We examine bouncing cosmology in the anisotropic Bianchi type-III framework within Brans-Dicke gravity, incorporating Kaniadakis holographic dark energy with Hubble and Granda-Oliveros radii as infrared cutoff. We reconstruct bouncing model through correspondence scheme utilizing power-law form of the scalar field in terms of average scale factor. The natural anisotropy in Bianchi type-III model modifies expansion dynamics, offering a broader perspective on early-universe evolution beyond standard isotropic models. We analyze key cosmological parameters, including deceleration, jerk, equation of state ωde , energy conditions, squared sound speed <InlineEquation ID="IEq1"> <EquationSource Format="TEX">${\upsilon }_{s}^{2}$</EquationSource> <EquationSource Format="MATHML"><math> <msubsup> <mi>υ</mi> <mrow> <mi>s</mi> </mrow> <mn>2</mn> </msubsup> </math></EquationSource> </InlineEquation> and <InlineEquation ID="IEq2"> <EquationSource Format="TEX">${{\omega }_{de}-\omega }_{de}{\prime}$</EquationSource> <EquationSource Format="MATHML"><math> <mrow> <msub> <mrow> <msub> <mi>ω</mi> <mrow> <mi mathvariant="italic">de</mi> </mrow> </msub> <mo>-</mo> <mi>ω</mi> </mrow> <mrow> <mi mathvariant="italic">de</mi> </mrow> </msub> <mo>′</mo> </mrow> </math></EquationSource> </InlineEquation> plane. Models are exhibiting oscillatory transitions across the phantom divide and evolves smoothly toward ωde at late times. The stability analysis based on the squared sound speed <InlineEquation ID="IEq3"> <EquationSource Format="TEX">${\upsilon }_{s}^{2}$</EquationSource> <EquationSource Format="MATHML"><math> <msubsup> <mi>υ</mi> <mrow> <mi>s</mi> </mrow> <mn>2</mn> </msubsup> </math></EquationSource> </InlineEquation> reveals that models remain dynamically stable over most of the cosmic history and admit instabilities near the bounce. A dynamical phase-space study in the <InlineEquation ID="IEq4"> <EquationSource Format="TEX">${{\omega }_{de}-\omega }_{de}{\prime}$</EquationSource> <EquationSource Format="MATHML"><math> <mrow> <msub> <mrow> <msub> <mi>ω</mi> <mrow> <mi mathvariant="italic">de</mi> </mrow> </msub> <mo>-</mo> <mi>ω</mi> </mrow> <mrow> <mi mathvariant="italic">de</mi> </mrow> </msub> <mo>′</mo> </mrow> </math></EquationSource> </InlineEquation> plane shows that both models evolve predominantly in the thawing region, implying an asymptotic approach to a cosmological constant. The energy condition analysis further confirms that the violation of the null and strong energy conditions is a necessary feature for the realization of the bounce.

Dynamics of Bouncing Cosmology in Brans-Dicke Gravity with Kaniadakis Holographic Dark Energy

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发表日期：

2025年12月1日

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K. Murali,
Y. Aditya,
S. K. Vali

摘要

We examine bouncing cosmology in the anisotropic Bianchi type-III framework within Brans-Dicke gravity, incorporating Kaniadakis holographic dark energy with Hubble and Granda-Oliveros radii as infrared cutoff. We reconstruct bouncing model through correspondence scheme utilizing power-law form of the scalar field in terms of average scale factor. The natural anisotropy in Bianchi type-III model modifies expansion dynamics, offering a broader perspective on early-universe evolution beyond standard isotropic models. We analyze key cosmological parameters, including deceleration, jerk, equation of state ω_de , energy conditions, squared sound speed ${\upsilon }_{s}^{2}$ $υ_{s}^{2}$ and ${{\omega }_{de}-\omega }_{de}{\prime}$ ${ω_{de} - ω}_{de}'$ plane. Models are exhibiting oscillatory transitions across the phantom divide and evolves smoothly toward ω_de at late times. The stability analysis based on the squared sound speed ${\upsilon }_{s}^{2}$ $υ_{s}^{2}$ reveals that models remain dynamically stable over most of the cosmic history and admit instabilities near the bounce. A dynamical phase-space study in the ${{\omega }_{de}-\omega }_{de}{\prime}$ ${ω_{de} - ω}_{de}'$ plane shows that both models evolve predominantly in the thawing region, implying an asymptotic approach to a cosmological constant. The energy condition analysis further confirms that the violation of the null and strong energy conditions is a necessary feature for the realization of the bounce.