Ida Laboratory, Tokyo Institute of Technology


		* Planetary Formation Planetary Formation around Class G and Class M Stars Terrestrial Planet Formation using N-body simulation Asteroid Distribution in Main Belt The effects of tidal resistance and secular resonances on the evolution of the Asteroid Distribution in the Main Belt Left Figure: an example of a result of proto planet formation around class M stars using N-body simulation Four Planets are formed in mean motion resonance five million years after collisions and merging of planetesimals due to Type-I migration. ※ Green: Earth Mass, Red:0.1-1 Earth Mass, Blue:0.01-0.1 Earth Mass, Black: < 0.01 Earth Mass 　　　　　 N-body Movie　[Credit: M.Ogihara] * Terrestrial Planets Thermal Evolution of Terrestrial Planets Simulation of a time dependent heat transfer using a planetary interior model The mantle convection in the interior of Earth The origine of the water and atmosphere of Earth The capture of the water and atmosphere of Earth The capture of the disk gas and the Ne problem Study on Mercury formation with SPH Mercury formation considering the effect of a giant impact The right figure show a result of a giant impact of protoplanets 　　　　　　　　　　　　　　　　　　　　　　　　　　　　　　　　　 SPH Movie [Credit: H.Genda] * Gas Giants evolution of an interior structure of a gas giant planet evolution of an interior structure of Jupiter with the Heneyey Method Formation of Gas Giants The accretion of planetesimals on a gas giant with 3-body simulation right figure: Evolution of planetesimal orbits due to protoplanet grouth Evolution of elements of an orbit of a planetesimal around protoplanet assuming Bondi-accretion x-axis and y-axis mean the distance between a planetesimal and the proto planet and eccentricity, respectively. [:Planetesimals] (Shiraishi & Ida, ApJ, 2008 submitted) ※ broken line:feeding zone at t =0yr(Jacobi energy = 0)、 solid line:feeding zone at t=1000yr Protoplanetary Disks Evolution of snow line in the protoplanetary disk simulation of a migration of the snow line using radiation transfer equations Photoevapolation in the protoplanetary disk The photoevapolation due to EUV from the Sun and the formation of a gap Dust falling and accretion affected by turbulence in a magnetic field MRI instability and dust accretion affected by turbulence in a magnetic field The right figure shows a behavior of dust in MRI instability [contour:dust density] (Kato et al.,2008 in preparation) * Extrasolar Planets Observation of extrasolar planets with Doppler method and Transit method Detection and Observation of extrasolar planets with Doppler method and Transit method Extrasolar Planets Formation Planetary Formation by Jumping Jupiter model Gas Giants in an Extrasolar System Formation of extrasolar gas giants with large cores due to giant impacts The left figure shows radial velocity changes of HD149026b, which has a large core inside. (Sato et al., ApJ, 2007)