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| DC 欄位 | 值 | 語言 |
|---|---|---|
| dc.contributor.advisor | 吳俊輝(Jiun-Huei Proty Wu) | |
| dc.contributor.author | Yu-Chiung Lin | en |
| dc.contributor.author | 林祐群 | zh_TW |
| dc.date.accessioned | 2021-06-15T11:21:44Z | - |
| dc.date.available | 2019-08-26 | |
| dc.date.copyright | 2016-08-26 | |
| dc.date.issued | 2016 | |
| dc.date.submitted | 2016-08-18 | |
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Astrophys. J., 651:142, 2006. | |
| dc.identifier.uri | http://tdr.lib.ntu.edu.tw/jspui/handle/123456789/49274 | - |
| dc.description.abstract | 我們使用 Pablo A. Rosado 的方法來計算來自雙星系統與旋轉中子星的重力波背景的譜函數，並且使用最近得到的模型與宇宙參數。Rosado 的重疊函數能夠顯示出重力波背景的可解析性與連續性。將我們計算出的不可解析背景和連續背景與觀測實驗的遺棄的靈敏度曲線做比較，我們可以得知該觀測實驗能探測到何種目標的重力波，以及是否會受到不可解析訊號的汙染。從我們的結果可以得知地面探測器不會受到來自雙星系統與旋轉中子星的不可解析背景的干擾。 | zh_TW |
| dc.description.abstract | We calculated the gravitational wave background from binary systems and rotating neutron stars using Pablo A. Rosado’s recipes of calculating spectral functions with the latest models and cosmological parameters. The overlap functions in Rosado’s works can characterize the resolvability and continuity of the background. Compare the predicted unresolvable and continuous gravitational wave backgrounds to the sensitivity curves of gravitational wave detectors, we can know from which target the background can be detected by the current and planned detectors, and whether the detector would be contaminate by the unresolvable signals. Our results show that the ground-based detectors are free
from the unresolvable backgrounds both from binary systems and rotating neutron stars. | en |
| dc.description.provenance | Made available in DSpace on 2021-06-15T11:21:44Z (GMT). No. of bitstreams: 1 ntu-105-R03244005-1.pdf: 4545568 bytes, checksum: 88f8fb696d986bf05ab6305466656435 (MD5) Previous issue date: 2016 | en |
| dc.description.tableofcontents | 口試委員會審定書 i
致謝 ii 中文摘要 iii Abstract iv Contents v List of Figures vii List of Tables ix 1 Introduction 1 2 Gravitational-Wave Background 4 2.1 Cosmological model . . . . . . . . . . . . . . . . . . . . . . . . . . . . 4 2.2 Spectral function . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 7 2.3 Resolvability of the background . . . . . . . . . . . . . . . . . . . . . . 10 2.4 Continuity of the background . . . . . . . . . . . . . . . . . . . . . . . . 13 3 Models For The Ensembles: Binaries 14 3.1 Stellar binaries . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 15 3.1.1 Energy spectrum . . . . . . . . . . . . . . . . . . . . . . . . . . 15 3.1.2 Time interval of emission in a frequency bin . . . . . . . . . . . 15 v3.1.3 Maximum and minimum frequencies . . . . . . . . . . . . . . . 16 3.1.4 Coalescence rate . . . . . . . . . . . . . . . . . . . . . . . . . . 17 3.1.5 Overlap function . . . . . . . . . . . . . . . . . . . . . . . . . . 19 3.1.6 Spectral function for stellar binary systems . . . . . . . . . . . . 20 3.1.7 Mass range . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 21 3.2 Massive black hole binaries . . . . . . . . . . . . . . . . . . . . . . . . . 23 4 Models For The Ensembles: Rotating Neutron Stars 26 4.1 Spectral function and overlap function . . . . . . . . . . . . . . . . . . . 26 4.2 Model for the ensemble of rotating neutron stars . . . . . . . . . . . . . . 31 4.2.1 Neutron star model . . . . . . . . . . . . . . . . . . . . . . . . . 31 4.2.2 Formation rate of neutron stars . . . . . . . . . . . . . . . . . . . 33 4.2.3 Energy evolution . . . . . . . . . . . . . . . . . . . . . . . . . . 34 4.2.4 Magnetic field and ellipticity distributions . . . . . . . . . . . . . 36 5 Results 38 5.1 Total backgrounds . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 38 5.2 Unresolvable backgrounds and the prospects of detection . . . . . . . . . 40 5.3 Continuous backgrounds . . . . . . . . . . . . . . . . . . . . . . . . . . 42 5.4 Backgrounds from each source . . . . . . . . . . . . . . . . . . . . . . . 42 5.5 Comparison with previous works . . . . . . . . . . . . . . . . . . . . . . 43 5.5.1 Compare to Rosado’s works . . . . . . . . . . . . . . . . . . . . 43 5.5.2 The unresolvable background . . . . . . . . . . . . . . . . . . . 44 6 Conclusion 49 Bibliography 50 | |
| dc.language.iso | en | |
| dc.subject | 靈敏度曲線 | zh_TW |
| dc.subject | 重力波 | zh_TW |
| dc.subject | 雙星系統 | zh_TW |
| dc.subject | 中子星 | zh_TW |
| dc.subject | 譜函數 | zh_TW |
| dc.subject | 重疊函數 | zh_TW |
| dc.subject | 可解析性 | zh_TW |
| dc.subject | 連續性 | zh_TW |
| dc.subject | spectral function | en |
| dc.subject | sensitivity curve | en |
| dc.subject | continuity | en |
| dc.subject | resolvability | en |
| dc.subject | Gravitational waves | en |
| dc.subject | binary system | en |
| dc.subject | neutron star | en |
| dc.subject | overlap function | en |
| dc.title | 雙星系統與旋轉中子星的重力波背景預測 | zh_TW |
| dc.title | Gravitational Waves Predicted from Stellar Binaries and Rotating Neutron Stars | en |
| dc.type | Thesis | |
| dc.date.schoolyear | 104-2 | |
| dc.description.degree | 碩士 | |
| dc.contributor.oralexamcommittee | 黃崇源(Chorng-Yuan Hwang),吳建宏 | |
| dc.subject.keyword | 重力波,雙星系統,中子星,譜函數,重疊函數,可解析性,連續性,靈敏度曲線, | zh_TW |
| dc.subject.keyword | Gravitational waves,binary system,neutron star,spectral function,overlap function,resolvability,continuity,sensitivity curve, | en |
| dc.relation.page | 55 | |
| dc.identifier.doi | 10.6342/NTU201602659 | |
| dc.rights.note | 有償授權 | |
| dc.date.accepted | 2016-08-19 | |
| dc.contributor.author-college | 理學院 | zh_TW |
| dc.contributor.author-dept | 天文物理研究所 | zh_TW |
| 顯示於系所單位： | 天文物理研究所 | |
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