Cosmological tests of sudden future singularities

Denkiewicz, Tomasz; Dąbrowski, Mariusz P.; Ghodsi, Hoda; Hendry, M.

doi:10.1103/physrevd.85.083527

Cited by 33 publications

(29 citation statements)

References 57 publications

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“…[19], SFS2 is just the standard dust (Einstein-de Sitter) limit δ → 0 of the SFS models, and SFS3 is plotted for the observationally best-fit region (supernovae, BAO, shift parameter) of the parameters as given in Refs. [20,21] and gives a complementary test of SFS models. As can be seen from the plots, SFS3 can mimic ΛCDM model, while SFS1 behaves differently than ΛCDM for large redshifts.…”

Section: Resultsmentioning

confidence: 99%

“…Here a ≡ a(t) is the scale factor, the dot means the derivative with respect to time t, G is the gravitational constant, c is the velocity of light, and the curvature index k = 0, ±1. For further considerations we set k = 0, and define an effective barotropic index as [21] …”

Section: Sfs and Fsfs In Isotropic Cosmologymentioning

confidence: 99%

“…It is easy to notice that in the limit δ → 0 and m = 2/3 one has H(z) = H 2 0 Ω m0 (1 + z) 3 , as for dust matter dominated case. Let us recall that the standard formula for the models which also includes the dark energy component Ω w0 reads as [21] …”

Section: Redshift Driftmentioning

confidence: 99%

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Redshift drift test of exotic singularity universes

et al. 2014

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We discuss how dynamical dark energy universes with exotic singularities may be distinguished from the standard ΛCDM model on the basis of their redshift drift signal, for which measurements both in the acceleration phase and in the deep matter era will be provided by forthcoming astrophysical facilities. Two specific classes of exotic singularity models are studied: sudden future singularity models and finite scale factor singularity models. In each class we identify the models which can mimic ΛCDM and play the role of dark energy as well as models for which redshift drift signals are significantly different from ΛCDM and the test can differentiate between them.

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Section: Resultsmentioning

confidence: 99%

Section: Sfs and Fsfs In Isotropic Cosmologymentioning

confidence: 99%

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Redshift drift test of exotic singularity universes

et al. 2014

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“…[65,66] using standard ruler and standard candle cosmological data constraining the form of the past expansion history of the universe. The possible existence of such events in the future light cone has also been investigated under specific assumptions of the functional form of the future Hubble expansion rate [67][68][69][70][71][72][73].…”

Section: Arxiv:160908528v2 [Gr-qc] 5 Nov 2016mentioning

confidence: 99%

Fate of bound systems through sudden future singularities

Perivolaropoulos

2016

Phys. Rev. D

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Sudden singularities occur in FRW spacetimes when the scale factor remains finite and different from zero while some of its derivatives diverge. After proper rescaling, the scale factor close to such a singularity at t = 0 takes the form a(t) = 1 + c|t| η (where c and η are parameters and η ≥ 0). We investigate analytically and numerically the geodesics of free and gravitationally bound particles through such sudden singularities. We find that even though free particle geodesics go through sudden singularities for all η ≥ 0, bound systems get dissociated (destroyed) for a wide range of the parameter c. For η < 1 bound particles receive a diverging impulse at the singularity and get dissociated for all positive values of the parameter c. For η > 1 (Sudden Future Singularities (SFS)) bound systems get a finite impulse that depends on the value of c and get dissociated for values of c larger than a critical value ccr(η, ω0) > 0 that increases with the value of η and the rescaled angular velocity ω0 of the bound system. We obtain an approximate equation for the analytical estimate of ccr(η, ω0). We also obtain its accurate form by numerical derivation of the bound system orbits through the singularities. Bound system orbits through Big Brake singularities (c < 0, 1 < η < 2) are also derived numerically and are found to get disrupted (deformed) at the singularity. However, they remain bound for all values of the parameter c considered.

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“…The problem of obtaining constraints on cosmological future singularities from astronomical observations was investigated for all five types of singularities: type I in [18], type II in [19], type III in [20], type IV in [21], type V in [16].…”

Section: Introductionmentioning

confidence: 99%

Singularities in particle-like description of FRW cosmology

Szydłowski

Stachowski

2018

Eur. Phys. J. C

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In this paper, we apply the method of reducing the dynamics of FRW cosmological models with a barotropic form of the equation of state to the dynamical system of the Newtonian type to detect the finite scale factor singularities and the finite-time singularities. In this approach all information concerning the dynamics of the system is contained in a diagram of the potential function V (a) of the scale factor. Singularities of the finite scale factor make themselves manifest by poles of the potential function. In our approach the different types of singularities are represented by critical exponents in the power-law approximation of the potential. The classification can be given in terms of these exponents. We have found that the pole singularity can mimic an inflation epoch. We demonstrate that the cosmological singularities can be investigated in terms of the critical exponents of the potential function of the cosmological dynamical systems. We assume that the general form of the model contains matter and some kind of dark energy which is parameterised by the potential. We distinguish singularities (by an ansatz involving the Lagrangian) of the pole type with the inflation and demonstrate that such a singularity can appear in the past.

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Cosmological tests of sudden future singularities

Cited by 33 publications

References 57 publications

Redshift drift test of exotic singularity universes

Redshift drift test of exotic singularity universes

Fate of bound systems through sudden future singularities

Singularities in particle-like description of FRW cosmology

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