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| DC 欄位 | 值 | 語言 |
|---|---|---|
| dc.contributor.advisor | 吳柏鋒 | zh_TW |
| dc.contributor.advisor | Po-Feng Wu | en |
| dc.contributor.author | 董沛承 | zh_TW |
| dc.contributor.author | Pei-Cheng Tung | en |
| dc.date.accessioned | 2024-08-05T16:24:55Z | - |
| dc.date.available | 2024-08-06 | - |
| dc.date.copyright | 2024-08-05 | - |
| dc.date.issued | 2024 | - |
| dc.date.submitted | 2024-07-24 | - |
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It’s a Breeze: The Circumgalactic Medium of a Dwarf Galaxy is Easy to Strip. arXiv: 2404.00129 [id='astro-ph.GA' fullname =′ AstrophysicsofGalaxies′isactive = Truealtname = Noneinarchive =′ astro − ph′isgeneral = Falsedescription =′ PhenomenapertainingtogalaxiesortheMilkyWay.Starclusters,HIIregionsandplanetarynebu Zhu, Weishan, Fupeng Zhang, and Long-Long Feng (Jan. 2022). “Impact of Cosmic Filaments on the Gas Accretion Rate of Dark Matter Halos”. In: The Astrophysical Journal 924.2, p. 132. ISSN: 1538-4357. DOI: 10.3847/1538-4357/ac37b9. URL: http://dx.doi.org/10.3847/1538-4357/ac37b9. | - |
| dc.identifier.uri | http://tdr.lib.ntu.edu.tw/jspui/handle/123456789/93535 | - |
| dc.description.abstract | 根據現代宇宙學，宇宙從較小的結構逐漸形成較大的結構。因此，研究矮星系的演化對於理解像銀河系這樣更大質量星系的形成和演化至關重要。在星系的演化歷史中，星系與其周圍的星系周介質(CGM)和星系際介質(IGM)之間的相互作用起著重要作用。從CGM和IGM吸積的氣體冷卻並流入星系，促進恆星形成。與此同時，來自恆星和中心超大質量黑洞(SMBH)的回饋將能量和物質返回CGM和IGM，形成一個包含各種氣體相態的動態生態系統。
在本研究中，我們集中研究了在紅移(z)為0、1和2的星形成矮星系中從周圍環境吸積氣體。我們使用Gizmo程式中的無網格方法進行了包含多種物理的3D、N體和流體動力學模擬。為了現實地解決這個問題，我們採用了最新宇宙學模擬IllustrisTNG的結果作為我們模擬的初始條件。我們檢查了吸積CGM氣體的物理性質，並研究了它如何影響不同環境中的矮星系演化。 我們的結果顯示，來自CGM的氣體可以顯著影響星系的重子含量，有助於總質量和恆星形成的增長。同一紅移下，來自CGM的貢獻也顯示出一致性。然而，來自IGM的氣體吸積在z∼2時顯著。這種來自IGM的強吸積流也觸發了星系中心的強烈AGN活動和緻密恆星形成。 | zh_TW |
| dc.description.abstract | According to modern cosmology, the universe forms hierarchically from smaller structures to larger ones. Therefore, studying the evolution of dwarf galaxies is crucial for understanding the formation and evolution of more massive galaxies, such as the Milky Way. Throughout a galaxy’s evolutionary history, the interactions between the galaxy, its circumgalactic medium (CGM), and the intergalactic medium (IGM) play important roles. Gas accreted from the CGM and IGM cools and flows into a galaxy, fueling star forma- tion. Meanwhile, feedback from stars and the central supermassive black hole (SMBH) returns energy and matter to the CGM and IGM, resulting in a dynamic ecosystem with various gas phases.
In this research, we focus on the accretion of gas from the surrounding environment to star-forming dwarf galaxies at redshifts (z) of 0, 1, and 2. We present 3D N-body and hydrodynamical simulations with multi-physics using the meshless method in the Gizmo code. To address the question realistically, we adopt the results from the state-of-the-art cosmology simulation, IllustrisTNG, as the initial conditions for our simulations. We have examined the physical properties of the accreting CGM gas and studied how it affects the evolution of dwarf galaxies in different environments. Our results demonstrate that gas from the CGM can significantly impact the galaxy’s baryon content, contributing to growth in total mass and star formation. The contribution from the CGM also shows consistency at the same redshift. However, gas accretion from the IGM is significant at z ∼ 2. This strong accretion flow from the IGM also triggers intense AGN activity and compact star formation at the galaxy’s center. | en |
| dc.description.provenance | Submitted by admin ntu (admin@lib.ntu.edu.tw) on 2024-08-05T16:24:55Z No. of bitstreams: 0 | en |
| dc.description.provenance | Made available in DSpace on 2024-08-05T16:24:55Z (GMT). No. of bitstreams: 0 | en |
| dc.description.tableofcontents | Acknowledgements iii
摘要 v Abstract vii Contents ix List of Figures xiii List of Tables xv Denotation xvii Chapter 1: Introduction 1 Chapter 2: Methodology 5 2.1 Hydrodynamics 5 2.1.1 Governing equations 7 2.1.2 Time Integration 10 2.1.3 Turbulent Mixing 10 2.1.4 Super-Lagrangian Refinement 11 2.2 Gravity 12 2.2.1 Softening Length 13 2.3 Cooling 14 2.4 Star Formation and Stellar Feedback 15 2.5 Supermassive Black Hole 16 2.6 Simulation Setup 18 2.6.1 Initial Conditions 18 2.6.2 Resolution 21 2.6.3 Simulation Settings 22 Chapter 3: Results 25 3.1 Basic Properties and Evolution of the Dwarf Galaxies 25 3.1.1 Star Formation Rate, Accretion Rate, and SMBH Mass Evolution 25 3.1.2 List of the Basic Properties 28 3.2 Baryon Evolution of the Dwarf Galaxies 30 3.2.1 Gas Morphology and Distribution 30 3.2.2 Newborn Star Distribution 31 3.2.3 Radial Mass Distribution 36 3.3 Phases in Disk, CGM, and IGM 39 3.3.1 Spatial Distribution of Different Gas Temperature 43 Chapter 4: Discussion 45 4.1 Metal Enrichment and Mixing in CGM 45 4.2 Phases Difference Comparing to Cosmological Simulation 46 4.3 Gas Accretion Contribution 49 4.3.1 Contribution to Star Formation 50 4.3.2 Contribution to Total Gas content 51 4.4 Comparison with More Massive Galaxies 56 Chapter 5: Conclusion 59 References 61 Appendix A — Numerical Details 71 Convergence Test 71 | - |
| dc.language.iso | en | - |
| dc.title | 矮星系及其環繞星系介質在宇宙時間下的共同演化 | zh_TW |
| dc.title | The Co-evolution of Dwarf Galaxies and Their Circumgalactic Medium Across Cosmic Time | en |
| dc.type | Thesis | - |
| dc.date.schoolyear | 112-2 | - |
| dc.description.degree | 碩士 | - |
| dc.contributor.coadvisor | 陳科榮 | zh_TW |
| dc.contributor.coadvisor | Ke-Jung Chen | en |
| dc.contributor.oralexamcommittee | 黃崇源;胡家瑜 | zh_TW |
| dc.contributor.oralexamcommittee | Chorng-Yuan Hwang;Chia-Yu Hu | en |
| dc.subject.keyword | 計算天文物理,矮星系,冷吸積,環繞星際物質,星系際介質, | zh_TW |
| dc.subject.keyword | Computational astrophysics,Dwarf galaxy,Cold accretion,Circumgalactic medium,Intergalactic medium, | en |
| dc.relation.page | 75 | - |
| dc.identifier.doi | 10.6342/NTU202400841 | - |
| dc.rights.note | 未授權 | - |
| dc.date.accepted | 2024-07-24 | - |
| dc.contributor.author-college | 理學院 | - |
| dc.contributor.author-dept | 應用物理研究所 | - |
| 顯示於系所單位： | 應用物理研究所 | |
文件中的檔案：
| 檔案 | 大小 | 格式 | |
|---|---|---|---|
| ntu-112-2.pdf 目前未授權公開取用 | 56.85 MB | Adobe PDF |
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