合併星系下超大質量黑洞與宿主星系的共同演化

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姓名	林祺紘(Chi-Hong Lin) 查詢紙本館藏	畢業系所	天文研究所
論文名稱	合併星系下超大質量黑洞與宿主星系的共同演化 (Co-evolution of Supermassive Black Holes and their Host Galaxies with Galaxy Mergers)
檔案	[Endnote RIS 格式] [Bibtex 格式] [相關文章] [文章引用] [完整記錄] [館藏目錄] 至系統瀏覽論文 (2024-8-1以後開放)
摘要(中)	星系合併對於星系演化是至關重要的過程，藉由階層式結構形成模型，星系的結構得以與宇宙學的理論連結，並且解釋碰撞星系能歷顯著的成長期，而星系中的超大質量黑洞也會同時演化，然而，合併事件往往需數億年來完成，我們無法觀測任意事件的完整細部過程，所以唯一能研究星系合併從開始到結束的物理細節是藉由數值模擬的方式；我們在美國國家科學研究計算中心的超級電腦上使用流體模擬程式--小精靈(GIZMO)進行模擬，它被認為可以適當地替複雜的星系交互作用與超大質量黑洞成長建立模型，其中模擬星系的物理參數來自觀測的結果（例如：蓋亞任務、阿塔卡瑪大型毫米及次毫米波陣列），利用如此的模擬並考慮不同的星系相關物理機制，我們可以研討超大質量黑洞與其宿主星系性質（像是核球、恆星形成率與氣體分佈等等）的共同演化。
摘要(英)	Galaxy mergers are crucial processes in galaxy evolution. They hold the key to connect the galactic structure to cosmology through the hierarchical structure formation, which explains that galaxy pairs undergoing a significant transitional stage, and the supermassive black holes (SMBHs) in the galaxies also evolve simultaneously. However, we cannot observe the entire process of any merger events, which take longer than a few billion years, so the only way to study the physics of galaxy mergers from beginning to the end is by utilizing numerical simulations. The hydrodynamics simulation code we used is called GIZMO, which is appropriate to model the processes of the complicated galaxy interactions and SMBH growth. We simulated galaxies with physical parameters based on the observational results (e.g. Gaia, ALMA) and run our simulations on powerful supercomputers at the National Energy Research Scientific Computing Center (NERSC) in the USA. By performing a suite of simulations with different physical conditions, we can investigate the co-evolution between SMBHs and their host galaxies for some properties such as bulge, star formation rate, gas distribution, and so on.
關鍵字(中)	★ 星系演化 ★ 計算天文物理 ★ 合併星系 ★ 超大質量黑洞 ★ 恆星形成 ★ 星際介質 ★ 星系核球 ★ 宇宙學	關鍵字(英)	★ Galaxy Evolution ★ Computational Astrophysics ★ Galaxy Merger ★ Supermassive Black Hole ★ Star Formation ★ Interstellar Medium ★ Galactic Bulge ★ Cosmology
論文目次	摘要v Abstract vi Contents vii 1 Introduction 1 2 Numerical Methods 4 2.1 GIZMO code . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 4 2.2 ISM and Stellar physics . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 5 2.3 Modeling the Supermassive Black Hole in Galaxy simulation . . . . . . . . . . . . . . . 6 2.3.1 The Growth of Black Hole . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 6 2.3.2 Feedbacks from SMBH . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 7 2.4 Initial Conditions . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 8 3 Results 11 3.1 Evolution of the SMBH . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 12 3.1.1 The Growth of the SMBH in an Isolated Galaxy . . . . . . . . . . . . . . . . . . . . . 12 3.1.2 Rapid Growth of SMBH with Major Merger . . . . . . . . . . . . . . . . . . . . . . . . . 14 3.2 Properties of Star Formation . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 15 3.2.1 SFRs in an Isolated Galaxy . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 15 3.2.2 Merger-driven Starburst . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 19 3.3 Bulge Evolution . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 22 3.3.1 The Bulge Growth with Minor Merger. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 25 4 Discussion 27 5 Conclusion 29 Bibliography 30
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指導教授	黃崇源陳科榮(Chorng-Yuan Hwang Ke-Jung Chen)	審核日期	2021-8-4
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