碩士 / 國立臺灣大學 / 天文物理研究所 / 96 / 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.
| Identifer | oai:union.ndltd.org:TW/096NTU05199002 |
| Date | January 2008 |
| Creators | Shih-Hsin Chang, 張世昕 |
| Contributors | 李太楓 |
| Source Sets | National Digital Library of Theses and Dissertations in Taiwan |
| Language | zh-TW |
| Detected Language | English |
| Type | 學位論文 ; thesis |
| Format | 58 |
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