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Planet のバックアップの現在との差分(No.39)


  • 追加された行はこの色です。
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#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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//|BGCOLOR(#ddf):|BGCOLOR(#ffd):|BGCOLOR(#ffd):|c
|[[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 | TBD||
|[[前期 第6回 7/12 14:00->#planet0712]]|樋口 有理可 | TBD||
|[[前期 第7回 7/26 14:00->#planet0719]]|原川 紘季 | TBD||
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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|


// ←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.
//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)
//古家:野津さん(理研) 
//石澤さん(京大)
//森島さん



//:&aname(planet1107){5/21}; 名前 タイトル|
//アブスト
//:&aname(long0514){5/14}; 名前 タイトル|
//アブスト
//:&aname(long0521){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%).