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作者(中文):張哲恩
作者(外文):Chang, Tze-En
論文名稱(中文):Kepler-210 行星系統軌道參數的研究
論文名稱(外文):Investigating the Orbital Parameters of the Kepler-210 Planetary System
指導教授(中文):江瑛貴
指導教授(外文):Jiang, Ing-Guey
口試委員(中文):葉麗琴
潘國全
口試委員(外文):Yeh, Li-Chin
Pan, Kuo-Chuan
學位類別:碩士
校院名稱:國立清華大學
系所名稱:天文研究所
學號:106025503
出版年(民國):109
畢業學年度:108
語文別:英文
論文頁數:54
中文關鍵詞:系外行星Kepler-210 行星系統凌星時間變異
外文關鍵詞:ExoplanetKepler-210 planetary systemTransit Timing Variations
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Kepler-210b和Kepler-210c是離恆星Kepler-210很近的兩顆行星,這兩顆行星有掩星現象及transit timing variation (TTV)。本篇論文的目標是運用擬合TTV的技巧得到兩顆行星的軌道參數並討論是否有第三顆行星存在於該系統的可能性,我們使用TTVFAST動力模型擬合來自文獻上的498掩星資料,我們同時也用Differential Evolution Markov Chain with snooker update 來探索卡方檢驗下的最小值。從我們的結果可以知道行星b和行星c的質量分別是0.02M_J和0.95M_J,根據卡方檢驗的結果,我們也提出第三顆行星存在的可能性,並提供第三顆行星的軌道參數。在所有可能的的行星軌道結構中,第三顆行星坐落於行星b和行星c之外的軌道是最有可能且是個穩定的行星系統。
Kepler-210 b and Kepler-210 c are two close-orbiting transiting planets with confirmed transit timing variations (TTVs). The aim of this thesis is to constrain the orbital parameters of both planets and discuss the plausibility of an additional planet in the system by fitting the TTVs. We have used the dynamical model, TTVFast, to fit the total 498 transit data from the literature. A Differential Evolution Markov Chain with snooker update was performed to search the minima chi-square value. From our analysis, we obtain the mass of 0.02 $M_{\rm J}$ and 0.95 $M_{\rm J}$ for planet b and planet c respectively. We also claim the possible existence of planet d regarding the minima chi-square and provide the system orbital parameters. In the most favorable scenario, planet d is outside the two transiting planets, which satisfies our stability check.
1 Introduction 7
2 Target Details 11
3 Method and Setup 13
3.1 TTVFast and MC3 . . . . . . . . . . . . . . . . . . . . . . 13
3.2 Parameters and Priors . .. . . . . . . . . . . . . . . . . . 17
3.2.1 Two-Planet Case . . . . . . . . . . . . . . . . . . . . . 18
3.2.2 Three-Planet Case . . . . . . . . . . . . . . . . . . . . 20
4 Results 22
4.1 Two-Planet Scenario . . . . . . . . . . . . . . . . . . . . 22
4.2 Three-Planet Scenario . . . . . . . . . . . . . . . . . . . 28
5 Discussions 37
5.1 Mass-Eccentricity Degeneracy . . . . . . . . . . . . . . . . 37
5.2 Stability . . . . . . . . . . . . . . . . . . . . . . . . . 38
5.3 Habitable Zone . . . . . . . . . . . . . . . . . . . . . . . 41
6 The Conclusion and Future Work 43
6.1 Conclusion . . . . . . . . . . . . . . . . . . . . . . . . . 43
6.2 Future Work . . . . . . . . . . . . . . . . . . . . . . . . 44
A DEMC with Snooker Update 45
B GELMAN & ROBIN Convergence 49
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