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- W2189015622 abstract "We discuss accretion of cores of giant planets from planetesimals, based on the results of N-body simulations. We derive the core isolation mass, which is a final core mass as a result of runaway/oligarchic growth, as functions of disk mass and semimajor axis. The core accretion rate is well predicted by a theoretical model based on two-body approximation. If cores reach a critical mass of ∼ 10M⊕ during the persistence of disk gas, gas accretion onto the cores occurs and gas giants are formed. Modeling the gas accretion process, we discuss the dependence of formation sites of gas giants on disk mass, assuming a constant dust-gas ratio. In the minimum mass disk for the Solar system, gas giants can be formed only just outside at a few AU. On the other hand, giants can be formed well inside the snow line in disks 10 times as massive as the minimum mass disk. In such inner regions, the core accretion is so fast, that formation of gas giants is completed before the gas is dissipated. Since planets grow very rapidly from 10M⊕ to 100M⊕, our model predicts the deficit of planets with intermediate masses (10M⊕ to 100M⊕ )a ta ∼ af ew AU, which we call desert. The idea of planet desert may be consistent with the current observational data and will be examined in detail by future observations." @default.
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- W2189015622 date "2006-12-01" @default.
- W2189015622 modified "2023-09-26" @default.
- W2189015622 title "Formation of Cores of Giant Planets and an Implication for Planet Desert" @default.
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