Research Gallery

The upper plot illustrates our model, which shows a hot Jupiter orbiting a CTTS in a magnetospheric cavity of a protoplanetary disk. The initial orbit of the planet is set to lie at the 2:1 orbital resonance with the inner edge of the disk. The lower plot shows the orbital evolution through tidal and magnetic interactions between a hot Jupiter and its host star in a magnetospheric cavity. Four cases are presented in terms of different initial masses: 0.7, 1, 1.5, and 2 Jupiter masses (Mj). Each panel has three different tracks by modulating the initial eccentricity. The blue line is the orbital evolution of a planet in a circular orbit; the green line illustrates the case in which the planet of a given initial mass can migrate inward over the longest distance; the red line shows that the planet with a critical eccentricity destructs at the breaking point.