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Planet ¤Î¥Ð¥Ã¥¯¥¢¥Ã¥×¥½¡¼¥¹(No.44)

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* ÏÇÀ±¥»¥ß¥Ê¡¼2018 [#zbb5ecca]

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** Schedule & History [#vfafd1d8]

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

|BGCOLOR(#ccf):|BGCOLOR(#ffc):|BGCOLOR(#ffc):|BGCOLOR(#fcf):|c
|ÆüÄø|ȯɽ|¥¿¥¤¥È¥ë|Remarks|h
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//|BGCOLOR(#ddf):|BGCOLOR(#ffd):|BGCOLOR(#ffd):|c
|[[Á°´ü Âè1²ó 5/17 15:00->#planet0517]]|²®¸¶ ÀµÇî| Formation of the terrestrial planets in the solar system around 1 au via radial concentration of planetesimals|15:00|
|[[Á°´ü Âè2²ó 5/24 15:00->#planet0524]]|ÇÈ¡¹ÇìÉô ¹­Î´ | Determination of outer edge of circumplanetary disk in local 3d hydrodynamic simulations |15:00|
|[[Á°´ü Âè3²ó 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|
|[[Á°´ü Âè4²ó 6/14 14:00->#planet0614]]|ºÙÌî ¼··î | Numerical simulations of the giant impact onto the magma ocean||
|[[Á°´ü Âè5²ó 6/28 14:00->#planet0628]]|ʼƬ ζ¼ù | On the origin of Phobos and Deimos||
|[[Á°´ü Âè6²ó 7/12 14:00->#planet0712]]|Èõ¸ý Í­Íý²Ä | Inner solar system objects with hyperbolic orbits: Interstellar origin or Oort cloud comets?||
|[[Á°´ü Âè7²ó 7/19 14:00->#planet0719]]|ÃæÌî ζǷ²ð | Ãæ¿´À±¼ÁÎ̤ˤè¤ë¸¶»ÏÏÇÀ±·Ï±ßÈ׿ʲ½¤ÎÊѲ½||
|[[Á°´ü Âè8²ó 7/26 14:00->#planet0726]]|ÃæÅè ºÌǵ | Orbital evolution of Saturn's mid-sized moons and the tidal heating of Enceladus||
|[[¸å´ü Âè1²ó 9/19 14:00->#planet0919]]|ÇÈ¡¹ÇìÉô ¹­Î´ | ÏÀʸ¾Ò²ð (Tanigawa et al. 2012, ApJ, Distribution of Accreting Gas and Angular Momentum onto Circumplanetary Disks)||
|[[¸å´ü Âè2²ó 10/3 14:00->#planet1003]]|¾®µ×ÊÝ ±Ñ°ìϺ | Planetesimal Formation by Gravitational Instability of a Porous Dust Disk||
|[[¸å´ü Âè3²ó 10/24 14:00->#planet1024]]|Âí ůϯ | Chondrule Survivability in the Protosolar disk ||
|[[¸å´ü Âè4²ó 10/31 13:00->#planet1031]]|Jason Man Yin Woo | The curious case of Mars' formation |13:00|
|[[¸å´ü Âè5²ó 11/7 14:00->#planet1107]]|¾¾ËÜÐһΠ|TBA ||
|[[¸å´ü Âè6²ó 11/21 14:00->#planet1121]]|Æ£°æÍªÎ¤ |On the radiation hydrodynamic simulations of formation of circumplanetary disks ||

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:&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.

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:&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}; ̾Á°¡¡¥¿¥¤¥È¥ë|
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