暗能量及其热力学性质的研究
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摘要
宇宙的加速膨胀是当代宇宙学的一个基本事实,它得到了来自Ia型超新星、宇宙微波背景辐射和基隆数字天宇测量以及宇宙大尺度等众多观测数据的证实,同时也成为宇宙学研究的一个重点和热点。对于当今宇宙加速膨胀的现象,一个得到普遍认同的解释是宇宙中均匀分布着一种称之为暗能量的特殊物质,它具有负压强,正是这种负压强推动了宇宙的加速膨胀。此外,也有修正的引力理论和额外维理论解释宇宙加速膨胀。
本文首先介绍了宇宙学的相关基础知识(第二章),内容包括宇宙学原理、标准宇宙学模型和暴涨宇宙学模型以及解释宇宙加速膨胀的几种常见暗能量模型和修正的引力理论。接着介绍了我们的主要研究工作(第三章到第五章)。首先我们研究了修正可变Chaplygin Gas模型以及相互作用的修正可变Chaplygin Gas模型的演化行为(第三章)。具体分析了模型中宇宙学参量：暗能量状态参量wde、各物质能量密度比Ωi以及减速因子q。此外,鉴于增长指标f与哈勃参数H(z)的结合可以提供探索暗能量的性质以及宇宙结构形成的重要信息,我们还讨论了修正可变Chaplygin Gas模型中增长指标f的演化特性。最后,介绍了甄别暗能量模型的Statefinder参数诊断法,并利月(?)Statefinder参数对相互作用的VMCG模型进行了诊断。
另一方面,宇宙在局域平衡下可以看作一个大的热力学系统,我们从热力学角度研究和探讨了暗能量的性质(第五章)。具体地,在参数化暗能量模型w=wo+w1(?),探讨表观视界和事件视界包络的宇宙中广义热力学定律是否成立；此外我们采用Markov Chain Monte Carlo方法,利用当前天文观测数据：SNIa超新星,重子声速振荡(BAO),观测的哈勃数据(OHD)以及宇宙微波背景辐射(CMB)限制了修正可变Chaplygin Gas模型的参数(第四章)。并利用这些限制参数值,探讨修正可变Chaplygin Gas模型中,表观视界、事件视界以及粒子视界包络的宇宙的广义热力学性质(第五章)。
最后我们给出本论文的结论与展望部分。
It has been confirmed that the expansion of our universe is accelerating at present, through numerous cosmological observations, such as the type Ⅰa Supernova, the cosmic microwave background anisotropy, the Sloan Digital Sky Survey and the large scale structure. Therefore, it has been one of the most important issues in the research of cosmology to explain the accelerating universe. Up to now, the popular explanation is that the present universe is dominated by an exotic component, dubbed dark energy, which is introduced to explain the accelerating expansion through negative pressure. In addition, modified gravity theories (f(R)) and higher-dimensional theories are also studied to interpret the accelerating universe.
A brief introduction of the background knowledge of cosmology are given at first (chapter1), which including the cosmological Principle, the standard cosmological model and the inflation cosmological model. Then we introduce some famous dark energy model and make some brief summary of their evolutions. Our work include in the chapters from3to5. Firstly we emphasized the evolution of Variable Modified Chaplygin Gas Model and the Variable Modified Chaplygin Gas Model with Interaction (chapter3). Specifically, the evolutions of related cosmological parameters such as the state parameter of dark energy wde, the fractional energy densities Ωi (i respectively denotes baryons, dark matter, dark energy), the deceleration parameter q. As the combination of the growth index f and the function H(z) can provide significant insight into the properties of dark energy and interpret the structure formation. We also discuss the growth index f in the VMCG model. Furthermore, the statefinder diagnostic is used to discuss the Variable Modified Chaplygin Gas Model with Interaction.
On the other hand, when local thermodynamic equilibrium, universe can be considered as a thermodynamical system. In a general independent dark energy model ω=ω0+ω1z(1+z)/(1+z2), we investigate the thermodynamical properties on the apparent horizon and event horizon (chapter5). In Chapter4, by adopting Markov Chain Monte Carlo method, Variable Modified Chaplygin Gas Model is constrained on the basis of the current observed data (SNIa, CMB, BAO, OHD). By using the mean values of parameters, we also studied the thermodynamical properties of the Variable Modified Chaplygin Gas Model (Chapter5) on the apparent horizon, event horizon and particle horizon respectively.
A conclusion is presented in the last section.
本文首先介绍了宇宙学的相关基础知识(第二章),内容包括宇宙学原理、标准宇宙学模型和暴涨宇宙学模型以及解释宇宙加速膨胀的几种常见暗能量模型和修正的引力理论。接着介绍了我们的主要研究工作(第三章到第五章)。首先我们研究了修正可变Chaplygin Gas模型以及相互作用的修正可变Chaplygin Gas模型的演化行为(第三章)。具体分析了模型中宇宙学参量：暗能量状态参量wde、各物质能量密度比Ωi以及减速因子q。此外,鉴于增长指标f与哈勃参数H(z)的结合可以提供探索暗能量的性质以及宇宙结构形成的重要信息,我们还讨论了修正可变Chaplygin Gas模型中增长指标f的演化特性。最后,介绍了甄别暗能量模型的Statefinder参数诊断法,并利月(?)Statefinder参数对相互作用的VMCG模型进行了诊断。
另一方面,宇宙在局域平衡下可以看作一个大的热力学系统,我们从热力学角度研究和探讨了暗能量的性质(第五章)。具体地,在参数化暗能量模型w=wo+w1(?),探讨表观视界和事件视界包络的宇宙中广义热力学定律是否成立；此外我们采用Markov Chain Monte Carlo方法,利用当前天文观测数据：SNIa超新星,重子声速振荡(BAO),观测的哈勃数据(OHD)以及宇宙微波背景辐射(CMB)限制了修正可变Chaplygin Gas模型的参数(第四章)。并利用这些限制参数值,探讨修正可变Chaplygin Gas模型中,表观视界、事件视界以及粒子视界包络的宇宙的广义热力学性质(第五章)。
最后我们给出本论文的结论与展望部分。
It has been confirmed that the expansion of our universe is accelerating at present, through numerous cosmological observations, such as the type Ⅰa Supernova, the cosmic microwave background anisotropy, the Sloan Digital Sky Survey and the large scale structure. Therefore, it has been one of the most important issues in the research of cosmology to explain the accelerating universe. Up to now, the popular explanation is that the present universe is dominated by an exotic component, dubbed dark energy, which is introduced to explain the accelerating expansion through negative pressure. In addition, modified gravity theories (f(R)) and higher-dimensional theories are also studied to interpret the accelerating universe.
A brief introduction of the background knowledge of cosmology are given at first (chapter1), which including the cosmological Principle, the standard cosmological model and the inflation cosmological model. Then we introduce some famous dark energy model and make some brief summary of their evolutions. Our work include in the chapters from3to5. Firstly we emphasized the evolution of Variable Modified Chaplygin Gas Model and the Variable Modified Chaplygin Gas Model with Interaction (chapter3). Specifically, the evolutions of related cosmological parameters such as the state parameter of dark energy wde, the fractional energy densities Ωi (i respectively denotes baryons, dark matter, dark energy), the deceleration parameter q. As the combination of the growth index f and the function H(z) can provide significant insight into the properties of dark energy and interpret the structure formation. We also discuss the growth index f in the VMCG model. Furthermore, the statefinder diagnostic is used to discuss the Variable Modified Chaplygin Gas Model with Interaction.
On the other hand, when local thermodynamic equilibrium, universe can be considered as a thermodynamical system. In a general independent dark energy model ω=ω0+ω1z(1+z)/(1+z2), we investigate the thermodynamical properties on the apparent horizon and event horizon (chapter5). In Chapter4, by adopting Markov Chain Monte Carlo method, Variable Modified Chaplygin Gas Model is constrained on the basis of the current observed data (SNIa, CMB, BAO, OHD). By using the mean values of parameters, we also studied the thermodynamical properties of the Variable Modified Chaplygin Gas Model (Chapter5) on the apparent horizon, event horizon and particle horizon respectively.
A conclusion is presented in the last section.
引文
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