Classification of cosmological milestones

Fernández–Jambrina, L.; Lazkoz, Ruth

doi:10.1103/physrevd.74.064030

Cited by 156 publications

(177 citation statements)

References 28 publications

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“…That is, the first derivative of the scale factor is singular. Depending on the definition used [34,35], they can be either strong or weak [36].…”

Section: Cosmological Singularitiesmentioning

confidence: 99%

Initial directional singularity in inflationary models

Fernández–Jambrina

2016

Phys. Rev. D

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In [1] a new cosmological model is proposed with no big bang singularity in the past, though past geodesically incomplete. This model starts with an inflationary era, follows with a stiff matter dominated period and evolves to accelerated expansion in an asymptotically de Sitter regime in a realistic fashion. The big bang singularity is replaced by a directional singularity. This singularity cannot be reached by comoving observers, since it would take them an infinite proper time lapse to go back to it. On the contrary, observers with nonzero linear momentum have the singularity at finite proper time in their past, though arbitrarily large. Hence, the time lapse from the initial singularity can be as long as desired, even infinity, depending on the linear momentum of the observer. This conclusion applies to similar inflationary models. Due to the interest of these models, we address here the properties of such singularities.

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“…That is, the first derivative of the scale factor is singular. Depending on the definition used [34,35], they can be either strong or weak [36].…”

Section: Cosmological Singularitiesmentioning

confidence: 99%

Initial directional singularity in inflationary models

Fernández–Jambrina

2016

Phys. Rev. D

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“…These less constrained material stresses introduce new possibilities for the evolution of Friedmann universes and can produce unexpected types of finite-time singularity which are far weaker than the curvature singularities that often accompany geodesic incompleteness [5,6,7,8,9,10]. We found [11,12,13] a whole new class of pressure-driven singularities that keep the scale factor, a, the cosmological expansion rate,ȧ/a, and the density, ρ, finite while permitting the pressure, p, and the deceleration −ä/a, to blow up at a finite time despite the energy conditions ρ > 0 and ρ + 3p > 0 holding, and regardless of the three-curvature.…”

Section: Introductionmentioning

confidence: 99%

A general sudden cosmological singularity

Barrow

Cotsakis

Tsokaros

2010

Class. Quantum Grav.

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“…We will present elsewhere the behavior of other dark energy related singularities/events [23][24][25] such as big freeze, sudden singularity, type-IV singularity, little rip, etc., in the EiBI framework [26].…”

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confidence: 99%

Is Eddington–Born–Infeld theory really free of cosmological singularities?

Bouhmadi-López

Chen

2014

Eur. Phys. J. C

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The Eddington-inspired-Born-Infeld (EiBI) theory has recently been resurrected. Such a theory is characterized by being equivalent to Einstein theory in vacuum but differing from it in the presence of matter. One of the virtues of the theory is that it avoids the Big Bang singularity for a radiation-filled universe. In this paper, we analyze singularity avoidance in this kind of model. More precisely, we analyze the behavior of a homogeneous and isotropic universe filled with phantom energy in addition to the dark and baryonic matter. Unlike the Big Bang singularity that can be avoided in this kind of model through a bounce or a loitering effect on the physical metric, we find that the Big Rip singularity is unavoidable in the EiBI phantom model even though it can be postponed towards a slightly further future cosmic time as compared with the same singularity in other models based on the standard general relativity and with the same matter content as described above.

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Classification of cosmological milestones

Cited by 156 publications

References 28 publications

Initial directional singularity in inflationary models

Initial directional singularity in inflationary models

A general sudden cosmological singularity

Is Eddington–Born–Infeld theory really free of cosmological singularities?

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