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| DC 欄位 | 值 | 語言 |
|---|---|---|
| dc.contributor.advisor | 賀培銘 | |
| dc.contributor.author | Shu-Jung Yang | en |
| dc.contributor.author | 楊書容 | zh_TW |
| dc.date.accessioned | 2021-05-19T18:05:05Z | - |
| dc.date.available | 2024-08-20 | |
| dc.date.available | 2021-05-19T18:05:05Z | - |
| dc.date.copyright | 2019-08-20 | |
| dc.date.issued | 2019 | |
| dc.date.submitted | 2019-08-16 | |
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| dc.identifier.uri | http://tdr.lib.ntu.edu.tw/jspui/handle/123456789/8064 | - |
| dc.description.abstract | 由Kawai、Matsuo及Yokokura所提出的KMY模型藉由計算半古典愛因斯坦方程得到自洽的黑洞演化，並發現此模型中之黑洞並不存在視界面（horizon）。 本論文主要藉由不同初始條件探討KMY模型中所有黑洞類型的可能性，透過數值模擬以及解析表述，我們發現有兩種黑洞類型，一是在KMY模型中已被提出的漸近黑洞類型(asymptotic black hole)，另一則是類薄殼黑洞(pseudo thin shell)。若塌縮物質的初始能量密度小於某臨界值，將形成漸近黑洞，反之則形成類薄殼黑洞。 | zh_TW |
| dc.description.abstract | By solving the semi-classical Einstein equation to get a self-consistent evolution process for black holes, the earlier work of Kawai, Matsuo and Yokokura introduced the notion of a black hole where there is no horizon. In this thesis, we use both numerical simulation and analytic expression to probe the possibility of other solutions to the semi-classical Einstein equation. We find that there are two types of solutions corresponding to different initial conditions. Whenever the initial energy density of the collapsing matter is smaller than a critical value, we arrive at an asymptotic black hole. We also derive the analytic expression for the second kind of black hole. They appear when the initial energy density is higher than the critical value, and they will be called pseudo thin shells. | en |
| dc.description.provenance | Made available in DSpace on 2021-05-19T18:05:05Z (GMT). No. of bitstreams: 1 ntu-108-R05222083-1.pdf: 1413794 bytes, checksum: 64a31e99c6d74be9185d3ec763b07aac (MD5) Previous issue date: 2019 | en |
| dc.description.tableofcontents | 1 Introduction 5
2 The Conventional Model Of Black Hole 9 2.1 Schwarzschild Metric 9 2.2 Hawking Radiation 10 2.3 Information Loss Paradox 13 3 The KMY Model 14 3.1 No Horizon In The KMY Model 20 3.2 Implication Of The KMY Model On Information Loss Paradox 21 4 Unphysicalness Of Ideal Thin Shell 22 4.1 Ideal Thin Shell 23 4.1.1 Constant Schwarzschild Radius 24 4.1.2 Shrinking Schwarzschild Radius 25 4.2 Pseudo-Thin Shell 26 4.3 Make Sense Of Thin Shells 30 5 The First Asymptotic States: Slope-1 Shell 33 5.1 Purpose Of Numerical Simulation 36 6 Numerical Simulation Setup 37 6.1 Each Discrete Shell As Pseudo-thin Shell 37 6.2 Removing Higher Derivatives 38 6.3 How To Interpret The Profile 40 6.4 Massive Core Inside The Collapsing Shells 42 7 Asymptotic States 44 7.1 a-r Graph In Static Background 44 7.2 a-r Graph in the KMY Model 47 7.3 Details Of The Profiles 52 7.4 Small Slope 52 7.5 Large Slope 55 8 Stability Of The Decaying Rate 58 9 Discussion and Conclusion 63 Bibliography 65 Appendix 69 | |
| dc.language.iso | en | |
| dc.title | KMY模型中的黑洞類型 | zh_TW |
| dc.title | Classification Of Black Holes In KMY Model | en |
| dc.type | Thesis | |
| dc.date.schoolyear | 107-2 | |
| dc.description.degree | 碩士 | |
| dc.contributor.oralexamcommittee | 黃宇廷,高賢忠 | |
| dc.subject.keyword | KMY模型,霍金輻射,反饋作用,半古典愛因斯坦方程,漸近黑洞類型, | zh_TW |
| dc.subject.keyword | the KMY model,Hawking radiation,back reaction,semi-classical Einstein equation,asymptotic black hole states, | en |
| dc.relation.page | 71 | |
| dc.identifier.doi | 10.6342/NTU201902989 | |
| dc.rights.note | 同意授權(全球公開) | |
| dc.date.accepted | 2019-08-16 | |
| 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 | 2024-08-20 | - |
| 顯示於系所單位： | 物理學系 | |
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| ntu-108-1.pdf | 1.38 MB | Adobe PDF | 檢視/開啟 |
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