| DC 欄位 |
值 |
語言 |
| DC.contributor | 天文研究所 | zh_TW |
| DC.creator | 以菈 | zh_TW |
| DC.creator | I Putu Wira Hadiputrawan | en_US |
| dc.date.accessioned | 2020-7-29T07:39:07Z | |
| dc.date.available | 2020-7-29T07:39:07Z | |
| dc.date.issued | 2020 | |
| dc.identifier.uri | http://ir.lib.ncu.edu.tw:88/thesis/view_etd.asp?URN=106229601 | |
| dc.contributor.department | 天文研究所 | zh_TW |
| DC.description | 國立中央大學 | zh_TW |
| DC.description | National Central University | en_US |
| dc.description.abstract | 摘要
海王星軌道外的柯伊伯帶有一個關鍵特徵在於，有些物體會與海王星伴隨著軌道共振。最具代表性的就是矮行星冥王星與海王星有著3：2的共振。在伴隨著冥王星附近，有許多稱為Plutinos的KBO(Kuiper belt objects)與海王星也有相同的軌道關係。根據行星軌道遷移理論，冥王星、Plutinos和其他族群因為海王星的向外遷移而被捕獲至3:2、4:3、5:3、 2:1和 5:2軌道共振。在此論文研究中，我們探討了在3：2共振中存在多個類似冥王星大小（或更大）物體的可能性，以及柯伊伯帶結構相對應的動力學影響。除了探究早期太陽系的混沌演化歷史外，這種情況引起了矮行星在碎片盤中的散射過程這類新興主題。我們從模擬結果得出的結論是，在海王星向外遷移之後，由海王星捕獲到共振區，從10到50天文單位範圍中，類冥王星物體的初始數目可能小於10個。對於以後的研究工作，該結果可以作為長期演化模擬邊界條件的參考。 | zh_TW |
| dc.description.abstract | Abstract
A key feature of the architecture of the Kuiper belt outside the orbit of Neptune has to do with the presence of objects trapped in different mean-motion resonances with Neptune. The dwarf planet, Pluto, in 3:2 resonance with Neptune is the most outstanding representative. Accompanying Pluto, there are many KBOs, called Plutinos, also have the same orbital relation with Neptune. According to the theory of planetary orbital migration, Pluto and Plutinos and other groups were captured into the 3:2, 4:3. 5:3, 2:1 and 5:2 resonances by the outward orbital drift of Neptune. In this study, we explored the possibility of the existence of multiple Pluto-sized (or bigger) objects in the 3:2 resonance and the corresponding dynamical effects on the structure of the Kuiper belt. Besides serving as a probe to the chaotic evolutionary history of the early solar system, this scenario is also of interest to the emerging topic of scattering process of dwarf planets in debris disks. Our results lead into conclusion that perhaps after Neptune migrated outward, the initial number of large planetoids in the disk region from 10 to 50 au that to be captured into resonance area with Neptune could be smaller than 10. For future work, this result can be used to determine the boundary condition for another set of long-term simulations | en_US |
| DC.subject | 行星式 | zh_TW |
| DC.subject | 柯伊伯帶 | zh_TW |
| DC.subject | 冥王星 | zh_TW |
| DC.subject | 太陽系 | zh_TW |
| DC.subject | 動態的 | zh_TW |
| DC.subject | 計算方式 | zh_TW |
| DC.subject | Planetary | en_US |
| DC.subject | Kuiper Belt | en_US |
| DC.subject | Pluto | en_US |
| DC.subject | Solar System | en_US |
| DC.subject | Dynamical | en_US |
| DC.subject | Computation | en_US |
| DC.title | 原始柯伊伯帶中冥王星大小物體的動力學演化 | zh_TW |
| dc.language.iso | zh-TW | zh-TW |
| DC.title | On the Dynamical Evolution of Pluto-Sized Objects in the Primordial Kuiper Belt | en_US |
| DC.type | 博碩士論文 | zh_TW |
| DC.type | thesis | en_US |
| DC.publisher | National Central University | en_US |