Within the non-interacting power-law holographic dark energy model, the Barrow and Tsallis parameters satisfy δ(2+Δ) = 4 − α(q0,j0), yielding δ ≈ 1.0–1.1 only after a prior on Δ is imposed.
Possible Generalization of Boltzmann-Gibbs Statistics
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Cosmographic Connection Between Cosmological And Planck Scales: The Barrow-Tsallis Entropy
Within the non-interacting power-law holographic dark energy model, the Barrow and Tsallis parameters satisfy δ(2+Δ) = 4 − α(q0,j0), yielding δ ≈ 1.0–1.1 only after a prior on Δ is imposed.