Finsler–Randers cosmology: dynamical analysis and growth of matter perturbations

Papagiannopoulos, G.; Basilakos, Spyros; Paliathanasis, Andronikos; Savvidou, Sofia; Stavrinos, P. C.

doi:10.1088/1361-6382/aa8be1

Cited by 55 publications

(35 citation statements)

References 72 publications

(160 reference statements)

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“…In Lorentzian geometry these symmetry demands on spacetime lead to a metric of Friedman-Lemaître-Robertson-Walker (FLRW) type. Finsler geometry has also been considered in the context of cosmological models [49][50][51][52][53][54]. In [11] the most general homogeneous and isotropic Finsler spacetimes were derived.…”

Section: Non Null-vgr Berwald Spacetimesmentioning

confidence: 99%

Berwald spacetimes and very special relativity

2018

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In this work we study Berwald spacetimes and their vacuum dynamics, where the latter are based on a Finsler generalization of the Einstein's equations derived from an action on the unit tangent bundle. In particular, we consider a specific class of spacetimes which are non-flat generalizations of the very special relativity (VSR) line element, to which we refer as very general relativity (VGR). We derive necessary and sufficient conditions for the VGR line element to be of Berwald type. We present two novel examples with the corresponding vacuum field equations: a Finslerian generalization of vanishing scalar invariant (VSI) spacetimes in Einstein's gravity as well as the most general homogeneous and isotropic VGR spacetime.

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Section: Non Null-vgr Berwald Spacetimesmentioning

confidence: 99%

Berwald spacetimes and very special relativity

2018

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“…We note that the canonical scalar field models are more informative compared to the non-canonical scalar field models. The physics of canonical scalar field models, which is mostly contained in the potential, V (φ(t)) where φ(t) is the underlying field, have gained a considerable interest in the cosmological community due to explaining various stages of the universe evolution, see [30,31,32,33,34,35,36,37,38,39,40,41,42,43,44,45,46,47,48,49,50,51,52,53,54,55,56,57] (also see [58,59,60,61,62]). The selection of quintessence scalar field models should not be much arbitrary, according to recently introduced swampland [63,64] and refined swampland [65] criteria.…”

Section: Introductionmentioning

confidence: 99%

Constraints on quintessence scalar field models using cosmological observations

Yang

Shahalam

Pal³

et al. 2019

Phys. Rev. D

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We consider a varieties of quintessence scalar field models in a homogeneous and isotropic geometry of the universe with zero spatial curvature aiming to provide stringent constraints using a series of cosmological data sets, namely, the cosmic microwave background observations (CMB), baryon acoustic oscillations (BAO), joint light curve analysis (JLA) from supernovae type Ia, redshift space distortions (RSD), and the cosmic chronometers (CC). From the qualitative evolution of the models, we find all of them are able to execute a fine transition from the past decelerating phase to the presently accelerating expansion where in addition, the equation of state of the scalar field (also the effective equation of state) might be close to that of the ΛCDM cosmology depending on its free parameters. From the observational analyses, we find that the scalar field parameters are unconstrained irrespective of all the observational datasets. In fact, we find that the quintessence scalar field models are pretty much determined by the CMB observations since any of the external datasets such as BAO, JLA, RSD, CC does not add any constraining power to CMB. Additionally, we observe a strong negative correlation between the parameters H0 (present value of the Hubble parameter), Ωm0 (density parameter for the matter sector, i.e., cold dark matter plus baryons) exists, while no correlation between H0, and σ8 (amplitude of the matter fluctuation) are not correlated. We also comment that the present models are unable to reconcile the tension on H0. Finally, we conclude our work with the Bayesian analyses which report that the non-interacting ΛCDM model is preferred over all the quintessence scalar field models.

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“…Following our previous works [130,131] we study how the implementation of the Finsler geometry affects the varying vacuum scenarios studied in GR as well as how the implementation of the varying vacuum responds in a Finsler Randers scenario.…”

Section: Varying Vacuum In a Finsler Randers Modelmentioning

confidence: 99%

“…Thus for a healthy theory to be viable, the critical point analysis should provide points where the universe will be accelerating and also these points to be stable. This analysis has been applied in various cosmological models, for instance see and references therein [130,131,[135][136][137][138][139][140][141][142][143][144][145][146][147] .…”

Section: Dynamical Evolutionmentioning

confidence: 99%

Dynamics in varying vacuum Finsler–Randers cosmology

et al. 2020

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In the context of Finsler-Randers theory we consider, for the first time, the cosmological scenario of the varying vacuum. In particular, we assume the existence of a cosmological fluid source described by an ideal fluid and the varying vacuum terms. We determine the cosmological history of this model by performing a detailed study on the dynamics of the field equations. We determine the limit of General Relativity, while we find new eras in the cosmological history provided by the geometrodynamical terms provided by the Finsler-Randers theory.

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Finsler–Randers cosmology: dynamical analysis and growth of matter perturbations

Abstract: 1 The Hubble parameter in the extended Finsler-Randers model is given by H 2 (a) = 8πG 3 ρm − a −2 aΨ(a)da − C 1 a 2 [see Eqs.(32) and (39) in Ref. [14]].

Cited by 55 publications

References 72 publications

Berwald spacetimes and very special relativity

Berwald spacetimes and very special relativity

Constraints on quintessence scalar field models using cosmological observations

Dynamics in varying vacuum Finsler–Randers cosmology

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