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http://tdr.lib.ntu.edu.tw/jspui/handle/123456789/34666完整後設資料紀錄
| DC 欄位 | 值 | 語言 |
|---|---|---|
| dc.contributor.advisor | 黃偉彥(W-Y. P. Hwang) | |
| dc.contributor.author | Chia-Hsun Chuang | en |
| dc.contributor.author | 莊家勛 | zh_TW |
| dc.date.accessioned | 2021-06-13T06:21:23Z | - |
| dc.date.available | 2006-02-07 | |
| dc.date.copyright | 2006-02-07 | |
| dc.date.issued | 2006 | |
| dc.date.submitted | 2006-01-24 | |
| dc.identifier.citation | [1] S. Perlmutter et al. [Supernova Cosmology Project Collaboration], Astro-
phys. J. 517, 565 (1999) [arXiv:astro-ph/9812133]. [2] A. G. Riess et al. [Supernova Search Team Collaboration], Astron. J. 116, 1009 (1998) [arXiv:astro-ph/9805201]. [3] J. L. Tonry et al. [Supernova Search Team Collaboration], Astrophys. J. 594, 1 (2003) [arXiv:astro-ph/0305008]. [4] R. A. Knop et al. [The Supernova Cosmology Project Collaboration], As- trophys. J. 598, 102 (2003) [arXiv:astro-ph/0309368]. [5] B. J. Barris et al., Astrophys. J. 602, 571 (2004) [arXiv:astro-ph/0310843]. [6] A. G. Riess et al. [Supernova Search Team Collaboration], Astrophys. J. 607, 665 (2004) [arXiv:astro-ph/0402512]. [7] C. L. Bennett et al., Astrophys. J. Suppl. 148, 1 (2003) [arXiv:astro- ph/0302207]; D. N. Spergel et al. [WMAP Collaboration], Astrophys. J. Suppl. 148, 175 (2003) [arXiv:astro-ph/0302209]. [8] T. Buchert, Gen. Rel. Grav. 9, 306 (2000) [arXiv:gr-qc/0001056]. [9] H. Iguchi, T. Nakamura and K. i. Nakao, Prog. Theor. Phys. 108, 809 (2002) [arXiv:astro-ph/0112419]. 41 42 BIBLIOGRAPHY [10] D. J. Schwarz, arXiv:astro-ph/0209584. [11] S. Rasanen, JCAP 0402, 003 (2004) [arXiv:astro-ph/0311257]. [12] S. Rasanen, JCAP 0411, 010 (2004) [arXiv:gr-qc/0408097]. [13] E. W. Kolb, S. Matarrese, A. Notari and A. Riotto, Phys. Rev. D 71, 023524 (2005) [arXiv:hep-ph/0409038]. [14] E. Barausse, S. Matarrese and A. Riotto, Phys. Rev. D 71, 063537 (2005) [arXiv:astro-ph/0501152]. [15] E. W. Kolb, S. Matarrese, A. Notari and A. Riotto, arXiv:hep-th/0503117. [16] A. Notari, arXiv:astro-ph/0503715. [17] S. Rasanen, arXiv:astro-ph/0504005. [18] E. W. Kolb, S. Matarrese and A. Riotto, arXiv:astro-ph/0506534. [19] E. E. Flanagan, Phys. Rev. D 71, 103521 (2005) [arXiv:hep-th/0503202]. [20] C. M. Hirata and U. Seljak, Phys. Rev. D 72, 083501 (2005) [arXiv:astro- ph/0503582]. [21] M. Giovannini, arXiv:hep-th/0505222. [22] H. Alnes, M. Amarzguioui and O. Gron, arXiv:astro-ph/0506449. [23] G. Lemaitre, Annales Soc. Sci. Brux. Ser. I Sci. Math. Astron. Phys. A 53, 51 (1933). [24] R. C. Tolman, Proc. Nat. Acad. Sci. 20, 169 (1934). [25] H. Bondi, Mon. Not. Roy. Astron. Soc. 107, 410 (1947). [26] D. Palle, Nuovo Cim. 117B, 687 (2002) [arXiv:astro-ph/0205462]. BIBLIOGRAPHY 43 [27] Y. Nambu and M. Tanimoto, arXiv:gr-qc/0507057. | |
| dc.identifier.uri | http://tdr.lib.ntu.edu.tw/jspui/handle/123456789/34666 | - |
| dc.description.abstract | 一般認為，如果宇宙中只存在產生吸引力的物質或能量，那麼宇宙必然只會減速膨脹。為了檢驗這個概念，我們在一個用來描述球對稱的塵埃流體的精確解中(Lemaitre-Tolman-Bondi solution)，找出了反例。因此，這個概念其實是令人懷疑的。對於宇宙的不均勻性，我們應該更深入的研究。這些例子，開啟一個新的角度去了解我們宇宙的演化。 | zh_TW |
| dc.description.abstract | It is the common consensus that the expansion of a universe always
slows down if the gravity provided by the energy sources therein is universally attractive. To examine this point we find counter-examples for the spherically symmetric dust fluid described by the Lemaitre-Tolman-Bondi solution. Thus, the validity of this naive consensus is indeed doubtful and the effects of inhomogeneities should be restudied. The example opens a new perspective for understanding the evolution of our universe. | en |
| dc.description.provenance | Made available in DSpace on 2021-06-13T06:21:23Z (GMT). No. of bitstreams: 1 ntu-95-R92222016-1.pdf: 478466 bytes, checksum: bd825db3a334832e6772befc1131dc2a (MD5) Previous issue date: 2006 | en |
| dc.description.tableofcontents | 1 Introduction 7
2 De‾nitions of Acceleration 11 2.1 Define Line Acceleration. . . . . . . . . . .11 2.2 Define Domain Acceleration . . . . . . . . .12 2.3 The Constraint of the Domain Acceleration . .13 3 Lemaitre-Tolman-Bondi (LTB) Solution 17 3.1 Basic of the LTB solution . . . . . . . . . .17 3.2 Constraints for the LTB Solution . . . . . . 19 4 Line Acceleration induced by Inhomogeneities . 21 4.1 When E(r) is a Constant . . . . . . . . . . .22 4.2 When E(r) is not a Constant . . . . . . . . .22 5 Domain Acceleration induced by Inhomogeneities 27 5.1 Domain Acceleration with tb(r) = 0 . . . . . 27 5.1.1 Previous Example . . . . . . . . . . . . . 27 5.1.2 Showing the Previous Example is Wrong . . .29 5.2 Domain Acceleration with tb(r) 6= 0 . . . . .30 6 Summary and Prospect 39 | |
| dc.language.iso | en | |
| dc.subject | 加速膨脹 | zh_TW |
| dc.subject | 不均勻 | zh_TW |
| dc.subject | 黑暗能量 | zh_TW |
| dc.subject | inhomogeneity | en |
| dc.subject | dark energy | en |
| dc.subject | inhomogeneities | en |
| dc.subject | cosmic acceleration | en |
| dc.title | 在塵埃宇宙中，不均勻性導致宇宙加速膨脹之探索 | zh_TW |
| dc.title | Inhomogeneity-Induced Cosmic Acceleration in a Dust Universe | en |
| dc.type | Thesis | |
| dc.date.schoolyear | 94-1 | |
| dc.description.degree | 碩士 | |
| dc.contributor.oralexamcommittee | 吳建宏,林文隆(W. Lin),陳丕燊(Pisin Chen),賀曾樸(Paul Ho),賀培銘(Pei-Ming Ho) | |
| dc.subject.keyword | 不均勻,黑暗能量,加速膨脹, | zh_TW |
| dc.subject.keyword | inhomogeneity,inhomogeneities,dark energy,cosmic acceleration, | en |
| dc.relation.page | 43 | |
| dc.rights.note | 有償授權 | |
| dc.date.accepted | 2006-01-25 | |
| 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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