Constraining Kaniadakis Holographic Dark Energy Model in Bianchi Type–III Cosmology

  • Y. Aditya Department of Mathematics, GMR Institute of Technology (GMRIT) – Deemed to be University, Rajam, India https://orcid.org/0000-0002-5468-9697
  • K. Dasunaidu Department of Mathematics, GMR Institute of Technology (GMRIT) – Deemed to be University, Rajam, India https://orcid.org/0000-0003-3583-2432
  • Muralasetti Nookaraju Department of Chemistry, Aditya University, Surampalem, India https://orcid.org/0000-0002-3743-8036
  • P. Silpa Department of Chemistry, Sri Vasavi Engineering College, Tadepalligudem, India
  • G. Suryanarayana Department of Mathematics, ANITS, Visakhapatnam, India https://orcid.org/0000-0002-4866-4020
DOI: https://doi.org/10.26565/2312-4334-2026-2-02
Keywords: Kaniadakis holographic dark energy, Brans–Dicke–Rastall gravity, Bianchi type–III universe, MCMC analysis, acceleration

Abstract

In this work, we study the cosmological dynamics of an anisotropic Bianchi type--III universe filled with Kaniadakis holographic dark energy and pressureless matter within the framework of Brans--Dicke--Rastall theory of gravity. To obtain exact solutions of the field equations, suitable relations among the metric potentials are assumed, together with a functional relation between the scalar field and the average scale factor. To constrain the model parameters, we perform a Markov Chain Monte Carlo analysis using joint CC+BAO datasets. The reconstructed Hubble parameter shows excellent agreement with observational data within the 1σ and 2σ confidence regions, and the estimated value of the Hubble constant is consistent with recent measurements. We derive several important cosmological parameters, including the Hubble parameter, deceleration parameter, equation of state parameter, scalar field, cosmic time and lookback time. The physical behavior of these parameters is analyzed through graphical representations. The deceleration parameter exhibits a smooth transition from an early decelerated phase to a late--time accelerated phase, with a transition redshift consistent with recent observational bounds. The equation of state parameter remains in the phantom region, indicating a dynamical dark energy behavior capable of driving the current accelerated expansion. Furthermore, the statefinder (r,s) and (r,q) diagnostics reveal that the model closely approaches the ΛCDM behavior at late times, while allowing deviations at earlier epochs. The Οm(z) diagnostic further supports the phantom--like nature of dark energy in the present framework. Overall, our results demonstrate that our model in Brans--Dicke--Rastall gravity provides a viable and observationally consistent description of the cosmic expansion history in an anisotropic universe.

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Published
2026-06-10
Cited
How to Cite
Aditya, Y., Dasunaidu, K., Nookaraju, M., Silpa, P., & Suryanarayana, G. (2026). Constraining Kaniadakis Holographic Dark Energy Model in Bianchi Type–III Cosmology. East European Journal of Physics, (2), 19-33. https://doi.org/10.26565/2312-4334-2026-2-02
Issue
No. 2 (2026): East European Journal of Physics
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Original Papers

Copyright (c) 2026 Y. Aditya, K. Dasunaidu, Muralasetti Nookaraju, P. Silpa, G. Suryanarayana

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