Holographic thermodynamic relation for dissipative and non-dissipative universes in a flat FLRW cosmology
arXiv:2408.11279 · doi:10.1140/epjc/s10052-025-13754-5
Abstract
To clarify a holographic modified thermodynamic relation, the present study applies a general formulation for cosmological equations in a flat FLRW universe to the first law of thermodynamics, using the Bekenstein-Hawking entropy and a dynamical Kodama-Hayward temperature . For the general formulation, both an effective pressure of cosmological fluids for dissipative universes (e.g., bulk viscous cosmology) and an extra driving term for non-dissipative universes (e.g., time-varying cosmology) are phenomenologically assumed. When is constant, the modified thermodynamic relation is equivalent to the formulation of the first law in standard cosmology. One side of this modified relation describes thermodynamic quantities in the bulk and can be divided into two time-derivative terms, namely and terms, where is the mass density of cosmological fluids and is the Hubble volume. Using the Gibbons-Hawking temperature , the other side of this relation, , can be formulated as the sum of and , which are equivalent to the and terms, respectively, with the magnitude of the term being proportional to the square of the term. In addition, the modified thermodynamic relation for constant is examined by applying the equipartition law of energy on the horizon. This modified thermodynamic relation reduces to a kind of extended holographic-like connection when a constant universe is considered. The evolution of thermodynamic quantities is also discussed, using a constant model, extending a previous analysis [Phys. Rev. D 108, 083515 (2023) (arXiv:2306.11285)].
Several paragraphs and references are added. [17 pages, 3 figures]
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