THE EVOLUTION OF DENSITY PERTURBATIONS IN THE UNIVERSE

被引:38
作者
LYTH, DH
STEWART, ED
机构
[1] Department of Physics, University of Lancaster, Lancaster
关键词
Cosmic background radiation; Cosmology; Galaxies: clustering;
D O I
10.1086/169200
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
This paper deals with certain aspects of the evolution of energy density perturbations in the universe, using the fluid flow approach initiated by Hawking instead of the usual metric perturbation initiated by Lifshitz. The fluid flow approach is on the whole simpler and more physically transparent. From a practical viewpoint the present paper may be regarded as a derivation of certain bounds on the energy density during inflation, which is more or less self-contained as far as the evolution of the density perturbations is concerned. Follow-ing earlier work by Lyth and Mukherjee, the equation of Bardeen for the comoving gauge density pertur-bation is derived carefully, emphasizing the similarity with the nonrelativistic case. The calculation is then extended to the case of two uncoupled fluids, thus providing a derivation of the Kodama-Sasaki equation which keeps track of the separate density perturbations. Its application is considered, with special reference to the cold dark matter scenarios. The initial spectra of perturbations coming from inflation are specified, taking careful account of the epoch when the dark matter first appears, and the final spectrum of perturbations is deduced. Comparison with present observations of the microwave background anisotropy and of the galaxy correlation function provides limits on the energy density during inflation. Finally the comoving and synchronous perturbations are related; it is proved that they become equal after matter domination and are related in a scale-independent way at early times, facts which were assumed in making the comparison with observation.
引用
收藏
页码:343 / 353
页数:11
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