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Planet のバックアップソース(No.48)

#norelated
* 惑星セミナー2018 [#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。

// セミナー発表順番
// 

** Schedule & History [#vfafd1d8]

[[2017年度>Planet2017]]
[[2016年度>Planet2016]]
[[2015年度>Planet2015]]
[[2014年度>Planet2014]]

|BGCOLOR(#ccf):|BGCOLOR(#ffc):|BGCOLOR(#ffc):|BGCOLOR(#fcf):|c
|日程|発表|タイトル|Remarks|h
|BGCOLOR(#ccf):|BGCOLOR(#ffc):|BGCOLOR(#ffc):|BGCOLOR(#fcf):|c
//|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 | 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 |TBA ||
|[[後期 第6回 11/21 14:00->#planet1121]]|藤井悠里 |On the radiation hydrodynamic simulations of formation of circumplanetary disks ||

//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

// ←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){5/21}; 名前 タイトル|
//アブスト