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| ???org.dspace.app.webui.jsptag.ItemTag.dcfield??? | Value | Language |
|---|---|---|
| dc.contributor.advisor | 薛熙于 | zh_TW |
| dc.contributor.advisor | Hsi-Yu Schive | en |
| dc.contributor.author | 李冠宏 | zh_TW |
| dc.contributor.author | Guan-Hong Li | en |
| dc.date.accessioned | 2023-06-14T16:20:09Z | - |
| dc.date.available | 2024-02-20 | - |
| dc.date.copyright | 2023-06-14 | - |
| dc.date.issued | 2023 | - |
| dc.date.submitted | 2023-02-20 | - |
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| dc.identifier.uri | http://tdr.lib.ntu.edu.tw/jspui/handle/123456789/87558 | - |
| dc.description.abstract | 本研究由超大質量黑洞提供動力，探討從梅歇爾-87 (M87) 星系核心出現的大型無線電噴流呈現出對稱的臨邊增光效應 (limb-brightening)。藉由考慮中央黑洞的吸積盤與黑洞磁層配置，我們探討了相應的 VLBI 觀測特徵，包括圖像和光譜，亦改進了僅由相對論性電漿在連接至黑洞的大尺度磁場之無重力模型(Force-free model)。我們發現，M87 之噴流的對稱性臨邊增光效應 (symmetrical limb-brightening) 需要擁有一個快速旋轉的黑洞，與之前的研究結果相似。這種性質是因為電漿沿著噴流內大尺度磁場運動與為黑洞自旋函數的光柱 (light cylinder)的位置密切相關。我們亦證明了在噴流中具有非軸對稱質量負載 (mass loading) 的情況下，可以在距黑洞不同距離處改變 M87 噴流邊緣的較亮側。 | zh_TW |
| dc.description.abstract | Powered by a supermassive black hole, the large-scale radio jet emerging from the core of the Messier 87 (M87) galaxy exhibits a symmetric limb-brightened feature. Taking into account the accretion and black hole magnetosphere configurations of the central engine, we explore corresponding VLBI observational features, including images and spectra, with an improved force-free jet model which only consists of relativistic plasma motions along large-scale magnetic fields attached to the central black hole. It is found that the symmetric limb-brightening feature of the M87 jet requires a fast-spinning black hole, similar to previous studies. Such property is because the plasma motion along the large-scale magnetic field within the jet is closely related to the location of the light cylinder, which is a function of black hole spin. We also demonstrate that it is possible to vary the brighter side of the M87 jet limb at different distances from the black hole with non-axisymmetric mass loading in the jet. | en |
| dc.description.provenance | Submitted by admin ntu (admin@lib.ntu.edu.tw) on 2023-06-14T16:20:08Z No. of bitstreams: 0 | en |
| dc.description.provenance | Made available in DSpace on 2023-06-14T16:20:09Z (GMT). No. of bitstreams: 0 | en |
| dc.description.tableofcontents | Verification Letter from the Oral Examination Committee i
Acknowledgments iii 摘要 v Abstract vii Contents ix List of Figures xiii List of Tables xvii Chapter 1 Introduction 1 Chapter 2 Method - Jet Model 5 2.1 streamline function 5 2.2 Jet velocity 7 2.3 Angular velocity of the magnetic field 9 2.4 Validation of the directions of Magnetic Field and Velocity Field 9 2.5 The Relativistic Doppler Effect - Beaming Factor 10 2.6 Mass loading 12 2.7 Jet terminal Lorentz factor 12 Chapter 3 Method - Radiative Transfer 15 3.1 Radiative transfer equation 15 3.2 Energy distribution of a single power law 18 3.3 Properties of non-thermal Synchrotron radiation 18 3.4 Ray-tracing Algorithm 19 Chapter 4 Imaging blurring due to finite beam size 21 4.1 Radio observation with Interferometry 21 4.2 Imaging blurring with non-circular gaussian beam 23 Chapter 5 Result and Discussion 29 5.1 Initial model A and fiducial model B 29 5.2 Validation 30 5.2.1 Model parameters in initial model A 30 5.2.2 Quantities and images of initial model A 31 5.2.3 Effects of free parameters adjustments in initial model A 35 5.2.3.1 emission - the jet shape index and the energy spectral index 35 5.2.3.2 mass loading - different injection location 35 5.3 Results 37 5.3.1 Model assumptions of fiducial model B 37 5.3.2 Model parameters in our fiducial model B 37 5.3.3 Quantities and Images in fiducial model B 38 5.3.3.1 Image at 43 GHz 39 5.3.3.2 Image at 86 GHz 40 5.3.4 Spectral Energy distribution (SED) 41 5.3.5 Comparisons between initial model A and fiducial model B 43 5.4 Discussion I: effect of black hole spin on the jet limb brightening 46 5.5 Discussion II: Non-axisymmetric mass loading 48 Chapter 6 Summary 53 References 55 Appendix A — Force-free model 63 A.1 Newtonian method for solving specific shape index 63 A.2 Different Inclination angles of viewing the jet 64 Appendix B — 5th ordered Runge-Kutta method 67 B.1 5th ordered Runge-Kutta Method 67 | - |
| dc.language.iso | en | - |
| dc.title | 模擬梅歇爾-87(Messier 87)中心快速旋轉黑洞之無線電噴流 | zh_TW |
| dc.title | Modeling M87 Radio Jet with a Fast-Spinning Black Hole | en |
| dc.type | Thesis | - |
| dc.date.schoolyear | 111-1 | - |
| dc.description.degree | 碩士 | - |
| dc.contributor.coadvisor | 卜宏毅 | zh_TW |
| dc.contributor.coadvisor | Hung-Yi Pu | en |
| dc.contributor.oralexamcommittee | 淺田圭一 | zh_TW |
| dc.contributor.oralexamcommittee | Keiichi Asada | en |
| dc.subject.keyword | 梅歇爾 87,黑洞,相對論性噴流,光線追蹤,輻射轉移, | zh_TW |
| dc.subject.keyword | M87,black hole,relativstic jet,ray-tracing,radiative transfer, | en |
| dc.relation.page | 72 | - |
| dc.identifier.doi | 10.6342/NTU202300524 | - |
| dc.rights.note | 同意授權(全球公開) | - |
| dc.date.accepted | 2023-02-20 | - |
| dc.contributor.author-college | 理學院 | - |
| dc.contributor.author-dept | 天文物理研究所 | - |
| dc.date.embargo-lift | 2024-02-20 | - |
| Appears in Collections: | 天文物理研究所 | |
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