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* ߥʡ2018 [#zbb5ecca]


// ߥʡȯɽ

** Schedule & History [#vfafd1d8]


|[[ 1 5/17 15:00->#planet0517]]| | Formation of the terrestrial planets in the solar system around 1 au via radial concentration of planetesimals|15:00|
|[[ 2 5/24 15:00->#planet0524]]|ȡ δ | Determination of outer edge of circumplanetary disk in local 3d hydrodynamic simulations |15:00|
|[[ 3 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|
|[[ 4 6/14 14:00->#planet0614]]|  | Numerical simulations of the giant impact onto the magma ocean||
|[[ 5 6/28 14:00->#planet0628]]|ʼƬ ζ | On the origin of Phobos and Deimos||
|[[ 6 7/12 14:00->#planet0712]]| ͭ | Inner solar system objects with hyperbolic orbits: Interstellar origin or Oort cloud comets?||
|[[ 7 7/19 14:00->#planet0719]]| ζǷ | 濴̤ˤ븶ϱ׿ʲѲ||
|[[ 8 7/26 14:00->#planet0726]]| ǵ | Orbital evolution of Saturn's mid-sized moons and the tidal heating of Enceladus||
|[[ 1 9/19 14:00->#planet0919]]|ȡ δ | ʸҲ (Tanigawa et al. 2012, ApJ, Distribution of Accreting Gas and Angular Momentum onto Circumplanetary Disks)||
|[[ 2 10/3 14:00->#planet1003]]| ѰϺ | Planetesimal Formation by Gravitational Instability of a Porous Dust Disk||
|[[ 3 10/24 14:00->#planet1024]]| ůϯ | Chondrule Survivability in the Protosolar disk ||
|[[ 4 10/31 13:00->#planet1031]]|Jason Man Yin Woo | The curious case of Mars' formation |13:00|
|[[ 5 11/7 14:00->#planet1107]]|һ |The formation and dynamical evolution of super-Earths through in-situ giant impacts around M dwarfs ||
|[[ 6 11/14 15:00->#planet1114]]|Adrien Leleu |Stability and detectability of co-orbital exoplanets |15:00- ߥʡ|
|[[ 7 11/21 13:00->#planet1121]]|ƣͪΤ |On the radiation hydrodynamic simulations of formation of circumplanetary disks ||
|[[ 8 11/29 14:00->#planet1129]]|Ĺëɧ |Reconsideration of Formation Process of Rocky Planetesimals |Thursday|
|[[ 9 12/19 14:00->#planet1219]]| |Metallicity Enhancement of Gas Giants by Late Accretion of Solids - the Effect of Orbital Evolution ||
|[[ 10 1/9 10:00->#planet0109]]|ӹ |N body simulation with collisional fragmentation for planet formation in giant impact stages ||
//|[[ 11 1/23 14:00->#planet0123]]|ͳ |Theoretical transmission spectra of exoplanet atmospheres with hydrocarbon haze: Exploration of metallicity-dependence and application to extremely low-density planet Kepler-51b ||
|[[ 11 2/13 15:00->#planet0213]]| |Gas flow around an embedded planet in a protoplanetary disk: the implications for planet formation ||


// ֥륹åϥȥ
:&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

:&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 MatsumotoThe 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 Mdwarfs. 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(planet1219){12/19}; Sho Shibata/ Metallicity Enhancement of Gas Giants by Late Accretion of Solids - the Effect of Orbital Evolution|
Recent studies of internal structure of gas giants suggest that their envelope is enriched with heavier elements than hydrogen and helium, relative to their central star composition. It is considered that these enrichment in heavy elements are caused by the capture of planetesimals during the late formation stage of gas giants. Zhou & Lin 2007 and Shiraishi & Ida 2008 performed orbital integrations of planetesimals around a growing protoplanet in a constant protoplanetary disk, and estimated the total captured mass of planetesimals for Jupiter and Saturn.  However, they assumed a simple formation models and neglected some physically important effects.
In this study, we investigated the effect of a planet migration on the capture of planetesimals, in a single-planetary system and a multi-planetary system, respectively. We find that planetesimals swept by a migrating planet are trapped at the mean-motion resonances (MMRs), which works as a barrier and prevents planetesimals from approaching the planet. Thus, planetary migration itself has little contribution to increasing the amount of captured planetesimals. However, in a multi-planetary system, we find an interesting process that breaks the resonance trap and increases the amount of planetesimals captured by the planets. This effect is important to consider the capture of planetesimals in a multi-planetary system.

//:&aname(planet0123){1/23}; Yui Kawashima/Theoretical transmission spectra of //exoplanet atmospheres with hydrocarbon haze: Exploration of metallicity-dependence and application to extremely low-density planet Kepler-51b|
//Recently, properties of exoplanet atmospheres have been constrained via multi-wavelength transit observation, which measures an apparent decrease in stellar brightness during planetary transit in front of its host star (called transit depth). Sets of transit depths so far measured at different wavelengths (called transmission spectra) for some exoplanets are featureless or flat, inferring the existence of haze particles in the atmospheres. Previous studies that addressed theoretical modeling of transmission spectra of hydrogen-dominated atmospheres with haze used some assumed distribution and size of haze particles. In Kawashima & Ikoma (2018), we developed new photochemical and microphysical models of the creation, growth, and settling of haze particles for deriving their size and number-density distributions in hydrogen-dominated atmospheres of close-in warm (< 1000 K) exoplanets. In this talk, using our developed models, we explore the metallicity-dependence of the production rate of haze and the resultant transmission spectra, and discuss implications for observations. Also, we apply our models to recently-observed extremely low-density planet Kepler-51b. We have found that for an extremely low-gravity planet such as Kepler-51b, haze particles grow significantly large in the upper atmosphere due to the small sedimentation velocity, resulting in the featureless or flat transmission spectrum in a wide wavelength range as observationally detected.
:&aname(planet0213){2/13}; Ayumu Kuwahara/Gas flow around an embedded planet in a protoplanetary disk: the implications for planet formation|
The three-dimensional structure of the gas flow around a planet is thought to influence the accretion of both gas and solid materials. In particular, the outflow in the mid-plane region may prevent the accretion of the solid materials and delay the formation of super-Earths' cores. However, it is not yet understood how the nature of the flow field and outflow speed change as a function of the planetary mass.
In this study, we investigate the dependence of gas flow around a planet embedded in a protoplanetary disc on the planetary mass.
Assuming an isothermal, inviscid gas disc, we perform three-dimensional hydrodynamical simulations on the spherical polar grid, which has a planet located at its centre.
We find that gas enters the Bondi or Hill sphere at high latitudes and exits through the mid-plane region of the disc regardless of the assumed planetary mass. The altitude from where gas predominantly enters the envelope varies with the planetary mass. We also derived the analytic solution of the outflow which is consistent of the results of simulations. The planet-induced gas flow may reduce the accretion of dust and pebbles onto the planet when planetary mass is larger than the square root of Stokes number of the particle. 
Our results suggest that the flow around proto-cores of super-Earths may delay their growth and, consequently, help them to avoid runaway gas accretion within the lifetime of the gas disc.
In this talk, I will also introduce a few latest results of test simulations related to the pebble accretion in the realistic three-dimensional gas flow field.

//:&aname(planet1107){5/21}; ̾ȥ|