10:00 AM - 10:15 AM
[AOS14-05] Cool Jupiters as Drivers of Planetesimal Transport to the Habitable Zone via Type-II Migration
Keywords:Habitable Zone, Planet Formation, MMR
Recent exoplanet observations have indicated that the number of terrestrial planets located around 1 AU is low due to the limitations of observational instruments. However, several upcoming missions planned through 2030 have the potential to detect such planets, making it increasingly important to understand planet formation processes within the habitable zones (HZs) of G-type stars similar to the Sun.
Previous studies have suggested that planets can form in dynamically stable regions within the Mean Motion Resonance (MMR) of giant gas planets. However, these studies have primarily assumed that giant gas planets form in situ, without adequately considering the effects of Type-II migration. Therefore, this study aims to quantitatively evaluate the possibility that planetesimals and protoplanets are trapped in MMRs during the Type-II migration of Cool Jupiters and are ultimately transported to the HZ.
For the analysis, we employ the N-body simulation code REBOUND and its extended version, REBOUNDx, incorporating physical processes such as Type-II migration, gas drag, and water sublimation. The initial conditions include the orbital elements of a Cool Jupiter at the time of its formation, the initial distribution of planetesimals and protoplanets, and the physical properties of the gas disk. Under these conditions, we analyze the efficiency of planetesimal transport to the HZ.
This presentation reports on the gravitational stability of planetary systems after experiencing Type-II migration, as well as the transport of planetesimals and protoplanets to the HZ, based on current findings.
Previous studies have suggested that planets can form in dynamically stable regions within the Mean Motion Resonance (MMR) of giant gas planets. However, these studies have primarily assumed that giant gas planets form in situ, without adequately considering the effects of Type-II migration. Therefore, this study aims to quantitatively evaluate the possibility that planetesimals and protoplanets are trapped in MMRs during the Type-II migration of Cool Jupiters and are ultimately transported to the HZ.
For the analysis, we employ the N-body simulation code REBOUND and its extended version, REBOUNDx, incorporating physical processes such as Type-II migration, gas drag, and water sublimation. The initial conditions include the orbital elements of a Cool Jupiter at the time of its formation, the initial distribution of planetesimals and protoplanets, and the physical properties of the gas disk. Under these conditions, we analyze the efficiency of planetesimal transport to the HZ.
This presentation reports on the gravitational stability of planetary systems after experiencing Type-II migration, as well as the transport of planetesimals and protoplanets to the HZ, based on current findings.