New Barrow holographic dark energy: cosmological dynamics and cosmic chronometer analysis
Abstract
We formulate new Barrow holographic dark energy (NBHDE) as a second-order expansion of the Barrow entropy correction near the standard holographic dark energy (HDE) limit, adopting the future event horizon as the infrared cutoff. Writing the Barrow factor in exponential form identifies (Δ/2)ln SBH, rather than Δ alone, as the expansion parameter. In a flat universe containing pressureless matter and NBHDE without a cosmological constant, we derive the background equations, establish consistency with the integral definition of the future event horizon, and recover HDE exactly at Δ=0. We assess this approximation against the unexpanded Barrow holographic dark energy (BHDE) density, locally and through independently normalized background evolutions. Across 0.50≤ c≤1.20 and 0≤Δ≤0.003, the maximum fractional density difference remains below 1% over −0.99≤ z≤5, while the normalized Hubble rates differ by less than 0.074% over 0≤ z≤5. Within this domain, the Barrow correction modestly changes the expansion rate and acceleration transition but more strongly affects the dark energy equation of state and phantom crossing. At c=0.80, wd0 shifts from −1.031 in HDE to −0.900 at Δ=0.003. We perform a conditional comparison with 36 spectroscopic cosmic chronometer (CC) measurements. At fixed H0=67.4 km s−1 Mpc−1 and Ωm0=0.30, the minimum lies on the HDE boundary at Δ=0 and c=0.8457. Minimizing over c at Δ=0.003 gives cmin=0.6879, with ΔχCC2≃1.0×10−3. NBHDE therefore provides a self-consistent, quantitatively controlled framework near the HDE limit, showing that Barrow corrections can alter dark energy behavior even when their effect on H(z) is largely compensated by changing c.
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BibTeX
@misc{azarakhsh2026barrow,
title = {{New Barrow holographic dark energy: cosmological dynamics and cosmic chronometer analysis}},
author = {Omid Azarakhsh and Tayeb Golanbari and Behrooz Malekolkalami and Kh. Saaidi},
howpublished = {arXiv},
year = {2026},
month = sep,
doi = {10.48550/arxiv.2609.16047},
eprint = {2609.16047},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2609.16047},
}
RIS
TY - UNPB
TI - New Barrow holographic dark energy: cosmological dynamics and cosmic chronometer analysis
AU - Omid Azarakhsh
AU - Tayeb Golanbari
AU - Behrooz Malekolkalami
AU - Kh. Saaidi
PY - 2026
DA - 2026/09/12
PB - arXiv
DO - 10.48550/arxiv.2609.16047
UR - https://arxiv.org/abs/2609.16047
AB - We formulate new Barrow holographic dark energy (NBHDE) as a second-order expansion of the Barrow entropy correction near the standard holographic dark energy (HDE) limit, adopting the future event horizon as the infrared cutoff. Writing the Barrow factor in exponential form identifies (Δ/2)ln S_BH, rather than Δ alone, as the expansion parameter. In a flat universe containing pressureless matter and NBHDE without a cosmological constant, we derive the background equations, establish consistency with the integral definition of the future event horizon, and recover HDE exactly at Δ=0. We assess this approximation against the unexpanded Barrow holographic dark energy (BHDE) density, locally and through independently normalized background evolutions. Across 0.50≤ c≤1.20 and 0≤Δ≤0.003, the maximum fractional density difference remains below 1% over −0.99≤ z≤5, while the normalized Hubble rates differ by less than 0.074% over 0≤ z≤5. Within this domain, the Barrow correction modestly changes the expansion rate and acceleration transition but more strongly affects the dark energy equation of state and phantom crossing. At c=0.80, w_d0 shifts from −1.031 in HDE to −0.900 at Δ=0.003. We perform a conditional comparison with 36 spectroscopic cosmic chronometer (CC) measurements. At fixed H_0=67.4 km s^−1 Mpc^−1 and Ω_m0=0.30, the minimum lies on the HDE boundary at Δ=0 and c=0.8457. Minimizing over c at Δ=0.003 gives c_min=0.6879, with Δχ_CC^2≃1.0×10^−3. NBHDE therefore provides a self-consistent, quantitatively controlled framework near the HDE limit, showing that Barrow corrections can alter dark energy behavior even when their effect on H(z) is largely compensated by changing c.
ER -