Cosmological tests of the osculating Barthel-Kropina dark energy model

Bouali, Amine; Chaudhary, Himanshu; Hama, Rattanasak; Harkó, Tiberiu; Sabau, Sorin V.; Martín, Marco San

doi:10.48550/arxiv.2301.10278

Cited by 2 publications

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“…For completeness, in this subsection we will examine a specific model. As one can see from the general Friedmann equations ( 48), (49), or equivalently from the effective darkenergy sector ( 55), (56), the appearance of the arbitrary functions W 0 (t) and W 1 (t), i.e. of A 0 (t), A 1 (t), makes the resulting cosmological phenomenology very capable.…”

Section: Specific Modelmentioning

confidence: 99%

“…For this specific example w DE lies in the quintessence regime. Nevertheless, note that according to the form of ( 55), (56), one could have other scenarios, in which w DE can be phantom-like, or experience the phantom divide cross-Fig. 1 Upper graph: The effective dark energy density parameter DE (green-solid), and the matter density parameter m (blue-dashed), as a function of the redshift z, for Finsler-Randers-Sasaki cosmology under the ansätze ( 46), (47), with y 0 = 1, y 1 = 10 −6 in units where κ = 1.…”

Section: Specific Modelmentioning

confidence: 99%

“…In Finsler and Finsler-like geometries more than one connection and curvature appear, which depend on the position and velocity, in contrast to GR in which there is only the Levi-Civita connection and the curvature of the Riemannian space. Therefore, gravity can be studied in a different way in the framework of an 8-dimensional Lorentz tangent bundle or a vector bundle which includes the observer (velocity/tangent vector) with extra internal/dynamical degrees of freedom [25][26][27][28][29][30]54], as well as in an osculating Riemannian and Barthel framework [55][56][57].…”

Section: Introductionmentioning

confidence: 99%

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Finsler–Randers–Sasaki gravity and cosmology

Kapsabelis,

Saridakis,

Stavrinos

2024

Eur. Phys. J. C

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We present for the first time a Friedmann-like construction in the framework of an osculating Finsler–Randers–Sasaki (F–R–S) geometry. In particular, we consider a vector field in the metric on a Lorentz tangent bundle, and thus the curvatures of horizontal and vertical spaces, as well as the extra contributions of torsion and non-linear connection, provide an intrinsic richer geometrical structure, with additional degrees of freedom, that lead to extra terms in the field equations. Applying these modified field equations at a cosmological setup we extract the generalized Friedmann equations for the horizontal and vertical space, showing that we obtain an effective dark energy sector arising from the richer underlying structure of the tangent bundle. Additionally, as it is common in Finsler-like constructions, we obtain an effective interaction between matter and geometry. Finally, we consider a specific model and we show that it can describe the sequence of matter and dark-energy epochs, and that the dark-energy equation of state can lie in the quintessence or phantom regimes, or cross the phantom divide.

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Section: Specific Modelmentioning

confidence: 99%

Section: Specific Modelmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Finsler–Randers–Sasaki gravity and cosmology

Kapsabelis,

Saridakis,

Stavrinos

2024

Eur. Phys. J. C

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“…where H th (z i ) represent the theoretical value obtained from our cosmological model, H obs (z i ) and represent the observed value of HP with a standard deviation 𝜎 2 H obs (z i ) (to see more and rundown all measurements see ref. [60] ).…”

Section: Hubble Measurement H(z)mentioning

confidence: 99%

Observational Constraining Study of New Deceleration Parameters in FRW Universe

Bouali

Chaudhary

Mumtaz

et al. 2023

Fortschritte der Physik

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In the current paper, a dark energy (DE) model reconstructed from the well‐motivated deceleration parameter (DP) is analyzed. A flat FRW Universe filled with radiation, dark matter (DM), and dark energy fluids is considered. The free parameters are constrained using measurements from Supernovae, Hubble, Gamma Ray Bursts, Quasars, and Baryon acoustic Oscillations. The model under study is found to be very supported by observation with respect to ΛCDM since . Besides, a cosmographic analysis is performed showing that the reconstructed model behaves similarly as ΛCDM does. Finally, a diagnostic analysis is performed reporting that the studied model behaves quintessence type at a late time.

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Cosmological tests of the osculating Barthel-Kropina dark energy model

Cited by 2 publications

References 0 publications

Finsler–Randers–Sasaki gravity and cosmology

Finsler–Randers–Sasaki gravity and cosmology

Observational Constraining Study of New Deceleration Parameters in FRW Universe

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