated subhalos associated with
MW-sized dark halos, and find that the values of surface densities from pure dark matter simulations
are in good agreement with those from observations even without employing any fitting procedures.
This implies that this surface density would not be largely affected by any baryonic feedbacks and thus universal.
Moreover, all subhalos on the small scales of dwarf satellites are expected to obey the universal relation, irrespective
of differences in their orbital evolutions, host halo properties, and observed redshifts.
In order to understand the origin of this universal dark halo relation. we also investigate orbital and dynamical evolutions
of subhalos and find that most of subhalos evolve generally along the specific r_max - V_max sequence even though these
subhalos have undergone different histories of mass assembly and tidal stripping.
This sequence, therefore, should be the key feature to understand the nature of the universal scaling relation.

:&aname(long0124){1/24}; Hiroshi Kobayashi (NAOJ): Three-Dimensional Radiation-Hydrodynamic Simulation of Clumpy Outflow and Its Application to Supercritical Accretors around Black Holes|
We study clumpy outflows from supercritical accretion flow around a stellar mass black hole by means of global three-dimensional (3-D) radiation-hydrodynamic (RHD) simulations.
In this work, we find that the radiatively driven outflow with the outflow rate of ~10 LEdd/c2 fragments into many clumps above the photosphere located at a few hundreds of Schwarzschild radius (rS) from the central black hole. Such clumps have a shape of a torn sheet, and are rotating around the central black hole with a sub-Keplerian velocity. The typical clump size is 30 rS or less in the radial direction and is more elongated in the angular directions, ~ hundreds of rS at most. When such clumps pass across the line of the sight of a distant observer, stochastic luminosity variations will be produced. The variation timescales are several seconds for a stellar-mass black hole with mass of ten to several tens of the solar mass and are in rough agreement with the observational results of some ultraluminous X-ray sources (ULXs). Our results thus provide a strong support of a hypothesis that the ULXs are powered by the supercritical accretion onto the stellar mass black hole.

:&aname(long0131){1/31}; Misako Tatsuuma (UTokyo): Gravitational Instability of a Dust Layer Composed of Porous Silicate Dust Aggregates in a Protoplanetary Disk| Planetesimal formation is one of the most important unsolved problems in planet formation theory. In particular, rocky planetesimal formation is difficult because silicate dust grains are easily disrupted when they collide. Recently, it has been proposed that they can grow as porous aggregates when their monomer radius is smaller than ~ 10 nm, which can also avoid the radial drift toward the central star. However, the stability of a layer composed of such porous silicate dust aggregates has not been investigated. Therefore, we investigate the gravitational instability of this dust layer. To evaluate the disk stability, we calculate Toomre's stability parameter Q, for which we need to evaluate the equilibrium random velocity of dust aggregates. We calculate the equilibrium random velocity considering gravitational scattering and collisions between dust aggregates, drag by mean flow of gas, stirring by gas turbulence, and gravitational scattering by gas density fluctuation due to turbulence. We derive the condition of the gravitational instability using the disk mass, dust-to-gas ratio, turbulent strength, orbital radius, and dust monomer radius. We find that, for the minimum mass solar nebula model at 1 au, the dust layer becomes gravitationally unstable when the turbulent strength alpha<10^{-5}. If the dust-to-gas ratio is increased twice, the gravitational instability occurs for alpha<10^{-4}. We also find that the dust layer is more unstable in disks with larger mass, higher dust-to-gas ratio, and weaker turbulent strength, at larger orbital radius, and with a larger monomer radius.

:&aname(long0131){1/31}; Kanji Mori (UTokyo): Quantum Mechanical Constraint on Carbon Fusion Reaction and Its Impact on Type Ia Supernovae|Type Ia supernovae (SNe Ia) are thought to be thermonuclear explosion of white dwarfs (WDs). Their progenitors are not well understood, but one of popular scenarios is the double degenerate (DD) scenario, which attributes SNe Ia to WD-WD binary mergers. The fate of the WD mergers depends on the rate of 12C+12C reaction. We assume a low energy resonance and impose an upperlimit to the resonance strength using the Wigner limit. The resultant resonant rate is applied to the DD scenario. We show that the strongest possible resonance will enhance the reaction rate by ~10^3 times compared with the standard rate, although some of resonances introduced in previous works are too strong. The resonant rate decreases the ignition temperature of carbon burning, therefore accretion induced collapse occurs more easily and the contribution of the DD scenario to the SNe Ia rate becomes smaller.

:&aname(long0328){3/28}; Tomoyuki Hanawa (Chiba University): Conservation of Total Energy Including Gravity in Hydrodynamical Simulations|Total energy of an astronomical system is of our great interest, since the evolution of the system depends on it.  Hence we solve the hydrodynamical equations taking account of the conservation in  numerical simulations of astrophysical objects. However, gravitational energy is often taken into account as a source term and the total energy including gravity is not guaranteed.   This is partly because it takes additional computational cost to solve hydrodynamical equations in the fully conservative form.  This paper shows that the total energy and momentum of a system are fully conserved down to the round off error if the source terms due to gravity are properly taken into account. The method is applicable both when the gravitational force is given by the Poisson equation or explicitly as a function.

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