Tidal and magnetic interactions between a hot Jupiter and its host star in a protoplanetary disk
Date Issued
2008
Date
2008
Author(s)
Chang, Shih-Hsin
Abstract
It has been shown from the current observational data that there is a mass-semimajorxis correlation for hot Jupiters. This correlation is related to the absence of less massiveiant planets (< 1 Jupiter mass) within 0.035AU from their parent stars. We employumerical simulations to model the orbital evolution of a planet inside the magneto-pheric cavity of a proto-planetary disk and compare the results with the observationalata. Our numerical result shows that while a massive planet can cause e ective stellarides accompanied with a magnetic torque on its star and then undergoes an orbit decay, less massive planet either survives or destructs at the 2:1 resonance with the innerdge of the disk depending on the eccentricity. We suggest that the tidal and magneticnteractions between young hot Jupiters and their parent proto-stars can explain theass-semimajor axis correlation for hot Jupiters.
Subjects
extrasolar planets
planet formation
protoplanetary disk
File(s)![Thumbnail Image]()
Loading...
Name
ntu-97-R95244006-1.pdf
Size
23.53 KB
Format
Adobe PDF
Checksum
(MD5):108a5947a77cc5301604359a3f930256