Decaying vacuum and evolution from early inflation to late acceleration

被引：0

作者：

Sarath, N. ^{[1
]}

Mathew, Titus K. ^{[1
]}

机构：

[1] Cochin Univ Sci & Technol, Dept Phys, Kochi 682022, Kerala, India

来源：

MODERN PHYSICS LETTERS A | 2021年 / 36卷 / 23期

关键词：

Running vacuum; primordial perturbation wavelength; COSMOLOGICAL CONSTANT; ENERGY;

D O I：

10.1142/S0217732321501601

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Decaying vacuum models are a class of models that incorporate a time-dependent vacuum energy density that can explain the entire evolution of the universe in a unified framework. A general solution to the Friedmann equation is obtained by considering vacuum energy density as a function of the Hubble parameter. We have obtained the asymptotic solution by choosing the equation of state for matter, Omega(m) = 0 and radiation, Omega(gamma) = 1/3. Finite boundaries in the early and late de Sitter epoch are defined by considering the evolution of primordial perturbation wavelength. An epoch invariant number Nc determines the number of primordial perturbation modes that cross the Hubble radius during each epoch.

引用

页数：14

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