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Journal articles on the topic 'Big Rip'

Author: Grafiati

Published: 7 June 2025

Last updated: 16 July 2025

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1

Holmes, Su. "Big Brother RIP." Celebrity Studies 2, no. 2 (2011): 214–17. http://dx.doi.org/10.1080/19392397.2011.574875.

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2

CHIMENTO, L. P., and RUTH LAZKOZ. "ON BIG RIP SINGULARITIES." Modern Physics Letters A 19, no. 33 (2004): 2479–84. http://dx.doi.org/10.1142/s0217732304015646.

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Here we discuss big rip singularities occurring in typical phantom models by violation of the weak energy condition. After that, we compare them with future late-time singularities arising in models where the scale factor ends in a constant value and there is no violation of the strong energy condition. In phantom models the equation of state is well defined along the whole evolution, even at the big rip. However, both the pressure and the energy density of the phantom field diverge. In contrast, in the second kind of model the equation of state is not defined at the big rip because the pressure bursts at a finite value of the energy density.

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3

Bouhmadi-López, Mariam, and José A. Jiménez Madrid. "Escaping the big rip?" Journal of Cosmology and Astroparticle Physics 2005, no. 05 (2005): 005. http://dx.doi.org/10.1088/1475-7516/2005/05/005.

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4

FRAMPTON, PAUL H., and KEVIN J. LUDWICK. "CYCLIC COSMOLOGY FROM THE LITTLE RIP." Modern Physics Letters A 28, no. 29 (2013): 1350125. http://dx.doi.org/10.1142/s0217732313501253.

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We revisit a cyclic cosmology scenario proposed in 2007 to examine whether its hypotheses can be sustained if the underlying big-rip evolution, which was assumed there, is replaced by the recently proposed little rip. We show that the separation into causal patches at turnaround is generally valid for a little rip, and therefore conclude that the little rip is equally as suitable a basis for cyclicity as is the big rip.

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5

Bouhmadi-López, Mariam, Pedro F. González-Díaz, and Prado Martín-Moruno. "Worse than a big rip?" Physics Letters B 659, no. 1-2 (2008): 1–5. http://dx.doi.org/10.1016/j.physletb.2007.10.079.

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6

Mishra, R. K., and A. Singh. "Variable cosmology with “big-rip”." EAS Publications Series 36 (2009): 101–4. http://dx.doi.org/10.1051/eas/0936013.

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7

Dimopoulos, Konstantinos. "Is the Big Rip unreachable?" Physics Letters B 785 (October 2018): 132–35. http://dx.doi.org/10.1016/j.physletb.2018.08.040.

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8

Borislavov Vasilev, Teodor, Mariam Bouhmadi-López, and Prado Martín-Moruno. "Classical and Quantum f(R) Cosmology: The Big Rip, the Little Rip and the Little Sibling of the Big Rip." Universe 7, no. 8 (2021): 288. http://dx.doi.org/10.3390/universe7080288.

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The big rip, the little rip and the little sibling of the big rip are cosmological doomsdays predicted by some phantom dark-energy models that could describe the future evolution of our universe. When the universe evolves towards either of these future cosmic events, all bounded structures and, ultimately, space–time itself are ripped apart. Nevertheless, it is commonly believed that quantum gravity effects may smooth or even avoid these classically predicted singularities. In this review, we discuss the classical and quantum occurrence of these riplike events in the scheme of metric f(R) theories of gravity. The quantum analysis is performed in the framework of f(R) quantum geometrodynamics. In this context, we analyze the fulfilment of the DeWitt criterion for the avoidance of these singular fates. This review contains as well new unpublished work (the analysis of the equation of state for the phantom fluid and a new quantum treatment of the big rip and the little sibling of the big rip events).

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9

Astashenok, Artyom V., Shinʼichi Nojiri, Sergei D. Odintsov, and Artyom V. Yurov. "Phantom cosmology without Big Rip singularity." Physics Letters B 709, no. 4-5 (2012): 396–403. http://dx.doi.org/10.1016/j.physletb.2012.02.039.

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10

Yadav, Anil Kumar. "Dissipative Future Universe Without Big Rip." International Journal of Theoretical Physics 50, no. 5 (2011): 1664–70. http://dx.doi.org/10.1007/s10773-011-0675-4.

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11

Barboza, Edésio M., and Nivaldo A. Lemos. "Does the Big Rip survive quantization?" General Relativity and Gravitation 38, no. 11 (2006): 1609–22. http://dx.doi.org/10.1007/s10714-006-0333-y.

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12

Bouhmadi-López, Mariam, Ahmed Errahmani, Prado Martín-Moruno, Taoufik Ouali, and Yaser Tavakoli. "The little sibling of the big rip singularity." International Journal of Modern Physics D 24, no. 10 (2015): 1550078. http://dx.doi.org/10.1142/s0218271815500789.

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In this paper, we present a new cosmological event, which we named the little sibling of the big rip. This event is much smoother than the big rip singularity. When the little sibling of the big rip is reached, the Hubble rate and the scale factor blow up, but the cosmic derivative of the Hubble rate does not. This abrupt event takes place at an infinite cosmic time where the scalar curvature explodes. We show that a doomsday à la little sibling of the big rip is compatible with an accelerating universe, indeed at present it would mimic perfectly a ΛCDM scenario. It turns out that, even though the event seems to be harmless as it takes place in the infinite future, the bound structures in the universe would be unavoidably destroyed on a finite cosmic time from now. The model can be motivated by considering that the weak energy condition should not be strongly violated in our universe, and it could give us some hints about the status of recently formulated nonlinear energy conditions.

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13

Faraoni, V. "Possible fates for the accelerating Universe." Canadian Journal of Physics 84, no. 6-7 (2006): 583–89. http://dx.doi.org/10.1139/p06-025.

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The accelerating Universe may end in eternal de Sitter expansion, in a Big Rip, or in super-exponential expansion. We discuss a gauge-independent stability analysis of de Sitter space in scalartensor and in modified gravity, the late-time dynamics of a phantom Universe with general potential, and the recent proposal of evading the Big Rip through wormhole tunneling.PACS Nos.: 98.80.k, 04.50.+h, 04.20.q

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14

BAMBA, KAZUHARU, CHAO-QIANG GENG, SHIN'ICHI NOJIRI, and SERGEI D. ODINTSOV. "CROSSING OF PHANTOM DIVIDE IN F(R) GRAVITY." Modern Physics Letters A 25, no. 11n12 (2010): 900–908. http://dx.doi.org/10.1142/s0217732310000058.

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An explicit model of F(R) gravity with realizing a crossing of the phantom divide is reconstructed. In particular, it is shown that the Big Rip singularity may appear in the reconstructed model of F(R) gravity. Such a Big Rip singularity could be avoided by adding R2 term or non-singular viable F(R) theory1 to the model because phantom behavior becomes transient.

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15

Khadekar, G. S., and N. V. Gharad. "Big Rip Singularity in 5D Viscous Cosmology." Open Astronomy Journal 7, no. 1 (2014): 7–11. http://dx.doi.org/10.2174/1874381101407010007.

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16

Pradhan, Sasmita Kumari, Sunil Kumar Tripathy, Zashmir Naik, Dipanjali Behera, and Mrutunjaya Bhuyan. "Big Rip Scenario in Brans-Dicke Theory." Foundations 2, no. 1 (2022): 128–39. http://dx.doi.org/10.3390/foundations2010007.

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In this work, we present a Big Rip scenario within the framework of the generalized Brans-Dicke (GBD) theory. In the GBD theory, we consider an evolving BD parameter along with a self-interacting potential. An anisotropic background is considered to have a more general view of the cosmic expansion. The GBD theory with a cosmological constant is presented as an effective cosmic fluid within general relativity which favours a phantom field dominated phase. The model parameters are constrained so that the model provides reasonable estimates of the Hubble parameter and other recent observational aspects at the present epoch. The dynamical aspects of the BD parameter and the BD scalar field have been analysed. It is found that the present model witnesses a finite time doomsday at a time of tBR≃16.14Gyr, and for this scenario, the model requires a large negative value of the Brans-Dicke parameter.

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17

Fabris, J. C., and D. Pavón. "Big rip avoidance via black hole production." Gravitation and Cosmology 15, no. 3 (2009): 234–40. http://dx.doi.org/10.1134/s0202289309030062.

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18

Alvarenga, F. G., A. B. Batista, J. C. Fabris, and S. Houndjo. "Quantum effects near the big rip revisited." Gravitation and Cosmology 16, no. 2 (2010): 105–17. http://dx.doi.org/10.1134/s0202289310020039.

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19

Calderón, Héctor, and William A. Hiscock. "Quantum fields and ‘big rip’ expansion singularities." Classical and Quantum Gravity 22, no. 4 (2005): L23—L26. http://dx.doi.org/10.1088/0264-9381/22/4/l01.

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20

Schewe, Philip F. "The big rip: A new cosmic doomsday." Physics Today 56, no. 10 (2003): 9. http://dx.doi.org/10.1063/1.4796907.

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21

GRANDA, L. N., and E. LOAIZA. "BIG RIP AND LITTLE RIP SOLUTIONS IN SCALAR MODEL WITH KINETIC AND GAUSS–BONNET COUPLINGS." International Journal of Modern Physics D 21, no. 01 (2012): 1250002. http://dx.doi.org/10.1142/s0218271812500022.

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Late time cosmological solutions for scalar field model with kinetic and Gauss–Bonnet couplings are considered. The quintom scenario is realized with and without Big Rip singularity. We find that under specific choice of the Gauss–Bonnet coupling, the model considerably simplifies, giving rise to solutions where the kinetic term is proportional to the square of the Hubble parameter. This allows to reconstruct the model for a suitable cosmological evolution. We considered a solution that matches the observed behavior of the equation of state, while Big Rip singularity may be present or absent, depending on the parameters of the solution. Evolutionary scenarios known as Little Rip, have also been considered.

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22

WEI, YI-HUAN. "SYMMETRIES ABOUT BIG RIP IN SO(1, 1) PHANTOM UNIVERSE." Modern Physics Letters A 21, no. 37 (2006): 2845–52. http://dx.doi.org/10.1142/s0217732306020299.

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We study the SO(1, 1) dark energy model with the inverse power law potential, V = V0Φ-n, and find for n<2 the model has the late-time phantom property and the universe will evolve to the future Big Rip. The inverse linear potential is a special case, for which the field and the scalar factor are respectively T-invariant and CT-invariant about the Big Rip.

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23

HOUNDJO, M. J. S., A. V. MONWANOU, and JEAN B. CHABI OROU. "QUANTUM EFFECTS FROM PARTICLE PRODUCTION ON BACKGROUND EVOLUTION AND CARDY–VERLINDE FORMULA IN f(R) GRAVITY." International Journal of Modern Physics D 20, no. 13 (2011): 2449–69. http://dx.doi.org/10.1142/s0218271811020457.

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We investigate particle production in an expanding universe under the assumption that the Lagrangian contains the Einstein term R plus a modified gravity term of the form Rα, where α is a constant. Dark fluid is considered as the main content of the universe and the big rip singularity appears. Quantum effects due to particle creation is analyzed near the singularity and we find that for α ∈ ]½, 1[, quantum effects are dominant and the big rip may be avoided whereas for α ∈ J the dark fluid is dominant and the singularity remains. The Cardy–Verlinde formula is also introduced and its equivalence with the total entropy of the universe is checked. It is found that this can always occur in Einstein gravity while in f(R) gravity, it holds only for [Formula: see text], n being the space dimension, corresponding to the situation in which the big rip cannot be avoided.

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24

Houndjo, M. J. S., C. E. M. Batista, J. P. Campos, and O. F. Piattella. "Finite-time singularities in f(R, T) gravity and the effect of conformal anomaly." Canadian Journal of Physics 91, no. 7 (2013): 548–53. http://dx.doi.org/10.1139/cjp-2013-0023.

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We investigate f(R, T) gravity models (where R is the curvature scalar and T is the trace of the stress–energy tensor of ordinary matter) that are able to reproduce the four known types of future finite-time singularities. We choose a suitable expression for the Hubble parameter to realise the cosmic acceleration and we introduce two parameters, α and Hs, which characterise each type of singularity. We address the conformal anomaly and we observe that it cannot remove the sudden singularity or the Big Brake, but, for some values of α, the Big Rip and the Big Freeze may be avoided. We also find that, even without taking into account the conformal anomaly, the Big Rip and the Big Freeze may be removed thanks to the presence of the T contribution of the f(R, T) theory.

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25

Oikonomou, V. K. "Is a topology change after a Big Rip possible?" International Journal of Geometric Methods in Modern Physics 16, no. 03 (2019): 1950048. http://dx.doi.org/10.1142/s0219887819500488.

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Motivated by condensed matter physical systems, in which a finite-time singularity indicates that the topology of the system changes, we critically examine the possibility of the Universe’s topology change at a finite-time cosmological singularity. We emphasize on Big Rip and Type II and IV cosmological singularities, which we classify to future spacelike and timelike singularities. For the Type IV and Type II singularities, since no geodesics incompleteness occurs, no topological change is allowed, by using Geroch’s theorem arguments. However, for the Big Rip case, Tipler’s arguments allow a topology change, if the spacetime in which the topology change occurs is non-compact and the boundary of this region are two topologically distinct three-dimensional spacelike partial Cauchy hypersurfaces. Also, some additional requirements must hold true, among which the weak energy condition, which can be satisfied in a geometric way in the context of a modified gravity. We critically examine Tipler’s arguments for the Big Rip case, and we discuss the mathematical implications of such a topological change, with regard to the final hypersurface on which geodesics incompleteness occurs.

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26

Oliveira-Neto, G., and L. G. Rezende Rodrigues. "Noncommutative cosmological models induced by a symplectic formalism coupled to phantom fluids." International Journal of Modern Physics A 34, no. 31 (2019): 1950206. http://dx.doi.org/10.1142/s0217751x19502063.

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In this paper, we consider homogeneous and isotropic noncommutative cosmological models induced by a symplectic formalism coupled to phantom perfect fluids and a cosmological constant. After computing the field equations, we solve them to find the scalar factor dynamics. We restrict our attention to expansive solutions that may represent the present expansion of our Universe. These solutions generate big rip singularities. We study how the parameters, of these models, modify the time it takes for the scalar factor to expand from zero till infinity, at the big rip.

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27

Xi, Ping, Xiang-hua Zhai, and Xin-zhou Li. "Alternative mechanism of avoiding the big rip or little rip for a scalar phantom field." Physics Letters B 706, no. 4-5 (2012): 482–89. http://dx.doi.org/10.1016/j.physletb.2011.11.055.

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28

Bakry, M. A., and Aryn T. Shafeek. "Big Rip and Big Crunch Cosmological Models in a Gravitational Field with Torsion." Gravitation and Cosmology 27, no. 1 (2021): 89–104. http://dx.doi.org/10.1134/s0202289321010047.

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29

Dagwal, V. J., D. D. Pawar, Y. S. Solanke, and H. R. Shaikh. "Tilted universe with big rip singularity in Lyra geometry." Modern Physics Letters A 35, no. 24 (2020): 2050196. http://dx.doi.org/10.1142/s0217732320501965.

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We have examined tilted cosmological models by using conformally flat space-time with wet dark fluid in Lyra geometry. In order to solve the field equations we have considered a power law. In this paper we have discussed tilted universe with time-dependent displacement field vector, heat conduction vectors and also discussed big rip singularity. Some physical and geometrical properties are also investigated. We have also extended our work to investigate the consistency of the derived model with observational parameter from the point of astrophysical phenomenon such as look-back time-redshift, proper distance, luminosity distance, angular-diameter distance and distance modulus.

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30

GRANDA, L. N., D. F. JIMENEZ, and C. SANCHEZ. "QUINTESSENTIAL AND PHANTOM POWER-LAW SOLUTIONS IN SCALAR TENSOR MODEL OF DARK ENERGY." International Journal of Modern Physics D 22, no. 09 (2013): 1350055. http://dx.doi.org/10.1142/s0218271813500557.

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We consider a scalar-tensor model of dark energy with kinetic and Gauss–Bonnet (GB) couplings. We study the conditions for the existence of quintessential and phantom power-law expansion, and also analyze these conditions in the absence of a potential (closely related to string theory). A mechanism to avoid the Big Rip singularity in various asymptotic limits of the model has been studied. It was found that the kinetic and GB couplings might prevent the Big Rip singularity in a phantom scenario. The autonomous system for the model has been used to study the stability properties of the power-law solution, and the center manifold analysis was used to treat zero eigenvalues.

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31

Sepehri, Alireza, Anirudh Pradhan, and Hassan Amirhashchi. "Removing the big rip singularity from anisotropic universe in super string theory." Canadian Journal of Physics 93, no. 11 (2015): 1324–29. http://dx.doi.org/10.1139/cjp-2014-0651.

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Recently, various observational data predict the possibility that dark energy could be in the form of phantom field. The positive phantom-energy density grows without limit with the expansion of the Universe and leads to a big-rip singularity at a finite future time. The main question arises: what is the origin of the big rip singularity in a four-dimensional Universe? To answer this question, in this paper, we propose a new model in super string theory that allows taking into account the Dirac and vector string tachyon in addition to the scalar one, which stretches between branes and antibranes. In this model, scalar and Dirac string tachyons cancel each other’s effects and the only effect induced by the vector tachyon can be observed in density and pressures of the universe. We observe that different scale factors, pressures, and dark energy equation of state parameters are produced in different directions because of inhomogeneous tachyon dynamics and consequently one anisotropic universe is formed. Also, these observations are given in terms of effective tachyon potential and the separation between branes and antibranes. Thus, we have shown that the expansion of the anisotropic Universe is controlled by the vector string tachyon and evolves from the non-phantom phase to the phantom one and consequently, the phantom-dominated era of the universe accelerates and ends up in a big-rip singularity.

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32

Brevik, I., and A. V. Timoshkin. "Rip brane cosmology from a viscous holographic dark fluid." International Journal of Geometric Methods in Modern Physics 17, no. 06 (2020): 2050087. http://dx.doi.org/10.1142/s0219887820500875.

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This paper is devoted to the application of the holographic principle to describe Rip brane cosmological models in the presence of a bulk viscosity. We make use of the generalized infrared-cutoff holographic dark energy, introduced by Nojiri and Odintsov. We consider various examples: Rip brane cosmology corresponding to the Little Rip case, asymptotic de Sitter theory, and the so-called Big Freeze theory leading to a singularity. Analytical expressions for infrared cutoffs, as well as the particle and the future horizons at the brane, are obtained. The equations for energy conservation on the brane within the holographic theory are obtained in each case. The correspondence between viscous cosmology and holographic cosmology on the brane is shown.

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33

Curbelo, Ruben, Tame Gonzalez, Genly Leon, and Israel Quiros. "Interacting phantom energy and avoidance of the big rip singularity." Classical and Quantum Gravity 23, no. 5 (2006): 1585–601. http://dx.doi.org/10.1088/0264-9381/23/5/010.

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34

Chimento, Luis P., and Ruth Lazkoz. "Duality gives rise to Chaplygin cosmologies with a big rip." Classical and Quantum Gravity 23, no. 9 (2006): 3195–203. http://dx.doi.org/10.1088/0264-9381/23/9/027.

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35

Brevik, Iver, Olesya Gorbunova, and Diego Sáez-Gómez. "Casimir effects near the big rip singularity in viscous cosmology." General Relativity and Gravitation 42, no. 6 (2010): 1513–22. http://dx.doi.org/10.1007/s10714-009-0923-6.

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36

Bisabr, Yousef. "Non-minimal gravitational coupling of phantom and big rip singularity." General Relativity and Gravitation 45, no. 8 (2013): 1559–66. http://dx.doi.org/10.1007/s10714-013-1544-7.

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37

Belkacemi, Moulay-Hicham, Zahra Bouabdallaoui, Mariam Bouhmadi-López, Ahmed Errahmani, and Taoufik Ouali. "An interacting holographic dark energy model within an induced gravity brane." International Journal of Modern Physics D 29, no. 09 (2020): 2050066. http://dx.doi.org/10.1142/s0218271820500662.

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In this paper, we present a model for the late-time evolution of the universe where a dark energy-dark matter interaction is invoked. Dark energy is modeled through an holographic Ricci dark energy component. The model is embedded within an induced gravity braneworld model. For suitable choices of the interaction coupling, the big rip and little rip induced by the holographic Ricci dark energy, in a relativistic model and in an induced gravity braneworld model, are removed. In this scenario, the holographic dark energy will have a phantom like behavior even though the brane is asymptotically de Sitter.

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38

Kumar, Suresh. "Probing the matter and dark energy sources in a viable Big Rip model of the Universe." Modern Physics Letters A 29, no. 25 (2014): 1450119. http://dx.doi.org/10.1142/s0217732314501193.

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Chevallier–Polarski–Linder (CPL) parametrization for the equation of state (EoS) of dark energy in terms of cosmic redshift or scale factor have been frequently studied in the literature. In this study, we consider cosmic time-based CPL parametrization for the EoS parameter of the effective cosmic fluid that fills the fabric of spatially flat and homogeneous Robertson–Walker (RW) spacetime in General Relativity. The model exhibits two worthy features: (i) It fits the observational data from the latest H(z) and Union 2.1 SN Ia compilations matching the success of ΛCDM model. (ii) It describes the evolution of the Universe from the matter-dominated phase to the recent accelerating phase similar to the ΛCDM model but leads to Big Rip end of the Universe contrary to the everlasting de Sitter expansion in the ΛCDM model. We investigate the matter and dark energy sources in the model, in particular, behavior of the dynamical dark energy responsible for the Big Rip end of Universe.

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39

Mathew, Titus K., Chinthak Murali, and J. Shejeelammal. "Evolution of non-interacting entropic dark energy and its phantom nature." Modern Physics Letters A 31, no. 12 (2016): 1650071. http://dx.doi.org/10.1142/s0217732316500711.

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Assuming the form of the entropic dark energy (EDE) as it arises from the surface term in the Einstein–Hilbert’s action, its evolution was analyzed in an expanding flat universe. The model parameters were evaluated by constraining the model using the Union data on Type Ia supernovae. We found that in the non-interacting case, the model predicts an early decelerated phase and a later accelerated phase at the background level. The evolutions of the Hubble parameter, dark energy (DE) density, equation of state parameter and deceleration parameter were obtained. The model hardly seems to be supporting the linear perturbation growth for the structure formation. We also found that the EDE shows phantom nature for redshifts z [Formula: see text] 0.257. During the phantom epoch, the model predicts big rip effect at which both the scale factor of expansion and the DE density become infinitely large and the big rip time is found to be around 36 Giga years from now.

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40

Bergstrom, Arne. "Big Crunch, Big Rip – or a Self-Similar Expansion Replenished by Dark Matter and Dark Energy?" International Journal of Physics 2, no. 5 (2014): 146–50. http://dx.doi.org/10.12691/ijp-2-5-3.

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41

Benaoum, Hachemi, Pierre-Henri Chavanis, and Hernando Quevedo. "Generalized Logotropic Models and Their Cosmological Constraints." Universe 8, no. 9 (2022): 468. http://dx.doi.org/10.3390/universe8090468.

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We propose a new class of cosmological unified dark sector models called “Generalized Logotropic Models”. They depend on a free parameter n. The original logotropic model is a special case of our generalized model corresponding to n=1. The ΛCDM model is recovered for n=0. In our scenario, the Universe is filled with a single fluid, a generalized logotropic dark fluid (GLDF), whose pressure P includes higher order logarithmic terms of the rest-mass density ρm. The total energy density ϵ is the sum of the rest-mass energy density ρmc2 and the internal energy density u which play the roles of dark matter energy density ϵm and dark energy density ϵde, respectively. We investigate the cosmological behavior of the generalized logotropic models by focusing on the evolution of the energy density, scale factor, equation of state parameter, deceleration parameter and squared speed of sound. Low values of n≤3 are favored. We also study the asymptotic behavior of the generalized logotropic models. In particular, we show that the model presents a phantom behavior and has three distinct ways of evolution depending on the value of n. For 0<n≤2, it leads to a little rip and for n>2 to a big rip. We predict the value of the big rip time as a function of n without any free (undetermined) parameter.

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42

Berndt, Nikolaus, and Alan D. Rendall. "Isotropization in the approach to big rip singularities for Cardassian models." Classical and Quantum Gravity 25, no. 14 (2008): 145007. http://dx.doi.org/10.1088/0264-9381/25/14/145007.

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43

Wu, Puxun, and Hongwei Yu. "Avoidance of big rip in phantom cosmology by gravitational back reaction." Nuclear Physics B 727, no. 1-2 (2005): 355–67. http://dx.doi.org/10.1016/j.nuclphysb.2005.07.022.

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44

Makarenko, Andrey N., Valery V. Obukhov, and Iliy V. Kirnos. "From Big to Little Rip in modified F(R,G) gravity." Astrophysics and Space Science 343, no. 1 (2012): 481–88. http://dx.doi.org/10.1007/s10509-012-1240-1.

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45

Dogru, Melis Ulu, and İhsan Yilmaz. "Expanding and nonexpanding conformal wormholes, in scalar–tensor theory." International Journal of Modern Physics D 24, no. 08 (2015): 1550064. http://dx.doi.org/10.1142/s0218271815500649.

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We study spherically symmetric spacetime with anisotropic fluid in the scalar–tensor theory of gravity based on Lyra geometry. We suggest two different solutions of field equations for the theory by using Casimir effect. Obtained static and nonstatic solutions are similar to nonexpanding Lorentzian wormhole and expanding FRW-type wormhole, respectively. Furthermore, we study singularities of obtained solutions. We emphasize whether the expanding and nonexpanding wormholes conform with Big Rip or Big Crunch scenarios. Also, physical and geometrical properties of the solutions have been discussed.

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46

Balakin, Alexander, and Alexei Ilin. "Dark Energy and Dark Matter Interaction: Kernels of Volterra Type and Coincidence Problem." Symmetry 10, no. 9 (2018): 411. http://dx.doi.org/10.3390/sym10090411.

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We study a new exactly solvable model of coupling of the Dark Energy and Dark Matter, in the framework of which the kernel of non-gravitational interaction is presented by the integral Volterra-type operator well-known in the classical theory of fading memory. Exact solutions of this isotropic homogeneous cosmological model were classified with respect to the sign of the discriminant of the cubic characteristic polynomial associated with the key equation of the model. Energy-density scalars of the Dark Energy and Dark Matter, the Hubble function and acceleration parameter are presented explicitly; the scale factor is found in quadratures. Asymptotic analysis of the exact solutions has shown that the Big Rip, Little Rip, Pseudo Rip regimes can be realized with the specific choice of guiding parameters of the model. We show that the Coincidence problem can be solved if we consider the memory effect associated with the interactions in the Dark Sector of the universe.

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Odintsov, S. D., and V. K. Oikonomou. "Big bounce with finite-time singularity: The F(R) gravity description." International Journal of Modern Physics D 26, no. 08 (2017): 1750085. http://dx.doi.org/10.1142/s0218271817500857.

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An alternative to the Big Bang cosmologies is obtained by the Big Bounce cosmologies. In this paper, we study a bounce cosmology with a Type IV singularity occurring at the bouncing point in the context of [Formula: see text] modified gravity. We investigate the evolution of the Hubble radius and we examine the issue of primordial cosmological perturbations in detail. As we demonstrate, for the singular bounce, the primordial perturbations originating from the cosmological era near the bounce do not produce a scale-invariant spectrum and also the short wavelength modes after these exit the horizon, do not freeze, but grow linearly with time. After presenting the cosmological perturbations study, we discuss the viability of the singular bounce model, and our results indicate that the singular bounce must be combined with another cosmological scenario, or should be modified appropriately, in order that it leads to a viable cosmology. The study of the slow-roll parameters leads to the same result indicating that the singular bounce theory is unstable at the singularity point for certain values of the parameters. We also conformally transform the Jordan frame singular bounce, and as we demonstrate, the Einstein frame metric leads to a Big Rip singularity. Therefore, the Type IV singularity in the Jordan frame becomes a Big Rip singularity in the Einstein frame. Finally, we briefly study a generalized singular cosmological model, which contains two Type IV singularities, with quite appealing features.

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Fèvre, Raymond. "From the Big Bang to the Big Rip: One Cycle of a Closed Granular Friedmann-Planck Universe." Journal of High Energy Physics, Gravitation and Cosmology 07, no. 02 (2021): 377–90. http://dx.doi.org/10.4236/jhepgc.2021.72021.

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Roman, Soltero Alberto Rafael. "A Topological Model of the Universe: Klein Bottle and the Unification of the Big Crunch and Big Rip." Revista Multidisciplinaria de Ciencia Básica, Humanidades, Arte y Educación 2, no. 9 (2024): 24–32. https://doi.org/10.5281/zenodo.14184103.

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This paper presents a topological model of the universe based on the geometry of the Klein bottle, proposing that the Big Crunch and Big Rip may represent two manifestations of a single event within a non-orientable, cyclic universe. Using Roman’s Theorem of inverse permutations, which suggests symmetrical inverse states, the study explores how this topology may support a dynamic where cosmic expansion and collapse occur within a unified, cyclical framework. The model aims to reconcile certain anomalies observed in the Cosmic Microwave Background (CMB) and the distribution of dark matter by proposing a non-orientable spatial configuration. Preliminary findings suggest that a Klein bottle topology could align with Lambda Cold Dark Matter (ΛCDM) model observations, offering a novel perspective on cosmic evolution that connects expansion phases with contraction within a continuous topological cycle. The implications for dark energy, cosmic inflation, and the universe’s ultimate fate are discussed, emphasizing the model’s potential for expanding current cosmological paradigms.

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Albarran, Imanol, Mariam Bouhmadi-López, Francisco Cabral, and Prado Martín-Moruno. "The quantum realm of the ``Little Sibling'' of the Big Rip singularity." Journal of Cosmology and Astroparticle Physics 2015, no. 11 (2015): 044. http://dx.doi.org/10.1088/1475-7516/2015/11/044.

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