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| DC 欄位 | 值 | 語言 |
|---|---|---|
| dc.contributor.advisor | 朱有花(You-Hua Chu) | |
| dc.contributor.author | Yu-Hsiu Huang | en |
| dc.contributor.author | 黃昱修 | zh_TW |
| dc.date.accessioned | 2022-11-25T05:34:28Z | - |
| dc.date.available | 2022-07-15 | |
| dc.date.copyright | 2021-07-20 | |
| dc.date.issued | 2021 | |
| dc.date.submitted | 2021-07-16 | |
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| dc.identifier.uri | http://tdr.lib.ntu.edu.tw/jspui/handle/123456789/82034 | - |
| dc.description.abstract | 星際塵埃在星系的輻射過程和恆星形成中起著重要作用。這些過程取決於粉塵的特性,例如粉塵豐度、粒度分佈和化學成分。另一方面,塵埃的演化與星際介質的物理條件有關,這可能受星系形成歷史的影響。為了了解不同宇宙時期塵埃形成和破壞的複雜過程,我在最先進的宇宙學模擬 Illustris The Next Generation (簡稱 TNG)中利用後處理模型,開發了一套新的高效塵埃演化模型。本論文主要關注兩個部分:塵埃在類銀河系星系的演化,以及恆星形成星系(starforming galaxy)的塵埃性質。在第一部分中,我通過將模型應用於 TNG 中的類銀河系星系並將計算出的塵埃特性並與觀測結果進行比較來驗證模型。在這部分,我不僅成功再現了銀河系消光曲線(extinction curve),還成功再現了在附近星系中觀察到的塵埃與金屬的比例關係。在第二部分,我嘗試探索不同宇宙時期恆星形成星系的塵埃特性。其中特別針對 TNG 中 z = 2 的恆星形成星系,因為宇宙恆星形成率在被稱為宇宙正午的時期達到峰值。在 z = 2 處,新樣本的晶粒尺寸分佈以大顆粒為主,大顆粒區域的彌散很小,這與類銀河系星系的塵埃尺寸演化不同。為了與宇宙正午觀測到的恆星形成星系的特性進行更穩健的比較,我使用輻射轉移(radiative transfer)模擬程式 SKIRT 計算每個星系的光譜能量分佈(spectral energy distribution)。利用我的模型,我討論了與塵埃相關的星系特性,例如衰減曲線和 IRX–β 關係。 | zh_TW |
| dc.description.provenance | Made available in DSpace on 2022-11-25T05:34:28Z (GMT). No. of bitstreams: 1 U0001-1507202113262800.pdf: 21088699 bytes, checksum: f1c8da15912be2e30ed09227558cedcc (MD5) Previous issue date: 2021 | en |
| dc.description.tableofcontents | "Verification Letter from the Oral Examination Committee i 致謝 iii 摘要 v Abstract vii Contents ix List of Figures xiii Chapter 1 Introduction 1.1 Dust in Galaxies ............................ 1 1.2 Numerical Understanding of Dust ................... 2 1.3 About This Work............................ 5 Chapter 2 Methods 2.1 IllustrisTNG .............................. 9 2.2 Dust Model............................... 11 2.2.1 Fundamental Mechanisms ...................... 12 2.2.2 Dense Gas Fraction .......................... 14 2.2.3 Dust Evolution and Gas Accretion .................. 15 2.2.4 Dust Evolution and Galaxy Mergers ................. 16 2.3 Extinction Curves and MieTheory................... 17 2.4 Radiative Transfer: SKIRT........................ 20 Chapter 3 Parameter Dependence 3.1 Gas Mass associated with the Dust Evolution . . . . . . . . . . . . . 23 3.2 Dense Gas Fraction........................... 25 3.3 Shattering and Coagulation....................... 25 3.4 Choice of Fiducial Parameters ..................... 30 Chapter 4 Milky-Way Analogs 4.1 Sample Selections for Miky-Way Analogs. . . . . . . . . . . . . . . 31 4.2 Results ................................. 33 4.2.1 Dust-to-Gas Ratio and Metallicity .................. 33 4.2.2 Grain Size Distributions........................ 37 4.2.3 ExtinctionCurves........................... 40 4.3 Discussion ............................... 41 4.3.1 D-to-Z: outliers and redshift evolution . . . . . . . . . . . . . . . . 42 4.3.2 Grain Size Distributions and Extinction curves . . . . . . . . . . . . 43 4.3.3 MW-like extinction curves ...................... 46 4.3.4 Dispersion in the Grain Size Distributions . . . . . . . . . . . . . . 48 4.3.5 Other Simulations of the Grain Size Distribution . . . . . . . . . . . 49 4.4 Conclusion ............................... 50 Chapter 5 Star-Forming Galaxies at Cosmic Noon 5.1 Sample Selection for Star-forming Galaxies . . . . . . . . . . . . . . 54 5.2 Results ................................. 55 5.2.1 Basic Dust Properties......................... 56 5.2.2 SEDs ................................. 59 5.2.3 IRX–β Relation............................ 61 5.2.4 Attenuation Curves .......................... 63 5.3 Discussion ............................... 64 5.3.1 Extinction versus Attenuation..................... 64 5.3.2 Effects of Age, Metallicity, and Stellar Mass on the Attenuation . . . 71 5.3.3 Complexity of Star–Dust Geometry in Attenuation . . . . . . . . . 75 5.4 Conclusions............................... 78 References 81 Appendix A — Resolution test 91 A.1 Effect on dust model .......................... 91" | |
| dc.language.iso | en | |
| dc.subject | 星際介質 | zh_TW |
| dc.subject | 塵埃 | zh_TW |
| dc.subject | 星系演化 | zh_TW |
| dc.subject | dust | en |
| dc.subject | interstellar medium | en |
| dc.subject | galaxy evolution | en |
| dc.title | 塵埃在星系中演化的理論模型 | zh_TW |
| dc.title | Theoretical Modeling of Dust Evolution in Galaxies | en |
| dc.date.schoolyear | 109-2 | |
| dc.description.degree | 碩士 | |
| dc.contributor.author-orcid | 0000-0002-4982-0208 | |
| dc.contributor.coadvisor | 平下博之(Hiroyuki Hirashita) | |
| dc.contributor.oralexamcommittee | 王為豪(Hsin-Tsai Liu),林彥廷(Chih-Yang Tseng),薛熙于 | |
| dc.subject.keyword | 塵埃,星系演化,星際介質, | zh_TW |
| dc.subject.keyword | dust,galaxy evolution,interstellar medium, | en |
| dc.relation.page | 93 | |
| dc.identifier.doi | 10.6342/NTU202101484 | |
| dc.rights.note | 同意授權(限校園內公開) | |
| dc.date.accepted | 2021-07-16 | |
| dc.contributor.author-college | 理學院 | zh_TW |
| dc.contributor.author-dept | 物理學研究所 | zh_TW |
| dc.date.embargo-lift | 2023-07-31 | - |
| 顯示於系所單位: | 物理學系 | |
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