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Planet のバックアップの現在との差分(No.20)


  • 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2017 [#zbb5ecca]
* 惑星セミナー2020 [#zbb5ecca]

惑星セミナーは原則として毎週火曜日の午後14:00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
// 脇田->押野->柴田->小久保->荻原->辰馬->瀧
// 

** 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|astro-ph|発表|h
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|[[前期 第1回 4/4>#planet0404]]|田中佑希 (3/20-24)|田中佑希 &br;「磁気流体波駆動のガス惑星からの質量放出」|
|[[前期 第2回 4/11>#planet0411]]|押野翔一(3/27-31) &br;柴田雄(4/3-7)|Steven Rieder(AICS, RIKEN)&br;「J1407b: a Super-Saturn or something else?」|
|[[前期 第3回 4/12>#planet0412]]||和田浩二(千葉工大)&br;「ダストアグリゲイトの衝突シミュレーション:成長できるのできないの?」|
|[[前期 第4回 4/25>#planet0425]]|小久保英一郎(4/10-14) &br;脇田茂(4/17-21)|脇田茂&br;「Asteroids and their compositions」|
|[[前期 第5回 5/9>#planet0509]]|荻原正博(4/24-28) &br;辰馬未沙子(5/1-5)||
|[[前期 第6回 5/16>#planet0516]]|瀧哲朗(5/8-12)|押野翔一&br;「High-Resolution N-body Simulations of Planet Formation」|
|[[前期 第7回 6/13>#planet0613]]|押上祥子(5/15-19)&br; 押野翔一(5/22-26)&br; 柴田雄(5/29-6/2)&br; 小久保英一郎(6/5-9)|柴田雄&br;「Spin of Protoplanets by Planetesimal accretion」|
|[[前期 第8回 7/4>#planet0704]]|脇田茂(6/12-16) &br;荻原正博(6/19-23) &br;辰馬未沙子(6/26-30)||
|[[前期 第9回 7/18>#planet0718]]|瀧哲朗(7/3-7) &br;押上祥子(7/10-14)|Ramon Brasser (ELSI)&br;「The Cool and Distant Formation of Mars」|
|[[前期 第10回 7/27>#planet0727]]|押野翔一(7/17-21)|辰馬未沙子&br;「Gravitational Instability of a Porous Silicate Dust Disk」|
|[[前期 第11回 8/3>#planet0803]]||Maxwell Cai (Leiden Observatory)&br;「Dynamical Evolution of Multiplanetary Systems in Star Clusters」|
|[[後期 第1回 9/5>#planet0905]]|柴田雄(7/24-28) &br;小久保英一郎(7/31-8/4) &br;脇田茂(8/7-8/11) &br;荻原正博(8/14-8/18)||
|[[後期 第2回 9/19>#planet0919]]||小久保英一郎&br;「The Final Stage of Terrestrial Planet Formation」|
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|日程|発表|タイトル|Remarks|担当|h
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//|BGCOLOR(#ddf):|BGCOLOR(#ffd):|BGCOLOR(#ffd):|BGCOLOR(#cff):|c
|[[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|

** astro-ph リンク [#gd4ae1b1]

:&aname(planet0404){4/4};|
//今後の候補
//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

田中佑希 (3/20-24)~

- [[Reassessment of the Null Result of the HST Search for Planets in 47 Tucanae:https://arxiv.org/abs/1703.06136]]
- [[Assessing the Habitability of the TRAPPIST-1 System Using a 3D Climate Model:https://arxiv.org/abs/1703.05815]]
- [[The GTC exoplanet transit spectroscopy survey. VII. Detection of sodium in WASP-52b's cloudy atmosphere:https://arxiv.org/abs/1703.06716]]
- [[Formation of TRAPPIST-1 and other compact systems:https://arxiv.org/abs/1703.06924]]
- [[Testing the existence of optical linear polarization in young brown dwarfs:https://arxiv.org/abs/1703.07341]]
- [[The effect of the stellar absorption line centre-to-limb variation on exoplanet transmission spectrum observations:https://arxiv.org/abs/1703.07585]]
- [[Planetesimal formation by the streaming instability in a photoevaporating disk:https://arxiv.org/abs/1703.07895]]

//:&aname(planet1107){5/21}; 名前 タイトル|
//アブスト

:&aname(planet0411){4/11};|
//:&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.

押野翔一(3/27-31)~
:&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%).

- [[The stability of tightly-packed, evenly-spaced systems of Earth-mass planets orbiting a Sun-like star:https://arxiv.org/abs/1703.08426]]
- [[Water transport to circumprimary habitable zones from icy planetesimal disks in binary star systems:https://arxiv.org/abs/1703.09000]]
- [[Size and density sorting of dust grains in SPH simulations of protoplanetary discs:https://arxiv.org/abs/1703.10385]]
:&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.

柴田雄(4/3-7)~
:&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.

- [[The cool and distant formation of Mars:https://arxiv.org/abs/1704.00184]]


:&aname(planet0425){4/25};|

小久保英一郎(4/10-14)~

- [[Plausible Compositions of the Seven TRAPPIST-1 Planets Using Long-term Dynamical Simulations:https://arxiv.org/abs/1704.02261]]
- [[The curiously warped mean plane of the Kuiper belt:https://arxiv.org/abs/1704.02444]]
- [[Limits on the Stability of TRAPPIST-1:https://arxiv.org/abs/1704.02957]]
- [[A Minimum Mass Nebula for M Dwarfs:https://arxiv.org/abs/1704.03265]]
- [[The Destruction of an Oort Cloud in a rich stellar cluster:https://arxiv.org/abs/1704.03341]]

脇田茂(4/17-21)~

- [[Testing the chondrule-rich accretion model for planetary embryos using calcium isotopes:https://arxiv.org/abs/1704.05726]]


:&aname(planet0509){5/9};|

荻原正博(4/24-28)~

- [[Planetary migration and the origin of the 2:1 and 3:2 (near)-resonant population of close-in exoplanets:https://arxiv.org/abs/1704.06459]]
- [[Acceleration of Cooling of Ice Giants by Condensation in Early Atmospheres:https://arxiv.org/abs/1704.07558]]
- [[Titan brighter at twilight than in daylight:https://arxiv.org/abs/1704.07460]]
- [[Avoiding resonance capture in multi-planet extrasolar systems:https://arxiv.org/abs/1704.07836]]

辰馬未沙子(5/1-5)~

- [[3D radiative transfer of intrinsically polarized dust emission based on aligned aspherical grains:https://arxiv.org/abs/1705.01047]]
- [[Survey of cold water lines in protoplanetary disks: indications of systematic volatile depletion:https://arxiv.org/abs/1705.00799]]
- [[A likely detection of a local interplanetary dust cloud passing near the Earth in the AKARI mid-infrared all-sky map:https://arxiv.org/abs/1705.01541]]


:&aname(planet0516){5/16};|

瀧哲朗(5/8-12)~

- [[Composition of Early Planetary Atmospheres II: Coupled Dust and Chemical Evolution in Protoplanetary Disks:https://arxiv.org/abs/1705.02381]]
- [[Chemical enrichment of giant planets and discs due to pebble drift:https://arxiv.org/abs/1705.03305]]
- [[Evidence for universality in the initial planetesimal mass function:https://arxiv.org/abs/1705.03889]]
- [[N-body simulations of planet formation via pebble accretion I: First Results:https://arxiv.org/abs/1705.04264]]

:&aname(planet0613){6/13};|

押上祥子(5/15-19)~

- [[Dynamics of Porous Dust Aggregates and Gravitational Instability of Their Disk:https://arxiv.org/abs/1705.04520]]
- [[Detection of the Yarkovsky effect for C-type asteroids in the Veritas family:https://arxiv.org/abs/1705.04333]]
- [[Shape models and physical properties of asteroids:https://arxiv.org/abs/1705.05710]]
- [[Driven by Excess? Climatic Implications of New Global Mapping of Near-Surface Water-Equivalent Hydrogen on Mars:https://arxiv.org/abs/1705.05556]]
- [[The compositional diversity of non-Vesta basaltic asteroids:https://arxiv.org/abs/1705.06304]]

押野翔一(5/22-26)~

- [[Formation of Close-in Super-Earths by Giant Impacts: Effects of Initial Eccentricities and Inclinations of Protoplanets:https://arxiv.org/abs/1705.07810]]
- [[In situ accretion of gaseous envelopes on to planetary cores embedded in evolving protoplanetary discs:https://arxiv.org/abs/1705.08147]]


柴田雄(5/29-6/2)~

- [[Internal Structure of Giant and Icy Planets: Importance of Heavy Elements and Mixing:https://arxiv.org/abs/1705.09320]]
- [[Capture of free-floating planets by stellar systems:https://arxiv.org/abs/1705.10332]]

小久保英一郎(6/5-9)~

- [[Cladistical analysis of the Jovian and Saturnian satellite systems:https://arxiv.org/abs/1706.01423]]
- [[Dynamics and Collisional Evolution of Closely Packed Planetary Systems:https://arxiv.org/abs/1706.01975]]


:&aname(planet0704){7/4};|

脇田茂(6/12-16)~

- [[Radially resolved simulations of collapsing pebble clouds in protoplanetary discs:https://arxiv.org/abs/1706.03655]]


荻原正博(6/19-23)~

- [[Stable habitable zones of single Jovian planet systems:https://arxiv.org/abs/1706.05805]]
- [[Exoplanets as probes of the winds of host stars: the case of the M dwarf GJ 436:https://arxiv.org/abs/1706.05894]]
- [[Eccentricity excitation and merging of planetary embryos heated by pebble accretion:https://arxiv.org/abs/1706.06329]]
- [[The California-Kepler Survey V. Peas in a Pod: Planets in a Kepler Multi-planet System are Similar in Size and Regularly Spaced:https://arxiv.org/abs/1706.06204]]
- [[A giant planet undergoing extreme ultraviolet irradiation by its hot massive-star host:https://arxiv.org/abs/1706.06723]]
- [[Cloud formation in metal-rich atmospheres of hot super-Earths like 55 Cnc e and CoRot7b:https://arxiv.org/abs/1706.07219]]
- [[Gap and rings carved by vortices in protoplanetary dust:https://arxiv.org/abs/1706.07131]]

辰馬未沙子(6/26-30)~

- [[Low-velocity collision behaviour of clusters composed of sub-mm sized dust aggregates:https://arxiv.org/abs/1706.07512]]
- [[Submillimetre-sized dust aggregate collision and growth properties:https://arxiv.org/abs/1706.07492]]
- [[NanoRocks: Design and Performance of an Experiment Studying Planet Formation on the International Space Station:https://arxiv.org/abs/1706.08625]]


:&aname(planet0718){7/18};|

瀧哲朗(7/3-7)~

- [[Generation of inclined protoplanetary discs and misaligned planets through mass accretion I: Coplanar secondary discs:https://arxiv.org/abs/1706.09905]]
- [[Energy Options for Future Humans on Titan:https://arxiv.org/abs/1707.00365]]
- [[Global Simulations of the Inner Regions of Protoplanetary Disks with Comprehensive Disk Microphysics:https://arxiv.org/abs/1707.00729]]
- [[Centrifugally driven winds from protostellar accretion discs. I - Formulation and initial results:https://arxiv.org/abs/1707.01088]]
- [[Changes in orientation and shape of protoplanetary discs moving through an ambient medium:https://arxiv.org/abs/1707.01096]]

押上祥子(7/10-14)~

- [[Comparing Jupiter interior structure models to Juno gravity measurements and the role of a dilute core:https://arxiv.org/abs/1707.01997]]
- [[The highly active Anhur-Bes regions in the 67P/Churyumov - Gerasimenko comet: results from OSIRIS/ROSETTA observations:https://arxiv.org/abs/1707.02945]]
- [[The size distribution of Near Earth Objects larger than 10 meters:https://arxiv.org/abs/1707.04066]]


:&aname(planet0727){7/27};|

押野翔一(7/17-21)~

- [[On the Impact Origin of Phobos and Deimos I: Thermodynamic and Physical Aspects:https://arxiv.org/abs/1707.06282]]


:&aname(planet0905){9/5};|

柴田雄(7/24-28)~

- [[Seasonal Mass Transfer on the Nucleus of Comet 67P/Chuyumov-Gerasimenko:https://arxiv.org/abs/1707.06812]]

小久保英一郎(7/31-8/4)~

- [[Reduced gas accretion on super-Earths and ice giants:https://arxiv.org/abs/1708.00767]]
- [[The Formation of Uranus and Neptune: Fine Tuning in Core Accretion:https://arxiv.org/abs/1708.00862]]
- [[Simulations of Small Solid Accretion onto Planetesimals in the Presence of Gas:https://arxiv.org/abs/1708.00450]]

脇田茂(8/7-8/11)~

- [[Ejection of Chondrules from Fluffy Matrices:https://arxiv.org/abs/1708.02326]]
- [[Early formation of planetary building blocks inferred from Pb isotopic ages of chondrules:https://arxiv.org/abs/1708.02631]]

荻原正博(8/14-8/18)~

- [[What pebbles are made of: Interpretation of the V883 Ori disk:https://arxiv.org/abs/1708.03328]]


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