Thermodynamics of Homogeneous and Isotropic Universe for Various Dark Energy Conditions

doi:10.26565/2312-4334-2025-1-04

Neeru Goyal Department of Applied Sciences, The NorthCap University, Gurugram, India https://orcid.org/0009-0007-0283-0584
Anil Kumar Yadav Department of Physics, United College of Engineering and Research, Greater Noida, India https://orcid.org/0000-0002-5174-5542
Tensubam Alexander Singh Department of Mathematical Sciences, Bodoland University, Kokrajhar, Assam, India https://orcid.org/0000-0003-2968-9350
Aditya Sharma Ghrera Department of Applied Sciences, The NorthCap University, Gurugram, India https://orcid.org/0000-0002-2715-5390
Asem Jotin Meitei Department of Mathematics, Pravabati College, Mayang Imphal-795132, Manipur, India; Department of Mathematics, Manipur University, Canchipur, Imphal, Manipur, India https://orcid.org/0000-0003-3384-5264
Kangujam Priyokumar Singh Department of Mathematics, Manipur University, Canchipur, Imphal, Manipur, India https://orcid.org/0000-0002-8784-4091

DOI: https://doi.org/10.26565/2312-4334-2025-1-04

Keywords: FRW Model, Homogeneous, Thermodynamics, Pantheon, Dark energy

Abstract

The thermodynamic properties of homogeneous and isotropic universe for various dark energy conditions with decaying cosmological term Λ(t) are investigated. To obtain the explicit solution of Einstein’s field equations, we have considered a linearly varying deceleration parameter in the form of q =-αt + m - 1 with α and m as scalar constants. We have constrained the model parameters H₀ and m as 68.495 km/s/Mpc and 1.591 respectively by bounding the derived model with combined pantheon compilation of SN Ia and H(z) data sets. Furthermore, we have studied the time varying dark energy states for two different assumptions i) Λ = Λ₁t^-2 and ii) Λ ꭀ [R(t)]⁻²ⁿ. For a specific assumption, our models indicate a dark energy like behaviour in in open, flat and closed space - time geometry. The temperature and entropy density of the model remain positive for both the cases i) Λ = Λ₁t^-2 and ii) Λ ꭀ [R(t)]⁻²ⁿ. Some physical properties of the universe are also discussed.

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