李太楓Lee, Ty-phoon臺灣大學:天文物理研究所謝和峯Hsieh, He-FengHe-FengHsieh2010-05-042018-06-282010-05-042018-06-282009U0001-1008200915422400http://ntur.lib.ntu.edu.tw//handle/246246/178569Close-in exoplanets receive more stellar irradiation, implying that the thermal tidesn these planets may not be negligible compared to the gravitational tides. To investigatehe properties of the atmospheric thermal tides excited by the irradiation from their parenttars, we perform a linear analysis to study the atmospheric perturbations of exoplanets.he torque due to the thermal tides acting on the spin of the planet is estimated andompared to that due to the gravitational tides. In particular, we study the thermal tidesn a hypothetical super-Earth with a hydrogen-rich atmosphere at about 0:47 AU from a Sunliketar and those in the radiative layer of the hot Jupiter HD 209458b. In the super-Earthase, the torques arising from both tides can be cancelled out in some ranges of forcingeriods, inferring that the super-Earth may have been escaped from the stage of beingidally locked by its parent star. In the case of gaseous planets, the thermal bulges haveeen argued not to exist in the literature. However, our study suggests that the thermalulges could form when the thermal variations of the atmosphere are not hydrostaticallyalanced by the redistribution of gas in the layer near the turning point of internal waves.n some ranges of forcing periods and Q-values, both torques can be cancelled out inhe case of the hot Jupiter HD 209458b. The results imply that some of the close-inxoplanets, including both super-Earths and gaseous planets, may not lie in synchronouslyotating states at their ages of serveral Gyrs.1 Introduction 6 Model Description 9.1 Plane-parallel atmosphere . . . . . . . . . . . . . . . . . . . . . . . . . . 10.1.1 Basic equations . . . . . . . . . . . . . . . . . . . . . . . . . . . 10.1.2 Background states . . . . . . . . . . . . . . . . . . . . . . . . . 11.1.3 Linear perturbation analysis . . . . . . . . . . . . . . . . . . . . 12.2 Torques due to the gravitational and thermal bulges . . . . . . . . . . . . 16.3 Dispersion relation of internal waves . . . . . . . . . . . . . . . . . . . . 18.4 Numerical method . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 22 Numerical Results 25.1 The super-Earth case . . . . . . . . . . . . . . . . . . . . . . . . . . . . 25.2 The HD 209458b case . . . . . . . . . . . . . . . . . . . . . . . . . . . 46 Summary and Discussions 57eferences…………62ppendix 63 The Derivation of Dispersion Relation of Internal Waves 64application/pdf27339980 bytesapplication/pdfen-US重力潮汐熱潮汐系外行星超級地球HD 209458bgravitational tidethermal tideexoplanetsuper-Earthhttp://ntur.lib.ntu.edu.tw/bitstream/246246/178569/1/ntu-98-R96244008-1.pdf