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| DC 欄位 | 值 | 語言 |
|---|---|---|
| dc.contributor.advisor | 黃偉彥 | |
| dc.contributor.author | Tse-Chun Wang | en |
| dc.contributor.author | 王則鈞 | zh_TW |
| dc.date.accessioned | 2021-06-14T16:50:45Z | - |
| dc.date.available | 2011-08-16 | |
| dc.date.copyright | 2011-08-16 | |
| dc.date.issued | 2011 | |
| dc.date.submitted | 2011-08-12 | |
| dc.identifier.citation | Bibliography
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| dc.identifier.uri | http://tdr.lib.ntu.edu.tw/jspui/handle/123456789/40542 | - |
| dc.description.abstract | 我們探討f(R)重力修正理論下宇宙學微擾之演化,f(R)重力修正理論是一種可以解釋宇宙加速膨脹卻不使用暗能的重力理論。在一般計算出微擾f(R)宇宙中演化的方式，一般人不考慮早期針對重力理論修正,並以廣義相對論下的微擾演化作為其在f(R)重力理論下的近似 (廣相近似)。在此論文中，我們檢測廣相近似的可行性。並且，我們更進一步得提出對於早期宇宙學微擾較佳近似。對於晚期，我們考慮由物質所主宰的宇宙(the matter dominated universe)中，傅立葉波長遠小於視界面的微擾(the sub-horizon perturbations)；並且,我們利用Tsujikawa的近似或Cruz-Dombriz, Dobado 和 Maroto的近似去算這些微擾的晚期演化。我們比較由我們方法(使用我們的早期近似)及一般做法(使用廣相近似計算早期微擾演化)所得出物質密度的微擾及其能量譜。我們發現在很多例子中，使用不同方式所得到的結果之間的差異可以高達百分之四十。與觀測誤差的百分之十作比較後，我們認為一般所使用的廣相近似在這些例子中是可能是有問題的，並且我們也認為較好的計算f(R)重力理論下宇宙學微擾演化是必要的。 | zh_TW |
| dc.description.provenance | Made available in DSpace on 2021-06-14T16:50:45Z (GMT). No. of bitstreams: 1 ntu-100-R98222067-1.pdf: 1312812 bytes, checksum: 8a000211835cde43582a2e766af0a4da (MD5) Previous issue date: 2011 | en |
| dc.description.tableofcontents | 1 Introduction 9
1.1 The Accelerating Universe . . . . . . . . . . . . . . . . . . . . . . . 9 1.2 f(R) Modified Gravity . . . . . . . . . . . . . . . . . . . . . . . . . 10 1.3 The Cosmological Perturbations . . . . . . . . . . . . . . . . . . . . 12 1.4 The Evolution of the Cosmological Perturbations . . . . . . . . . . 13 2 Equations of Motion for the Perturbations in the f(R) Cosmology 15 2.1 Background Evolution . . . . . . . . . . . . . . . . . . . . . . . . . 15 2.2 The Evolution Equations of the Cosmological Perturbations . . . . 16 2.2.1 The Metric Perturbations and the Perturbed Field Equations 17 2.2.2 The Evolution Equations of the Metric Perturbations . . . . 18 2.2.3 The Stress-Energy Perturbations and the Evolution Equa- tions of the Stress-Energy Perturbations . . . . . . . . . . . 20 3 Calculating the Evolution of Perturbations in the f(R) Cosmology 23 3.1 Modified CMBFAST . . . . . . . . . . . . . . . . . . . . . . . . . . 24 3.1.1 The Framework of Modified CMBFAST . . . . . . . . . . . 24 33.2 A Conventional Method of Calculating the Evolution of the Pertur- bations in the f(R) Cosmology . . . . . . . . . . . . . . . . . . . . 26 3.3 The Two-Scale Problem . . . . . . . . . . . . . . . . . . . . . . . . 27 3.4 Our New Approximation for the Perturbations in the Early Universe 29 3.5 Two Approximations for Perturbations at Late Times . . . . . . . . 30 3.6 Summary of the Method to Solve Perturbations . . . . . . . . . . . 31 4 Results and Discussions 33 4.1 The Designer f(R) Model . . . . . . . . . . . . . . . . . . . . . . . 33 4.2 Compare Two Early-Time Approximations . . . . . . . . . . . . . . 35 4.2.1 Comparing the GR Early-Time Approximation and Ours . . 38 4.2.2 The Evolution of the Matter Energy Density Perturbations . 40 4.2.3 The Power Spectra of Matter Density Perturbation . . . . . 46 5 Summary 49 A The Numerical Tools 53 A.1 Modified CMBFAST with Our Approximation . . . . . . . . . . . . 53 A.2 The Tsujikawa Approximation Code . . . . . . . . . . . . . . . . . 63 A.3 The CDDM approximation code . . . . . . . . . . . . . . . . . . . . 67 Bibliography 71 | |
| dc.language.iso | en | |
| dc.subject | 宇宙學微擾 | zh_TW |
| dc.subject | 一般的計算f(R)宇宙學微擾演化方法 | zh_TW |
| dc.subject | f(R)重力修正理論 | zh_TW |
| dc.subject | 我們新的計算f(R)宇宙學微擾演化之方法 | zh_TW |
| dc.subject | cosmological perturbations | en |
| dc.subject | f(R) gravity | en |
| dc.subject | accelerating expansion of the universe | en |
| dc.subject | our method for calculating the evolution of the pertur- bations in f(R) gravity | en |
| dc.subject | the conventional method for calculating the evolution of the per- turbations in f(R) gravity | en |
| dc.title | f(R)宇宙之微擾 | zh_TW |
| dc.title | Perturbations in the f(R) Cosmology | en |
| dc.type | Thesis | |
| dc.date.schoolyear | 99-2 | |
| dc.description.degree | 碩士 | |
| dc.contributor.coadvisor | 顧哲安 | |
| dc.contributor.oralexamcommittee | 詹傳宗,李大興,張祥光,何俊麟 | |
| dc.subject.keyword | f(R)重力修正理論,宇宙學微擾,一般的計算f(R)宇宙學微擾演化方法,我們新的計算f(R)宇宙學微擾演化之方法, | zh_TW |
| dc.subject.keyword | accelerating expansion of the universe,f(R) gravity,cosmological perturbations,the conventional method for calculating the evolution of the per- turbations in f(R) gravity,our method for calculating the evolution of the pertur- bations in f(R) gravity, | en |
| dc.relation.page | 74 | |
| dc.rights.note | 有償授權 | |
| dc.date.accepted | 2011-08-12 | |
| dc.contributor.author-college | 理學院 | zh_TW |
| dc.contributor.author-dept | 物理研究所 | zh_TW |
| 顯示於系所單位： | 物理學系 | |
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