原始行星盤內熱木星與母恆星之間的潮汐及磁交互作用

Abstract

It has been shown from the current observational data that there is a mass-semimajor axis correlation for hot Jupiters. This correlation is related to the absence of less massive giant planets (< 1 Jupiter mass) within 0.035AU from their parent stars. We employ numerical simulations to model the orbital evolution of a planet inside the magneto- spheric cavity of a proto-planetary disk and compare the results with the observational data. Our numerical result shows that while a massive planet can cause e ective stellar tides accompanied with a magnetic torque on its star and then undergoes an orbit decay, a less massive planet either survives or destructs at the 2:1 resonance with the inner edge of the disk depending on the eccentricity. We suggest that the tidal and magnetic interactions between young hot Jupiters and their parent proto-stars can explain the mass-semimajor axis correlation for hot Jupiters.