臺灣博碩士論文加值系統

本論文我們以粒子模擬和低等溫模型來研究球狀星團。首先，我們檢驗模擬中的變量圖和特定性質的粒子來探討星團和中質量黑洞的交互作用。然後，我們透過觀測的資料和低等溫模型配合，研究十八個球狀星團的性質，並估計這些星團的模型參數和物理尺寸。整體而言，模型能描述這些星團。此外，我們亦討論較特殊的星團及探討其他議題如中質量黑洞的可能宿主以及非各向同性。我們發現部份參數之間有較強的相關性，其反應銀河系潮汐力和星團的動力學演化之影響。

In this work, we used N-body simulations and lowered isothermal models to study globular clusters. We examined the profiles and specific properties of the particles in the simulations to investigate the interactions between the cluster and the intermediate-mass black hole. The eighteen globular clusters were studied through the fitting of the observational data with a family of lowered isothermal models. The model parameters and the physical sizes of these clusters were estimated. In general, the models could describe these clusters well and some special clusters were discussed individually. The subjects like the candidate hosts of the intermediate-mass black holes and the anisotropy were also discussed. Some stronger correlations between the parameters were revealed which could provide the imprint of the Galactic tidal field and dynamical evolutions of the clusters.

List of Figures 3
List of Tables 4
1 Introduction 5
2 Simulation Set up 10
2.1 Density and Potential . . . . . . . . . . . . . . . . . . . . . . . . . . 10
2.2 Initial Conditions . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 12
2.3 Cluster Parameters . . . . . . . . . . . . . . . . . . . . . . . . . . . . 15
3 Simulation Results 18
3.1 Cluster Profiles . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 18
3.2 Particles with Specific Properties . . . . . . . . . . . . . . . . . . . . 21
3.3 Model Descriptions . . . . . . . . . . . . . . . . . . . . . . . . . . . . 24
4 Lowered Isothermal Models 25
4.1 Mathematical Form . . . . . . . . . . . . . . . . . . . . . . . . . . . . 25
4.2 Model Properties . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 26
5 Observational Data 29
5.1 Surface Brightness . . . . . . . . . . . . . . . . . . . . . . . . . . . . 29
5.2 Kinematic Profiles . . . . . . . . . . . . . . . . . . . . . . . . . . . . 30
6 Determination of Physical Parameters 32
6.1 Concepts . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 32
6.2 Fitting Procedure . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 34
7 Fitting Results 36
7.1 Comparison with Previous Work . . . . . . . . . . . . . . . . . . . . 37
7.2 Profiles . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 41
7.3 Possible Intermediate-Mass Black Hole ? . . . . . . . . . . . . . . . . 42
7.4 Anisotropy . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 47
7.5 Imprint of Galactic Tidal Field . . . . . . . . . . . . . . . . . . . . . 51
8 Summary and Conclusions 56
Bibliography 59

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