Japan Geoscience Union Meeting 2015

Presentation information


Symbol P (Space and Planetary Sciences) » P-PS Planetary Sciences

[P-PS21] Planetary Sciences

Sun. May 24, 2015 2:15 PM - 4:00 PM A02 (APA HOTEL&RESORT TOKYO BAY MAKUHARI)

Convener:*Kosuke Kurosawa(Planetary Exploration Research Center, Chiba Institute of Technology), Keiko Hamano(Department of Earth and Planetary Science, Graduate School of Science, University of Tokyo), Chair:Hiroshi Kobayashi(Department of Physics, Nagoya University), Sin-iti Sirono(Department of Earth and Planetary Sciences, Nagoya University)

3:30 PM - 3:45 PM

[PPS21-19] Effect of wave propagation for a planet-induced gap formation in protoplanetary disks

*Kazuhiro KANAGAWA1, Takayuki MUTO2, Hidekazu TANAKA1, Takayuki TANIGAWA3, Taku TAKEUCHI4 (1.ILTS, Hokkaido University, 2.Division of Liberal Arts, Kogakuin University, 3.School of Medicine, University of Occupational and Environmental Health, 4.Department of Earth and Planetary Sciences, Tokyo Institute of Technology)

Keywords:protoplanetary disk, disk-planet interaction, disk evolution

In a protoplanetary disc, a large planet is able to create the so-called disc gap, which is a low gas density region along with the planetary orbit, due to the gravitational interaction between the disc and the planet. The gap formation significantly affects the orbital evolution of planets such as the transition from type I migration to type II migration. It also prevents disc gas from accreting onto the planet and slows down the planetary growth. In addition, the gap formation induced by a giant planet possibly explains the formation of the so-called pre-transition disc with a ring gap. Hence, it is important to determine the relation between the planet mass and the gap depth and width.

According to our analysis with the one-dimensional model, the propagation and damping of the density wave excited by the planet is closely related to the gap depths and widths (Kanagawa et al 2015). Therefore, we computed the gap structure around the planet using FARGO, which is an open source code for hydrodynamic simulation. Results of the simulation show that in the case with the large planet (such as Jupiter), low-mode waves (in particular m=2 mode) become stronger than high-mode waves. Because the low-mode waves would be difficult to be damped by shock dispersion, these waves can propagate farther from the planet than high-mode waves.
In this talk, I will illustrate the results and discuss the wave propagation and gap formation for large planets.