- 追加された行はこの色です。
- 削除された行はこの色です。
#norelated
* 惑星セミナー2018 [#zbb5ecca]
* 惑星セミナー2020 [#zbb5ecca]
惑星セミナーは原則として毎週木曜日の14:00から理論部セミナー室で開催しています。~
astro-phセミナーは毎週金曜日の12:30から理論部セミナー室で開催しています。
惑星セミナーは原則として毎週木曜日の14:00から開催しています。（連絡係：星野 遥, 荒川 創太, 古家 健次, 荻原 正博）~
astro-phセミナーは毎週金曜日の12:00から開催しています。（連絡係：Carol Kwok）
// セミナー発表順番
//
** Schedule & History [#vfafd1d8]
[[2019年度>Planet2019]]
[[2018年度>Planet2018]]
[[2017年度>Planet2017]]
[[2016年度>Planet2016]]
[[2015年度>Planet2015]]
[[2014年度>Planet2014]]
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|日程|発表|タイトル|Remarks|h
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|[[前期 第1回 5/17 15:00->#planet0517]]|荻原 正博| Formation of the terrestrial planets in the solar system around 1 au via radial concentration of planetesimals|15:00|
|[[前期 第2回 5/24 15:00->#planet0524]]|波々伯部 広隆 | Determination of outer edge of circumplanetary disk in local 3d hydrodynamic simulations |15:00|
|[[前期 第3回 5/30 14:00->#planet0530]]|Dimitri Veras | The growing field of post-main-sequence exoplanetary science, with strong connections to the solar system|Wednesday@Rinko room|
|[[前期 第4回 6/14 14:00->#planet0614]]|細野 七月 | Numerical simulations of the giant impact onto the magma ocean||
|[[前期 第5回 6/28 14:00->#planet0628]]|兵頭 龍樹 | On the origin of Phobos and Deimos||
|[[前期 第6回 7/12 14:00->#planet0712]]|樋口 有理可 | Inner solar system objects with hyperbolic orbits: Interstellar origin or Oort cloud comets?||
|[[前期 第7回 7/19 14:00->#planet0719]]|中野 龍之介 | 中心星質量による原始惑星系円盤進化の変化||
|[[前期 第8回 7/26 14:00->#planet0726]]|中嶋 彩乃 | Orbital evolution of Saturn's mid-sized moons and the tidal heating of Enceladus||
|[[後期 第1回 9/19 14:00->#planet0919]]|波々伯部 広隆 | 論文紹介 (Tanigawa et al. 2012, ApJ, Distribution of Accreting Gas and Angular Momentum onto Circumplanetary Disks)||
|[[後期 第2回 10/3 14:00->#planet1003]]|小久保 英一郎 | Planetesimal Formation by Gravitational Instability of a Porous Dust Disk||
|[[後期 第3回 10/24 14:00->#planet1024]]|瀧 哲朗 | Chondrule Survivability in the Protosolar disk ||
|[[後期 第4回 10/31 13:00->#planet1031]]|Jason Man Yin Woo | The curious case of Mars' formation |13:00|
|[[後期 第5回 11/7 14:00->#planet1107]]|松本侑士 |The formation and dynamical evolution of super-Earths through in-situ giant impacts around M dwarfs ||
|[[後期 第6回 11/14 15:00->#planet1114]]|Adrien Leleu |Stability and detectability of co-orbital exoplanets |15:00- 院生セミナー室|
|[[後期 第7回 11/21 14:00->#planet1121]]|藤井悠里 |On the radiation hydrodynamic simulations of formation of circumplanetary disks ||
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|日程|発表|タイトル|Remarks|担当|h
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|[[前期 第1回 4/9 15:00->#planet0409]]|All members| Self-introduction |15:00|荻原|
|[[前期 第2回 4/16 14:00->#planet0409]]|Haruka Hoshino, Hirotaka Hohokabe| Small ASJ meeting ||荒川|
|[[前期 第3回 4/23 14:00->#planet0409]]|Yuki Yoshida, Eiichiro Kokubo| Small ASJ meeting ||星野|
|[[前期 第4回 5/14 14:00->#planet0409]]|Sota Arakawa| Thermal history and tidal evolution of trans-Neptunian satellite systems ||古家|
|[[前期 第5回 5/28 14:00->#planet0528]]|Takuya Takarada (ABC)| Radial-velocity search and statistical studies for short-period planets in the Pleiades open cluster ||荒川|
|[[前期 第6回 6/4 16:00->#planet0606]]|Beibei Liu (Lund Univ)| Pebble-driven planet formation around very low-mass stars and brown dwarfs |16:00|荻原|
|[[前期 第7回 7/9 14:00->#planet0606]]|Yuka Fujii|Detecting molecular lines of warm/temperate exoplanets with mid-infrared high-resolution spectroscopy||星野|
|[[前期 第8回 7/21 14:00->#planet0606]]|Masato Ishizuka (U. Tokyo)|Studies of exoplanets with high resolution spectroscopy||古家|
|[[後期 第1回 10/16 14:00->#planet1016]]|Makiko Ban|Free-floating planet research and perspective||荻原|
|[[後期 第2回 10/30 14:30->#planet1030]]|Yuki Tanaka (Tohoku Univ.)|Gap formation by a super-Jupiter-mass planet and its effects on the planetary mass accretion rate|14:30|荻原|
//今後の候補
//内部：小久保、押野、荻原、波々伯部、Carol、星野
//原川さん、森島さん、森さん（東工大）、芝池さん（東工大）
//小林さん（名大）、佐々木さん（京大）←理論コロキウム？
//高橋実道さん，長谷川幸彦さん
//小久保さん：Ishigakiさん(ISAS)
//荻原：駒木さん(東大), Sakurabaさん(東工大), Liu(Lund)
//荒川：本間和明さん (D1), 長谷川幸彦さん (東大駒場)
//古家：Gianni Cataldi(東大天文)，野津翔太さん(理研)
//石澤さん(京大)
//森島さん
// ←ダブルスラッシュはコメントアウト
:&aname(planet0530){5/30}; Dimitri Veras, The growing field of post-main-sequence exoplanetary science, with strong connections to the solar system|
The quest for identifying the bulk chemical composition of extrasolar
planets and robust observational evidence that between 25% and 50% of
all Milky Way white dwarfs host currently dynamically-active planetary
systems motivate investigations that link their formation and fate.
Here I provide a review of our current knowledge of these systems,
including an update on the observational and theoretical aspects of
the groundbreaking discovery of at least one disintegrating minor
planet transiting white dwarf WD 1145+017. I show how this field
incorporates several facets of solar system physics and chemistry, and
how its interdisciplinary nature requires input from orbital dynamics,
stellar evolution, astrochemistry, atmospheric science and surface
processes.
//アブスト
:&aname(planet1031){10/31}; Jason Woo, The curious case of Mars' formation|
Dynamical models of planet formation coupled with cosmochemical data from martian meteorites show that Mars'
isotopic composition is distinct from that of Earth. Reconciliation of formation models with meteorite data require that
Mars grew further from the Sun than its present position. Here, we evaluate this compositional difference in more detail
by comparing output from two N-body planet formation models. The first of these planet formation models simulates
what is termed the `Classical' case wherein Jupiter and Saturn are kept in their current orbits. We compare these
results with another model based on the `Grand Tack', in which Jupiter and Saturn migrate through the primordial
asteroid belt. Our estimate of the average fraction of chondrite assembled into Earth and Mars assumes that the initial
solid disk consists of only sources of enstatite chondrite composition in the inner region, and ordinary chondrite in the
outer region. Results of these analyses show that both models tend to yield Earth and Mars analogues whose accretion
zones overlap. The Classical case fares better in forming Mars with its documented composition (29% to 68% enstatite
chondrite plus 32% to 67% ordinary chondrite) though the Mars analogues are generally too massive. We also further
calculate the isotopic composition of 17O, 50Ti, 54Cr, 142Nd, 64Ni, and 92Mo in the martian mantle from the Grand
Tack simulations. We find that it is possible to match the calculated isotopic composition of all the above elements in
Mars' mantle with their measured values, but the resulting uncertainties are too large to place good restriction on the
early dynamical evolution and birth place of Mars.
:&aname(planet1107){11/7}; Yuji Matsumoto The formation and dynamical evolution of super-Earths through in-situ giant impacts around M dwarfs|
Recently, Earth-sized exoplanets are observed around TRAPPIST-1, which is M8 dwarf and has ~0.08 solar mass. Several on-going missions are targeting planets around M dwarfs. It is expected that more and more such planetary system around M dwarfs would be observed. There are some theoretical studies considering planetary formation around M dwarfs. However, the formation and dynamical evolution of close-in super-Earths have not understood systematically yet. We investigate the formation of close-in super-Earths through N-body simulations around M dwarfs. We use the same disk model with changing the stellar mass. At first, the dynamical evolution of isolation mass protoplanets is studied. As Matsumoto & Kokubo (2017) reported, protoplanets collide with their neighboring protoplanets soon after the orbital crossing around 1 solar mass star. Around M dwarfs, dynamical scattering between protoplanets becomes violent and such tournament-like collisional evolution is not seen. We also perform calculations with the systems that initially have protoplanets and planetesimals around M dwarfs. We find that planetesimals are ejected during some close scattering by protoplanets. The growth of protoplanets would be suppressed due to the ejection of planetesimals.
:&aname(planet1114){11/14}; Adrien Leleu/ Stability and detectability of co-orbital exoplanets|
Despite the existence of co-orbital bodies in the solar system (1:1 Mean-motion resonance), and the prediction of the formation of co-orbital planets by planetary system formation models, no co-orbital exoplanets (also called trojans) have been detected thus far. It can be due to the rarity of the configuration, the degeneracy of the co-orbital signature with other configurations, or the observational biases. After a description of various stable co-orbital configurations for a pair of planet, I will discuss the stability of the lagrangian equilibria (L4 and L5) during the migration in the protoplanetary disc for the variables associated to the resonant angle, but also in the direction of the eccentricities and inclination. Finally I will discuss the signature of co-orbitals exoplanets in Transit Timing Variation, transits, and combination of transit and radial velocity measurements.
//:&aname(planet1107){5/21}; 名前 タイトル|
//アブスト
//:&aname(planet0418){4/18}; Carina Heinreichsberger, Terrestrial or Gaseous? A classification of exoplanets according to density, mass and radius|
//When looking at Exoplanet Archives the class of a planet is not given. Therefore I tried to find an easy and fast way to classify exoplanets using only density, mass and radius. In this talk I will discuss the formation theory of Planets to explain the boundaries between the different classes (gas, terrestrial) and show the results of my empirical study.
:&aname(planet0604){6/4}; Beibei Liu, Pebble-driven planet formation around very low-mass stars and brown dwarfs|
We conduct a pebble-driven planet population synthesis study to investigate the formation of planets around very low-mass stars and brown dwarfs, in the (sub)stellar mass range between 0.01 M⊙ and 0.1 M⊙. Based on the extrapolation of numerical simulations of planetesimal formation by the streaming instability, we obtain the characteristic mass of the planetesimals and the initial masses of the protoplanets (largest bodies from the planetesimal size distributions), in either the early self-gravitating phase or the later non-self-gravitating phase of the protoplanetary disk evolution. We find that the initial protoplanets form with masses that increase with host mass, orbital distance and decrease with disk age. Around late M-dwarfs of 0.1 M⊙, these protoplanets can grow up to Earth-mass planets by pebble accretion. However, around brown dwarfs of 0.01 M⊙, planets do not grow larger than Mars mass when the initial protoplanets are born early in self-gravitating disks, and their growth stalls at around 0.01 Earth-mass when they are born late in non-self-gravitating disks. Around these low mass stars and brown dwarfs, we find no channel for gas giant planet formation because the solid cores remain too small. When the initial protoplanets form only at the water-ice line, the final planets typically have ≳15% water mass fraction. Alternatively, when the initial protoplanets form log-uniformly distributed over the entire protoplanetary disk, the final planets are either very water-rich (water mass fraction ≳15%) or entirely rocky (water mass fraction ≲5%).
:&aname(planet1016){10/16}; Makiko Ban, Free-floating planet research and perspective|
The free-floating planet (FFP) is a unique type of exoplanet. There have been very scarce discoveries about it because of the difficulty of observation. The up-comming space-based telescope missions (Euclid and Roman) are expected to boost the FFP research. Here, I'd like to introduce FFPs, the challenges about the research we are facing, and future perspectives that will be offered by those up-comming missions through my latest paper.
:&aname(planet1030){10/30}; Yuki Tanaka, Gap formation by a super-Jupiter-mass planet and its effects on the planetary mass accretion rate|
A giant planet embedded in a protoplanetary disk creates a gap structure along with its orbit by disk-planet interaction. Physical properties of the gap depend on several conditions such as mass of the planet and disk structures, and they affect both mass accretion rate onto the planet via the gap and migration rate of the planet. Therefore, the properties of the gap are important to investigate formation and evolution of planetary systems.
Recently, numerical simulations of the disk-planet interaction have been done intensively, and the disk properties such as width and depth of the gap, and mass accretion rate have been studied. However, previous studies mainly focused on planets less massive than Jupiter. In addition, there are a discrepancy between several previous works on the mass accretion rate onto the planet heavier than Jupiter. Since a lot of super-Jupiter-mass planets have been found, formation and evolution of them in the protoplanetary disk should be investigated in more detail.
We performed a set of hydrodynamic simulation of disk-planet interaction and investigated the properties of the gap and their parameter dependence. We varied the planetary mass from 1 to 10 Jupiter masses. We found that the gap becomes deeper as planet's mass increases up to around 3 Jupiter masses, but in more massive cases the outer edge of the gap shows significant eccentricity, which is consistent with several previous works. In this eccentric regime, the gap depth becomes shallower than an empirical relation between the depth and the planetary mass due to non-steady behavior of the gap outer edge. We also estimated the mass accretion rate onto the planet by using our result and found that the accretion rate can increase when the planet's mass is heavier because of the eccentricity of the gap.
