Gravitational baryogenesis in Gauss-Bonnet braneworld cosmology
Abstract
The present study investigates the feasibility of gravitational baryogenesis in a Gauss-Bonnet (GB) modified Randall-Sundrum (RS) type II braneworld cosmology. The modified expansion rate of the Universe in this scenario evolves through three distinct expansion regimes, the GB regime at early times where the expansion rate H ∼ ρ1/3 falls more slowly than the standard expansion law H∼ ρ1/2 of GR, then the RS type era with an enhanced expansion H ∼ ρ, before finally reducing to the standard expansion law in the low energy limit. Gravitational baryogenesis depends on Ṙ and requires Ṙ <0. This condition is satisfied for the GB and GR regimes. However, Ṙ>0 for the RS regime and successful baryogenesis requires either that the decoupling temperature occurs during the GB regime or that the Universe makes a direct transition from the GB regime to the GR regime. The GB baryon asymmetry η(T) is proportional to μ(1+w)(1−w)(1+1/β), where μ is the energy scale μ≡ 1/l associated with the bulk curvature scale l, β≡ 4 αμ2, where α is the GB coupling, and w is the equation of state parameter p=w ρ. Studies of inflation in GB-braneworld cosmology place constraints on the allowed ranges of the parameters μ and β. Guided by these, the asymmetry has been calculated for ranges of $(μ, β, w)$ and it is found that the observed values can be obtained for a value of β within the range (10−2 − 10−3) for μ=1012 GeV, and within the range (10−1− 10−2) for μ=1013 GeV. All values of η for μ=1014 are too high. In contrast to GR where η is zero for a radiation dominated Universe (w=1/3), it is non-zero in GB braneworld cosmology.
Related
BibTeX
@misc{whittingham2026gravitational,
title = {{Gravitational baryogenesis in Gauss-Bonnet braneworld cosmology}},
author = {Ian B Whittingham},
howpublished = {arXiv},
year = {2026},
month = oct,
doi = {10.48550/arxiv.2610.38188},
eprint = {2610.38188},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2610.38188},
note = {CC BY 4.0},
}
RIS
TY - UNPB
TI - Gravitational baryogenesis in Gauss-Bonnet braneworld cosmology
AU - Ian B Whittingham
PY - 2026
DA - 2026/10/28
PB - arXiv
DO - 10.48550/arxiv.2610.38188
UR - https://arxiv.org/abs/2610.38188
AB - The present study investigates the feasibility of gravitational baryogenesis in a Gauss-Bonnet (GB) modified Randall-Sundrum (RS) type II braneworld cosmology. The modified expansion rate of the Universe in this scenario evolves through three distinct expansion regimes, the GB regime at early times where the expansion rate H ∼ ρ^1/3 falls more slowly than the standard expansion law H∼ ρ^1/2 of GR, then the RS type era with an enhanced expansion H ∼ ρ, before finally reducing to the standard expansion law in the low energy limit. Gravitational baryogenesis depends on Ṙ and requires Ṙ <0. This condition is satisfied for the GB and GR regimes. However, Ṙ>0 for the RS regime and successful baryogenesis requires either that the decoupling temperature occurs during the GB regime or that the Universe makes a direct transition from the GB regime to the GR regime. The GB baryon asymmetry η(T) is proportional to μ(1+w)(1−w)(1+1/β), where μ is the energy scale μ≡ 1/l associated with the bulk curvature scale l, β≡ 4 αμ^2, where α is the GB coupling, and w is the equation of state parameter p=w ρ. Studies of inflation in GB-braneworld cosmology place constraints on the allowed ranges of the parameters μ and β. Guided by these, the asymmetry has been calculated for ranges of $(μ, β, w)$ and it is found that the observed values can be obtained for a value of β within the range (10^−2 − 10^−3) for μ=10^12 GeV, and within the range (10^−1− 10^−2) for μ=10^13 GeV. All values of η for μ=10^14 are too high. In contrast to GR where η is zero for a radiation dominated Universe (w=1/3), it is non-zero in GB braneworld cosmology.
ER -