發(fā)布時(shí)間：2018-02-12 08:22

  本文關(guān)鍵詞： 暗能量 宇宙學(xué) 加速膨脹 減速因子　出處：《寧波大學(xué)》2013年碩士論文　論文類型：學(xué)位論文

【摘要】：Ia型超新星觀測(SNIa)，重子聲學(xué)振蕩(BAO)和微波背景輻射(CMB)等天文觀測表明我們的宇宙正處在一個(gè)加速膨脹的階段。通常，人們認(rèn)為宇宙中存在一種具有負(fù)壓的暗能量從而導(dǎo)致了宇宙今天的加速膨脹。現(xiàn)有絕大部分暗能量模型都支持宇宙加速度應(yīng)該還處在一個(gè)持續(xù)增大的階段。利用低紅移的SNIa和BAO觀測數(shù)據(jù)以及CPL參數(shù)化模型，人們發(fā)現(xiàn)宇宙膨脹加速度很可能在過去不久已進(jìn)入了減小階段。一旦加入高紅移的CMB數(shù)據(jù)，觀測仍支持宇宙膨脹加速度在增大。這就表明低紅移數(shù)據(jù)(SNIa和BAO)與高紅移(CMB)數(shù)據(jù)可能存在某些不相容性。如果將曲率因子k作為一個(gè)自由參數(shù)，SNIa+BAO觀測數(shù)據(jù)和SNIa+BAO+CMB觀測數(shù)據(jù)將都支持宇宙膨脹加速度可能進(jìn)入減小階段。因此，曲率因子k有效的緩解了低紅移數(shù)據(jù)與高紅移數(shù)據(jù)之間的不相容問題。 本文根據(jù)MCMC方法和CPL參數(shù)化模型，利用最新的觀測數(shù)據(jù)重新探討了宇宙減速因子的演化情況。觀測數(shù)據(jù)包括來自Union2的超新星數(shù)據(jù),來自WMAP7的CMB數(shù)據(jù),以及來自4個(gè)不同的BAO項(xiàng)目的BAO數(shù)據(jù)。四個(gè)BAO項(xiàng)目分別來是6度視場星系巡天項(xiàng)目,斯隆數(shù)字巡天結(jié)合2度視場星系紅移巡天的項(xiàng)目,Wigglez暗能量測量項(xiàng)目和重子振蕩光譜測量項(xiàng)目。我們分別研究了減速因子在假定空間平坦和空間彎曲情形下的演化。當(dāng)只考慮超新星或者超新星加上重子聲學(xué)振蕩時(shí),除了來自WiggleZ暗能量測量項(xiàng)目的數(shù)據(jù)外,無論空間平坦還是空間彎曲,數(shù)據(jù)都支持宇宙現(xiàn)在膨脹的加速度是在減小，而當(dāng)微波背景輻射的數(shù)據(jù)被考慮進(jìn)去時(shí)，，結(jié)果則強(qiáng)烈的支持ΛCDM模型，而且宇宙膨脹的加速度仍然是在增大過程中。因此，最新數(shù)據(jù)表明考慮宇宙空間彎曲因素并不能有效的緩解SNIa+BAO與CMB數(shù)據(jù)之間的矛盾。
[Abstract]:Astronomical observations such as the Ia supernova observation, baryon acoustic oscillation (BAO) and microwave background radiation (CMB) indicate that our universe is at a stage of accelerating expansion. It is believed that there is a kind of dark energy with negative pressure in the universe, which leads to the accelerating expansion of the universe today. Most of the existing dark energy models support that the acceleration of the universe should be at a stage of continuous increase. Low-redshift SNIa and BAO observations and CPL parameterized models, It has been found that the expansion acceleration of the universe has probably entered a decreasing phase in the past few years. Once Gao Hong's CMB data are added, Observations still support an increase in the expansion acceleration of the universe. This suggests that there may be some incompatibility between the low redshift data (SNIa and AO) and the Gao Hong shift (CMBs) data. If the curvature factor k is taken as a free parameter, the SNIa BAO data and the SNIa may exist. The BAO CMB observations will all support the possibility that the expansion acceleration of the universe may enter a reduced phase. Curvature factor k effectively alleviates the incompatibility between low red shift data and Gao Hong shift data. Based on the MCMC method and the CPL parameterized model, the evolution of the cosmic deceleration factor is revisited with the latest observational data. The observed data include supernova data from Union2 and CMB data from WMAP7. And BAO data from four different BAO projects. The four BAO projects are the six Field of View Galaxy Survey Project. We study the evolution of the deceleration factor under the assumption of space flatness and spatial curvature, respectively, in conjunction with the Sloan Digital Sky Survey and the two dimensional field of view galaxies' red-shift survey projects, Wigglez dark energy measurement and baryon oscillatory spectral measurements, respectively. When only supernova or supernova is considered plus baryon acoustic oscillation, With the exception of data from the WiggleZ dark energy measurement project, whether the space is flat or curved, the data support that the expansion acceleration of the universe is now decreasing, and when the microwave background radiation data are taken into account, The results strongly support the CDM model, and the acceleration of cosmic expansion is still in the process of increasing. Therefore, the latest data show that considering space bending factors can not effectively alleviate the contradiction between SNIa BAO and CMB data.
【學(xué)位授予單位】：寧波大學(xué)
【學(xué)位級(jí)別】：碩士
【學(xué)位授予年份】：2013
【分類號(hào)】：P159

【共引文獻(xiàn)】

相關(guān)期刊論文 前10條

1 M.Sharif;Sehrish Azeem;;Dark Energy Models and Cosmic Acceleration with Anisotropic Universe in f(T) Gravity[J];Communications in Theoretical Physics;2014年04期

2 A.Sheykhi;H.Alavirad;A.Bagheri;E.Ebrahimi;;Quintessence Reconstruction of Interacting HDE in a Non-Flat Universe[J];Communications in Theoretical Physics;2014年06期

3 ZHANG JingFei;ZHAO LiAng;ZHANG Xin;;Revisiting the interacting model of new agegraphic dark energy[J];Science China(Physics,Mechanics & Astronomy);2014年02期

4 LU JianBo;CHEN LiDong;XU LiXin;LI TianQiang;;Comparing the VGCG model as the unification of dark sectors with observations[J];Science China(Physics,Mechanics & Astronomy);2014年04期

5 WU Juan;LI ZhengXiang;WU PuXun;YU HongWei;;Constrains on f(T) gravity with the strong gravitational lensing data[J];Science China(Physics,Mechanics & Astronomy);2014年05期

6 周挽平;;額外維空間中的三維球引力場[J];綿陽師范學(xué)院學(xué)報(bào);2014年02期

7 李微;李丹;;具有體積粘性的Chaplygin氣體作為統(tǒng)一的暗流體模型[J];渤海大學(xué)學(xué)報(bào)(自然科學(xué)版);2014年02期

8 Ming-Jian Zhang;Wen-Biao Liu;;Redshift drift reconstruction for some cosmological models from observations[J];Research in Astronomy and Astrophysics;2013年12期

9 Tian-Long Zu;Jie-Wen Chen;Yang Zhang;;A class of transient acceleration models consistent with Big Bang cosmology[J];Research in Astronomy and Astrophysics;2014年02期

10 Nejat T.Yilmaz;;Supergravity-induced interactions on thick branes[J];Chinese Physics B;2014年04期

相關(guān)博士學(xué)位論文 前2條

1 黃鵬;暗能量與f（T）引力相關(guān)問題研究[D];北京工業(yè)大學(xué);2013年

2 王鈺婷;暗能量的擾動(dòng)和積分的Sachs-Wolfe效應(yīng)[D];大連理工大學(xué);2013年

相關(guān)碩士學(xué)位論文 前10條

1 祁景釗;暗能量模型的甄別與動(dòng)力學(xué)研究[D];河北大學(xué);2013年

2 翟永佳;f（R）引力中黑洞的擬正則模[D];上海師范大學(xué);2013年

3 潘文劍;全息暗能量模型與宇宙空間演生現(xiàn)象的研究[D];南昌大學(xué);2013年

4 高原;修正的Chaplygin氣體作為非均勻暗能量對(duì)宇宙結(jié)構(gòu)形成的影響[D];遼寧師范大學(xué);2013年

5 張欣;Horava-Lifshitz引力理論的熱力學(xué)行為以及全息暗能量的熱力學(xué)描述[D];遼寧師范大學(xué);2013年

6 高健;關(guān)于Cardassian冪律模型在非平直宇宙中粘滯效應(yīng)對(duì)宇宙演化影響的研究[D];遼寧師范大學(xué);2013年

7 韓偉麗;關(guān)于加速膨脹宇宙中f（R）引力模型構(gòu)建的研究[D];遼寧師范大學(xué);2013年

8 林亮亮;關(guān)于f（R，L_m）引力理論及其相關(guān)問題的研究[D];遼寧師范大學(xué);2013年

9 蘇洋洋;MCG暗能量模型在球塌縮理論下對(duì)宇宙結(jié)構(gòu)形成的影響[D];遼寧師范大學(xué);2012年

10 孫小雨;關(guān)于廣義Hobbit模型的理論研究[D];遼寧師范大學(xué);2012年

本文編號(hào)：1505193