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| DC 欄位 | 值 | 語言 |
|---|---|---|
| dc.contributor.advisor | 朱有花 | |
| dc.contributor.author | Un-Pang Chang | en |
| dc.contributor.author | 曾遠鵬 | zh_TW |
| dc.date.accessioned | 2021-06-17T02:29:10Z | - |
| dc.date.available | 2017-08-25 | |
| dc.date.copyright | 2017-08-25 | |
| dc.date.issued | 2017 | |
| dc.date.submitted | 2017-08-17 | |
| dc.identifier.citation | (1) Arbutina, B., & Urošević, D. 2005, MNRAS, 360, 76
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| dc.identifier.uri | http://tdr.lib.ntu.edu.tw/jspui/handle/123456789/68653 | - |
| dc.description.abstract | 關於大麥哲倫星雲（LMC）中的超新星殘骸（SNRs）的最近研究顯示，X射線光度與殘骸大小之間，存在有趣的關係。大小相近的核塌縮（CC）超新星殘骸會有截然不同的光度。我們想瞭解箇中原因。故此，我們提出假說：高X射線發射產生在高密度地帶，而低發射則在低密度處。X射線與Hα發射率皆為氣體的溫度與密度函數，但它們的函數形式並不相同。我們使用X射線與Hα表面亮度去考察殘骸的物理環境，並探究X射線光度與大小關係的原由。 | zh_TW |
| dc.description.abstract | Recent study about the supernova remnants (SNRs) in the Large Magellanic Cloud (LMC) shows that there is an interesting relationship between the X-ray luminosity and the size of the SNRs. Core-collapse (CC) SNRs of similar sizes may have distinct magnitudes of luminosity. We want to figure out the reason. Thus, we speculate that high X-ray emission is produced in a high ambient density, whereas low X-ray emission in a low one. Both X-ray and Hα emissivities are functions of temperature and density of the emitting gas, but the functions of form are different. We use X-ray and Hα surface brightnesses to examine the physical conditions of the SNRs and investigate the origin of the X-ray luminosity and size relationship. | en |
| dc.description.provenance | Made available in DSpace on 2021-06-17T02:29:10Z (GMT). No. of bitstreams: 1 ntu-106-R02244001-1.pdf: 1862290 bytes, checksum: 3106eaaba5f7467e4806704437400e09 (MD5) Previous issue date: 2017 | en |
| dc.description.tableofcontents | 口試委員會審定書 ...i
誌謝 ...ii 中文摘要 ...iii Abstract ...iv Contents ...v List of Figures ...vii List of Tables ...ix Chapter 1. Introduction ...1 Chapter 2. Hα and X-ray Emissions ...9 Chapter 3. Calibration between MCELS and HST Data ...11 Chapter 4. X-ray-bright SNRs ...13 Chapter 5. First Trial Plot ...24 Chapter 6. Densities from Leahy (2017) ...26 Chapter 7. Lx-ne graph and 4 discrepancies on it ...29 Chapter 8. Summary and Conclusion ...34 Reference ...36 Appendix I. Calibration between MCELS and HST Data ...37 Appendix II. SB, R, ΔR, Lpc and the rms densities ...41 Appendix III. Relative position of the HII region N159 and the SNR J0540−6944 ...45 | |
| dc.language.iso | en | |
| dc.subject | 周邊密度 | zh_TW |
| dc.subject | 核塌縮超新星殘骸 | zh_TW |
| dc.subject | Hα發射 | zh_TW |
| dc.subject | X射線光度 | zh_TW |
| dc.subject | 大麥哲倫星雲 | zh_TW |
| dc.subject | X-ray luminosity | en |
| dc.subject | Hα emission | en |
| dc.subject | Large Magellanic Cloud | en |
| dc.subject | core-collapse supernova remnants | en |
| dc.subject | ambient density | en |
| dc.title | 瞭解超新星殘骸的X射線光度與大小之關係 | zh_TW |
| dc.title | Understanding the X-ray Luminosity-Size
Relationship of Supernova Remnants | en |
| dc.type | Thesis | |
| dc.date.schoolyear | 105-2 | |
| dc.description.degree | 碩士 | |
| dc.contributor.oralexamcommittee | 王名儒,林俐暉,陳林文 | |
| dc.subject.keyword | 核塌縮超新星殘骸,大麥哲倫星雲,周邊密度,X射線光度,Hα發射, | zh_TW |
| dc.subject.keyword | core-collapse supernova remnants,Large Magellanic Cloud,ambient density,X-ray luminosity,Hα emission, | en |
| dc.relation.page | 46 | |
| dc.identifier.doi | 10.6342/NTU201703854 | |
| dc.rights.note | 有償授權 | |
| dc.date.accepted | 2017-08-18 | |
| 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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