9:15 AM - 9:30 AM
[AOS11-02] Water supply to the Habitable Zone of G-type stars and formation of terrestrial planets associated with the formation of Cool Jupiter
Keywords:Water Delivery, Planet Formation, Habitability, Cool Jupiter
The Habitable Zone (HZ) around G-type stars is crucial for the presence of liquid water on a planet's surface. However, the constraints of the HZ do not guarantee the supply of water, thus, it is necessary to confirm whether a planet is habitable through observation. Additionally, it is possible to verify the supply of water through calculations, which requires considering scenarios where water can be supplied while planets form.
In this study, we propose a model where the supply of water is facilitated through a process involving the inward migration of giant gas planets within the protoplanetary disk gap structures (Type-II planet migration), along with the inward movement of icy protoplanets into the HZ.Particularly, this model anticipates efficient transport of icy protoplanets as they are captured in mean motion resonances (MMR) during the migration process. We calculate the amount of water supplied by this model using the N-body calculation code library "REBOUND" to develop a simulation code that includes Type-II planet migration, thereby computing the transport of icy protoplanets. Water is supplied through the collision of icy protoplanets, transported from beyond the snow line, with the protoplanet. The process of water sublimation from the surface of icy protoplanets inside the snow line is also calculated to compute the amount of water supplied to the protoplanet.
As a result, the amount of water present on the remaining protoplanets after planet migration is approximately 10-44% of the mass of Earth's water content, and as a result of planet formation, we could confirm the presence of terrestrial planets with about 0.6M⊕ mass at around 1au, containing about 9.5% of Earth's water content. Moreover, during the process of planet migration, the icy protoplanets and water-supplied protoplanets moved inward while being captured in MMRs as proposed in our model, colliding and accreting, which also confirmed the validity of the model itself.
Hence, water supply through Type-II planet migration can be considered a useful process for supplying water to habitable planets. By applying this model to other systems with giant gas planets outside the HZ, it becomes possible to investigate the presence of habitable planets within the HZ. If similar results are obtained in other systems, the presence of giant gas planets outside the HZ could potentially serve as an indicator of habitable planets. This study is intended for presentation in a conference proceeding, emphasizing its importance in the search for habitable planet.
In this study, we propose a model where the supply of water is facilitated through a process involving the inward migration of giant gas planets within the protoplanetary disk gap structures (Type-II planet migration), along with the inward movement of icy protoplanets into the HZ.Particularly, this model anticipates efficient transport of icy protoplanets as they are captured in mean motion resonances (MMR) during the migration process. We calculate the amount of water supplied by this model using the N-body calculation code library "REBOUND" to develop a simulation code that includes Type-II planet migration, thereby computing the transport of icy protoplanets. Water is supplied through the collision of icy protoplanets, transported from beyond the snow line, with the protoplanet. The process of water sublimation from the surface of icy protoplanets inside the snow line is also calculated to compute the amount of water supplied to the protoplanet.
As a result, the amount of water present on the remaining protoplanets after planet migration is approximately 10-44% of the mass of Earth's water content, and as a result of planet formation, we could confirm the presence of terrestrial planets with about 0.6M⊕ mass at around 1au, containing about 9.5% of Earth's water content. Moreover, during the process of planet migration, the icy protoplanets and water-supplied protoplanets moved inward while being captured in MMRs as proposed in our model, colliding and accreting, which also confirmed the validity of the model itself.
Hence, water supply through Type-II planet migration can be considered a useful process for supplying water to habitable planets. By applying this model to other systems with giant gas planets outside the HZ, it becomes possible to investigate the presence of habitable planets within the HZ. If similar results are obtained in other systems, the presence of giant gas planets outside the HZ could potentially serve as an indicator of habitable planets. This study is intended for presentation in a conference proceeding, emphasizing its importance in the search for habitable planet.