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Growth of Perturbations using Lambert$W$ Equation of State

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arxiv 2011.12058 v1 pith:FLMAQXWN submitted 2020-11-24 gr-qc

Manisha Banerjee , Sudipta Das , Abdulla Al Mamon , Subhajit Saha , Kazuharu Bamba This is my paper · ORCID
classification gr-qc
keywords lambertdarkenergygrowthmodelcomponentequationfunction
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abstract

Recently, a novel equation of state (EoS) parameter for dark energy has been introduced which deals with a special mathematical function, known as the Lambert$W$ function. In this paper, we study the effect on the growth of perturbations for the Lambert$W$ dark energy model. We perform the analysis for two different approaches. In the first case we consider the universe to be filled with two different fluid components, namely, the baryonic matter component and the Lambert$W$ dark energy component, while in the second case we consider that there is a single fluid component in the universe whose equation of state parameter is described by the Lambert$W$ function. We then compare the growth rates of Lambert$W$ model with that for a standard $\Lambda$CDM model as well as the CPL model. Our results indicate that the presence of Lambert$W$ dynamical dark energy sector changes the growth rate and affects the matter fluctuations in the universe to a great extent.

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  1. Analytic Integration of the Lambert W Cosmic Fluid Model H(z) Formula

    math-ph 2026-08 conditional novelty 4.0 of 10

    An exact analytic formula for ln(H(z)/H0) in the Lambert W cosmic fluid model, obtained by evaluating log-integral antiderivatives of the Lambert W function.

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