Presentation Information
[PPS04-P33]Coevolution calculations of multiple giant planets and a protoplanetary disk:
applications to our solar system and the PDS 70 system
Keiji Suzuki1, *Hidekazu Tanaka1 (1.Graduate School of Science, Tohoku University)
Keywords:
Jupiter,Saturn,PDS 70,protoplanetary disk,solar nebula
To elucidate the formation process and final masses of giant planets, the evolution of their protoplanetary disk must be solved simultaneously. In this study, we constructed a one-dimensional coevolution model of multiple giant planets and a protoplanetary disk. We used a precise planetary gap model planetary gas accretion rates, both of which were validated by hydrodynamical simulations. We applied this model to the formation of Jupiter and Saturn and to the PDS 70 planetary system. In our application to the formation of Jupiter and Saturn, we investigated the constraints on the disk mass required to reproduce their masses. Our results show that, at the start of Jupiter's gas accretion, the gas disk surface density must decrease to ~1/10 of the minimum mass solar nebula (MMSN) model, and to ~1/100 of the MMSN model by the time Jupiter is nearly fully formed. Such a less massive disk cannot cause the grand tack migration of Jupiter and Saturn. Conversely, a less massive disk during Jupiter's formation is consistent with Callisto's formation model.
In our application to the PDS 70 system, our coevolution calculation successfully reproduced the observed planetary masses and disk density distribution. Though, the accretion rates onto each planet are about one order of magnitude larger than values suggested by observations. Furthermore, our one-dimensional coevolution calculations successfully reproduced the results of previous hydrodynamic simulations of the PDS 70 system under the same conditions.
In our application to the PDS 70 system, our coevolution calculation successfully reproduced the observed planetary masses and disk density distribution. Though, the accretion rates onto each planet are about one order of magnitude larger than values suggested by observations. Furthermore, our one-dimensional coevolution calculations successfully reproduced the results of previous hydrodynamic simulations of the PDS 70 system under the same conditions.