Dark energy perturbations revisited

被引:11
作者
Li, Mingzhe [1 ,4 ,5 ]
Cai, Yifu [2 ,6 ]
Li, Hong [2 ,5 ]
Brandenberger, Robert [3 ]
Zhang, Xinmin [2 ,5 ]
机构
[1] Nanjing Univ, Dept Phys, Nanjing 210093, Peoples R China
[2] Chinese Acad Sci, Inst High Energy Phys, Beijing 100049, Peoples R China
[3] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada
[4] Nanjing Univ, Purple Mt Observ, Joint Ctr Particle Nucl Phys & Cosmol, Nanjing 210093, Peoples R China
[5] Chinese Acad Sci, Theoret Phys Ctr Sci Facil, Beijing 100049, Peoples R China
[6] Arizona State Univ, Dept Phys, Tempe, AZ 85287 USA
基金
加拿大自然科学与工程研究理事会; 中国国家自然科学基金;
关键词
Dark energy; Cosmological perturbations; MICROWAVE BACKGROUND ANISOTROPIES; EQUATION-OF-STATE; COSMOLOGICAL CONSEQUENCES; CONSTRAINTS; SUPERNOVAE; COMPONENT; DYNAMICS; UNIVERSE;
D O I
10.1016/j.physletb.2011.06.061
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
In this Letter we study the evolution of cosmological perturbations in the presence of dynamical dark energy, and revisit the issue of dark energy perturbations. For a generally parameterized equation of state (EoS) such as w(D) (z) = w(0) + w(1) z/1+z (for a single fluid or a single scalar field), the dark energy perturbation diverges when its EoS crosses the cosmological constant boundary w(D) = -1. In this Letter we present a method of treating the dark energy perturbations during the crossing of the w(D) = -1 surface by imposing matching conditions which require the induced 3-metric on the hypersurface of w(D) = -1 and its extrinsic curvature to be continuous. These matching conditions have been used widely in the literature to study perturbations in various models of early universe physics, such as Inflation, the Pre-Big-Bang and Ekpyrotic scenarios, and bouncing cosmologies. In all of these cases the EoS undergoes a sudden change. Through a detailed analysis of the matching conditions, we show that delta(D) and theta(D) are continuous on the matching hypersurface. This justifies the method used (Zhao et al., 2005, 2007; Xia et al., 2006, 2008) [1-4] in the numerical calculation and data fitting for the determination of cosmological parameters. We discuss the conditions under which our analysis is applicable. (C) 2011 Elsevier B.V. All rights reserved.
引用
收藏
页码:5 / 11
页数:7
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