Kaniadakis Holographic Dark Energy with Particle Horizon as IR Cutoff
Abstract
We construct a holographic dark-energy model using Kaniadakis entropy with the particle horizon as the infrared cutoff, consistently modifying both the holographic density and the Friedmann background. In standard Einstein gravity, noninteracting particle-horizon holographic dark energy (HDE) does not produce the sufficiently negative pressure required for late-time accelerated expansion. We show that the Kaniadakis deformation changes this behavior while the particle horizon is retained. For the representative parameter choice K=1.90×10−36, with ΩDE0=0.7 and c2=0.64, the deceleration parameter changes sign at z≃0.585 in the noninteracting case. Including the interaction strengths b2=0.03 and $0.06$ changes the transition only slightly, giving z≃0.586 and $0.589$, respectively. Thus, for the parameter set considered here, the interaction does not generate the acceleration; rather, the transition is already present in the noninteracting Kaniadakis model and the interaction produces only a small shift in its timing. We derive the autonomous evolution equations, the effective dark-energy equation of state, and the deceleration parameter. The adiabatic squared sound speed is also examined as a diagnostic of the effective-fluid stability, while statefinder variables are used to characterize deviations from ΛCDM. Finally, we verify that the K→0 limit continuously recovers standard Einstein-gravity particle-horizon HDE, for which the noninteracting model remains decelerating.
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BibTeX
@misc{asvar2026kaniadakis,
title = {{Kaniadakis Holographic Dark Energy with Particle Horizon as IR Cutoff}},
author = {A. Asvar and M. Mohammadi and A. Sheykhi},
howpublished = {arXiv},
year = {2026},
month = sep,
doi = {10.48550/arxiv.2609.10320},
eprint = {2609.10320},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2609.10320},
note = {CC BY 4.0},
}
RIS
TY - UNPB
TI - Kaniadakis Holographic Dark Energy with Particle Horizon as IR Cutoff
AU - A. Asvar
AU - M. Mohammadi
AU - A. Sheykhi
PY - 2026
DA - 2026/09/09
PB - arXiv
DO - 10.48550/arxiv.2609.10320
UR - https://arxiv.org/abs/2609.10320
AB - We construct a holographic dark-energy model using Kaniadakis entropy with the particle horizon as the infrared cutoff, consistently modifying both the holographic density and the Friedmann background. In standard Einstein gravity, noninteracting particle-horizon holographic dark energy (HDE) does not produce the sufficiently negative pressure required for late-time accelerated expansion. We show that the Kaniadakis deformation changes this behavior while the particle horizon is retained. For the representative parameter choice K=1.90×10^−36, with Ω_DE0=0.7 and c^2=0.64, the deceleration parameter changes sign at z≃0.585 in the noninteracting case. Including the interaction strengths b^2=0.03 and $0.06$ changes the transition only slightly, giving z≃0.586 and $0.589$, respectively. Thus, for the parameter set considered here, the interaction does not generate the acceleration; rather, the transition is already present in the noninteracting Kaniadakis model and the interaction produces only a small shift in its timing. We derive the autonomous evolution equations, the effective dark-energy equation of state, and the deceleration parameter. The adiabatic squared sound speed is also examined as a diagnostic of the effective-fluid stability, while statefinder variables are used to characterize deviations from ΛCDM. Finally, we verify that the K→0 limit continuously recovers standard Einstein-gravity particle-horizon HDE, for which the noninteracting model remains decelerating.
ER -