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| DC 欄位 | 值 | 語言 |
|---|---|---|
| dc.contributor.advisor | 鄭士康(Shyh-Kang Jeng),陳丕燊(Pisin Chen) | |
| dc.contributor.author | Yu-Hsiang Lin | en |
| dc.contributor.author | 林裕翔 | zh_TW |
| dc.date.accessioned | 2021-06-13T03:17:16Z | - |
| dc.date.available | 2011-08-01 | |
| dc.date.copyright | 2011-08-01 | |
| dc.date.issued | 2011 | |
| dc.date.submitted | 2011-07-29 | |
| dc.identifier.citation | [1] E. P. Hubble, Proc. Nat. Acad. Sci. 15, 168 (1929).
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| dc.identifier.uri | http://tdr.lib.ntu.edu.tw/jspui/handle/123456789/31674 | - |
| dc.description.abstract | 有許多文獻探討宇宙背景輻射的非等向性溫度分布中，l = 2模態的強度和理論預測相比異常偏低的問題。大部分的文獻都提出和標準暴漲模型不同的預測，認為宇宙初始能譜在大尺度的部分有截止的現象。我們研究一個在暴漲期之前具有一段物質主宰時期的早期宇宙模型，並且以第一原理進行計算，檢查這樣的截止現象是否存在。 | zh_TW |
| dc.description.abstract | The problem of quadrupole anomaly in the cosmic microwave background temperature anisotropy spectrum is treated in many works. Most of them provide scenarios different from the one of standard inflation and point to a cutoff of power in the primordial power spectrum at large scales. We study the scenario of the early universe with a pre-inflation matter era, and make an ab initio calculation to check the existence of the infrared cutoff. | en |
| dc.description.provenance | Made available in DSpace on 2021-06-13T03:17:16Z (GMT). No. of bitstreams: 1 ntu-100-R95942023-1.pdf: 1326034 bytes, checksum: 2b53eb9a9f5c80e89dfbf798dcfa4383 (MD5) Previous issue date: 2011 | en |
| dc.description.tableofcontents | Contents
口試委員會審定書........................................................................................i 誌謝..............................................................................................................ii 中文摘要......................................................................................................iv Abstract.......................................................................................................v Contents........................................................................................................vi List of Figures............................................................................................ix Chapter 1 Introduction…………………………………………………...1 1.1 The expanding universe..................................................... 1 1.2 The CMB anisotropy and the quadrupole anomaly…....... 4 1.3 Proposed explanations to the quadrupole anomaly............ 6 1.3.1 Different initial conditions…………………………7 1.3.2 Different potentials………………………...………8 1.3.3 Reconstruction from CMB data……………………9 1.4 The pre-inflation matter era: issues and solutions proposed in the thesis….................. 9 1.4.1 Issues in the calculation of the primordial spectrum…………………………………...……….9 1.4.2 Ab initio treatment proposed in the thesis………...12 1.5 Chapter outline…............................................................. 13 Chapter 2 The zero-order universe…….........................................….... 14 2.1 The scale factor in ΛCDM model.................................... 14 2.1.1 The Robertson-Walker metric…….………………14 2.1.2 The Friedmann equations…………………………15 2.1.3 The numerical solution…………………….……..19 2.2 The scale factor in inflation era…................................... 23 2.2.1 The horizon and flatness problems………….…....23 2.2.2 Inflation as a solution to the problems……………27 2.2.3 The scalar field formulation……………………....30 2.2.4 The Planck units…………………………………..33 Chapter 3 The cosmological perturbation theory in inflation era…... 35 3.1 The metric perturbations….............................................. 35 3.2 The infinitesimal transformations and the gauges………38 3.2.1 The infinitesimal transformation of coordinate and the metric perturbation…………………………....38 3.2.2 Eliminate the gauge degrees of freedom by choosing a gauge…………………………………..………...43 3.3 The perturbation of energy-momentum tensor................ 45 3.4 The perturbed Einstein equation….................................. 46 Chapter 4 Quantization of inflaton field under various scenarios…....48 4.1 The pure inflation scenario………………………..…….49 4.1.1 Quantization of the inflaton field at early times….49 4.1.2 Validity conditions of the approximation…...…….55 4.2 The pre-inflation matter era…………………………..…55 4.2.1 Quantization of the inflaton field at early times.…58 4.2.2 Validity conditions of the approximation……...….59 4.3 The power spectrum of the quantum fluctuations…….…60 Chapter 5 The primordial power spectra…........................................... 63 5.1 The pure inflation scenario…………………………...…63 5.1.1 The expansion of modes………………………….63 5.1.2 The time-evolution of the inflaton field and the metric perturbation………………………………..67 5.1.3 The primordial power spectra…………………….72 5.2 The results of the case with pre-inflation matter era…….74 5.2.1 The expansion of modes………………………….74 5.2.2 The time-evolution of the inflaton field and the metric perturbation…………………………..……80 5.2.3 The primordial power spectra…………………….83 Chapter 6 Conclusions…......................................................................... 86 References..................................................................................................87 List of Figures Chapter 1 Fig 1.1 The “Big Bang” model of the universe…………………………………….……2 Fig 1.2 The CMB temperature anisotropy spectrum………………………..…………...4 Fig 1.3 The composition of the universe……………………………………………….. 6 Chapter 2 Fig 2.1 The scale factor of ΛCDM model……………………………………………21 Fig 2.2 The scale factor of ΛCDM model, in log-log plot……………………….…..22 Fig 2.3 The power-law behavior of the scale factor of ΛCDM model………………22 Fig 2.4 The scale factor in the inflation era……………………………………….…32 Fig 2.5 The scalar field in inflation era…………………………………………..…..32 Fig 2.6 The time derivative of scalar field in inflation era……………………….….33 Fig 2.7 The time derivative of scalar field in inflation era, enlarged at the end of inflation………………………………………………………………..…….33 Chapter 5 Fig 5.1 The expansion of modes.…………………..…………………………..…….... 65 Fig 5.2 The time evolution of the inflaton field and the metric perturbation……..……68 Fig 5.3 The same plots as figure 5.2, for the mode whose physical wavelength is 1/10 to the size of the Hubble radius today……………………………………….……69 Fig 5.4 The same plots as figure 5.2, for the mode whose physical wavelength is 1/100 to the size of the Hubble radius today…………………………….……………69 Fig 5.5 The time evolution of R…………………………………………………….…..71 Fig. 5.6 The primordial power spectra of , , and ………………….………..74 Fig. 5.7 The expansion of modes, with pre-inflation matter era…………….…………76 Fig. 5.8 The expansion of modes………………………………………………………78 Fig. 5.9 The separate enlarged plots of the mode whose physical wavelength today is equal to the Hubble radius today…..…………………………………………79 Fig 5.10 The time evolutions of various fields………………………………………...81 Fig 5.11 The same plots as figure 5.10, for the mode whose physical wavelength is 1/10 to the size of the Hubble radius today…..……………………………………82 Fig 5.12 The same plots as figure 5.10, for the mode whose physical wavelength is 1/100 to the size of the Hubble radius today…..……………………………..83 Fig. 5.13 The primordial power spectra of , , and , in the case with pre-inflation matter era………………………………………………………85 | |
| dc.language.iso | zh-TW | |
| dc.title | 對於初始能譜長波段截止的研究 | zh_TW |
| dc.title | Ab initio investigation on the infrared cutoff of the primordial power spectrum | en |
| dc.type | Thesis | |
| dc.date.schoolyear | 99-2 | |
| dc.description.degree | 碩士 | |
| dc.contributor.oralexamcommittee | 吳俊輝 | |
| dc.subject.keyword | 宇宙學,初始能譜,宇宙背景輻射,暴漲,早期宇宙, | zh_TW |
| dc.subject.keyword | cosmology,primordial power spectrum,CMB,inflation,early universe, | en |
| dc.relation.page | 88 | |
| dc.rights.note | 有償授權 | |
| dc.date.accepted | 2011-07-29 | |
| dc.contributor.author-college | 電機資訊學院 | zh_TW |
| dc.contributor.author-dept | 電信工程學研究所 | zh_TW |
| 顯示於系所單位： | 電信工程學研究所 | |
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