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Journal articles on the topic 'Dark energy models'

Author: Grafiati

Published: 18 May 2024

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1

POLARSKI, DAVID. "DARK ENERGY." International Journal of Modern Physics D 22, no. 14 (2013): 1330027. http://dx.doi.org/10.1142/s0218271813300279.

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Dark energy models account for the present accelerated expansion of the universe. Many models were suggested and investigated, based on very different physical principles. We will review some representative models emphasizing similarities and differences between these various approaches.

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2

Motta, Verónica, Miguel A. García-Aspeitia, Alberto Hernández-Almada, Juan Magaña, and Tomás Verdugo. "Taxonomy of Dark Energy Models." Universe 7, no. 6 (2021): 163. http://dx.doi.org/10.3390/universe7060163.

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The accelerated expansion of the Universe is one of the main discoveries of the past decades, indicating the presence of an unknown component: the dark energy. Evidence of its presence is being gathered by a succession of observational experiments with increasing precision in its measurements. However, the most accepted model for explaining the dynamic of our Universe, the so-called Lambda cold dark matter, faces several problems related to the nature of such energy component. This has led to a growing exploration of alternative models attempting to solve those drawbacks. In this review, we br

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3

Khurshudyan, Martiros, and Asatur Khurshudyan. "Some Interacting Dark Energy Models." Symmetry 10, no. 11 (2018): 577. http://dx.doi.org/10.3390/sym10110577.

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In this paper, we study various cosmological models involving new nonlinear forms of interaction between cold dark matter (DM) and dark energy (DE) assuming that DE is a barotropic fluid. The interactions are nonlinear either due to log ( ρ d e / ρ d m ) or log ( ρ d m / ρ d e ) parameterizations, respectively. The main purpose of this paper is to demonstrate the applicability of the forms of suggested interactions to the problem of modern cosmology known as accelerated expansion of the Universe. Using the differential age of old galaxies expressed in terms of H ( z ) data, the peak position o

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4

Tawfik, Abdel Nasser, and Eiman Abou El Dahab. "Review on Dark Energy Models." Gravitation and Cosmology 25, no. 2 (2019): 103–15. http://dx.doi.org/10.1134/s0202289319020154.

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5

Sahni, Varun, and Yuri Shtanov. "Braneworld models of dark energy." Journal of Cosmology and Astroparticle Physics 2003, no. 11 (2003): 014. http://dx.doi.org/10.1088/1475-7516/2003/11/014.

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6

Sahni, Varun. "Theoretical models of dark energy." Chaos, Solitons & Fractals 16, no. 4 (2003): 527–37. http://dx.doi.org/10.1016/s0960-0779(02)00221-7.

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7

YOO, JAEWON, and YUKI WATANABE. "THEORETICAL MODELS OF DARK ENERGY." International Journal of Modern Physics D 21, no. 12 (2012): 1230002. http://dx.doi.org/10.1142/s0218271812300029.

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Mounting observational data confirm that about 73% of the energy density consists of dark energy which is responsible for the current accelerated expansion of the Universe. We present observational evidences and dark energy projects. We then review various theoretical ideas that have been proposed to explain the origin of dark energy; they contain the cosmological constant, modified matter models, modified gravity models and the inhomogeneous model. The cosmological constant suffers from two major problems: one regarding fine-tuning and the other regarding coincidence. To solve them there aros

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Chan, R., M. F. A. da Silva, and Jaime F. Villas da Rocha. "Star models with dark energy." General Relativity and Gravitation 41, no. 8 (2009): 1835–51. http://dx.doi.org/10.1007/s10714-008-0755-9.

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9

Arun, Kenath, S. B. Gudennavar, A. Prasad, and C. Sivaram. "Alternate models to dark energy." Advances in Space Research 61, no. 1 (2018): 567–70. http://dx.doi.org/10.1016/j.asr.2017.08.006.

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Pearson, Jonathan A. "Material models of dark energy." Annalen der Physik 526, no. 7-8 (2014): 318–39. http://dx.doi.org/10.1002/andp.201400052.

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11

QIU, TAOTAO, YI-FU CAI, and XINMIN ZHANG. "NULL ENERGY CONDITION AND DARK ENERGY MODELS." Modern Physics Letters A 23, no. 32 (2008): 2787–98. http://dx.doi.org/10.1142/s0217732308026194.

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Null Energy Condition (NEC) requires the equation of state (EoS) of the universe wu satisfy wu ≥ -1, which implies, for instance in a universe with matter and dark energy dominating wu = w m Ω m + w de Ω de = w de Ω de ≥ -1. In this paper we study constraints on the dark energy models from the requirement of the NEC. We will show that with Ω de ~ 0.7, w de < -1 at present epoch is possible. However, NEC excludes the possibility of w de < -1 forever as happened in the Phantom model, but if w de < -1 stays for a short period of time as predicted in the Quintom theory, NEC can be satisfi

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12

Avelino, P. P., and H. M. R. da Silva. "Effective dark energy equation of state in interacting dark energy models." Physics Letters B 714, no. 1 (2012): 6–10. http://dx.doi.org/10.1016/j.physletb.2012.06.063.

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13

Boyle, Latham A., Robert R. Caldwell, and Marc Kamionkowski. "Spintessence! New models for dark matter and dark energy." Physics Letters B 545, no. 1-2 (2002): 17–22. http://dx.doi.org/10.1016/s0370-2693(02)02590-x.

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14

Sussman, Roberto A., Israel Quiros, and Osmel Martín González. "Inhomogeneous models of interacting dark matter and dark energy." General Relativity and Gravitation 37, no. 12 (2005): 2117–43. http://dx.doi.org/10.1007/s10714-005-0199-4.

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15

Arun, Kenath, S. B. Gudennavar, and C. Sivaram. "Dark matter, dark energy, and alternate models: A review." Advances in Space Research 60, no. 1 (2017): 166–86. http://dx.doi.org/10.1016/j.asr.2017.03.043.

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16

Feng, Haoyang. "Integrated study of dark matter and dark energy models." Theoretical and Natural Science 34, no. 1 (2024): 162–71. http://dx.doi.org/10.54254/2753-8818/34/20241173.

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Dark matter and dark energy are used as two important concepts in cosmology to explain some of the observed phenomena in the universe. Dark matter is one of the most dominant constituents of the Universe, and it influences the structural formation of the Universe through gravity, including the formation and evolution of galaxies, clusters, and the large-scale structure of the Universe. Dark energy is believed to be one of the causes of the accelerated expansion of the Universe, and its presence explains the observed phenomenon of the accelerating rate of expansion of the Universe. Although the

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17

Lima, J. A. S. "Alternative dark energy models: an overview." Brazilian Journal of Physics 34, no. 1a (2004): 194–200. http://dx.doi.org/10.1590/s0103-97332004000200009.

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18

Bag, Satadru, Swagat S. Mishra, and Varun Sahni. "New tracker models of dark energy." Journal of Cosmology and Astroparticle Physics 2018, no. 08 (2018): 009. http://dx.doi.org/10.1088/1475-7516/2018/08/009.

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19

Pignol, Guillaume. "Probing Dark Energy models with neutrons." International Journal of Modern Physics A 30, no. 24 (2015): 1530048. http://dx.doi.org/10.1142/s0217751x15300483.

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There is a deep connection between cosmology — the science of the infinitely large — and particle physics — the science of the infinitely small. This connection is particularly manifest in neutron particle physics. Basic properties of the neutron — its Electric Dipole Moment and its lifetime — are intertwined with baryogenesis and nucleosynthesis in the early Universe. I will cover this topic in the first part, that will also serve as an introduction (or rather a quick recap) of neutron physics and Big Bang cosmology. Then, the rest of the paper will be devoted to a new idea: using neutrons to

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20

Paul, Prasenjit, and Rikpratik Sengupta. "Generalized Phenomenological Models of Dark Energy." Advances in High Energy Physics 2020 (February 20, 2020): 1–8. http://dx.doi.org/10.1155/2020/5249839.

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It was first observed at the end of the last century that the universe is presently accelerating. Ever since, there have been several attempts to explain this observation theoretically. There are two possible approaches. The more conventional one is to modify the matter part of the Einstein field equations, and the second one is to modify the geometry part. We shall consider two phenomenological models based on the former, more conventional approach within the context of general relativity. The phenomenological models in this paper consider a Λ term firstly a function of a¨/a and secondly a fu

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21

Saha, Bijan. "Isotropic and anisotropic dark energy models." Physics of Particles and Nuclei 45, no. 2 (2014): 349–96. http://dx.doi.org/10.1134/s1063779614020026.

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22

Frampton, Paul H., Kevin J. Ludwick, Shinʼichi Nojiri, Sergei D. Odintsov, and Robert J. Scherrer. "Models for little rip dark energy." Physics Letters B 708, no. 1-2 (2012): 204–11. http://dx.doi.org/10.1016/j.physletb.2012.01.048.

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23

CAI, RONG-GEN. "SOME REMARKS ON DARK ENERGY MODELS." International Journal of Modern Physics D 20, no. 08 (2011): 1313–25. http://dx.doi.org/10.1142/s0218271811019499.

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In this talk I classify dark energy models existing in the literatures into three classes. The first one is to ascribe the cosmic acceleration to modifications of general relativity at cosmological scales. The second one is due to the backreaction of perturbations, or say, the effect of inhomogeneity of the universe. The third one is some exotic component in the universe, which appears in the right hand side of Einstein's field equations. For each class I demonstrate some examples.

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24

Myung, Yun Soo, and Min-Gyun Seo. "Origin of holographic dark energy models." Physics Letters B 671, no. 4-5 (2009): 435–39. http://dx.doi.org/10.1016/j.physletb.2009.01.001.

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25

Horvat, R. "Entanglement in holographic dark energy models." Physics Letters B 693, no. 5 (2010): 596–99. http://dx.doi.org/10.1016/j.physletb.2010.09.014.

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26

Myung, Yun Soo. "Instability of holographic dark energy models." Physics Letters B 652, no. 5-6 (2007): 223–27. http://dx.doi.org/10.1016/j.physletb.2007.07.033.

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27

Kurek, Aleksandra, Orest Hrycyna, and Marek Szydłowski. "Constraints on oscillating dark energy models." Physics Letters B 659, no. 1-2 (2008): 14–25. http://dx.doi.org/10.1016/j.physletb.2007.10.074.

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28

Kim, Kyoung Yee, Hyung Won Lee, and Yun Soo Myung. "Instability of agegraphic dark energy models." Physics Letters B 660, no. 3 (2008): 118–24. http://dx.doi.org/10.1016/j.physletb.2007.12.045.

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29

CHEN, CHIEN-WEN, JE-AN GU, and PISIN CHEN. "CONSISTENCY TEST OF DARK ENERGY MODELS." Modern Physics Letters A 24, no. 21 (2009): 1649–57. http://dx.doi.org/10.1142/s0217732309031028.

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Recently we proposed a new approach to test dark energy models based on the observational data. In that work we focused particularly on quintessence models for demonstration and invoked a widely used parametrization of the dark energy equation of state. In this paper we take the more recent SN Ia , CMB and BAO data, invoke the same parametrization, and apply this method of consistency test to five dark energy models, including the ΛCDM model, the generalized Chaplygin gas, and three quintessence models: exponential, power-law and inverse-exponential potentials. We find that the exponential pot

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30

Khurshudyan, M., E. Chubaryan, and B. Pourhassan. "Interacting Quintessence Models of Dark Energy." International Journal of Theoretical Physics 53, no. 7 (2014): 2370–78. http://dx.doi.org/10.1007/s10773-014-2036-6.

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31

Mishra, Shruti, and Dr Avinash Singh. "Background Constraints on Dark Energy Models." Journal of Physics: Conference Series 2576, no. 1 (2023): 012016. http://dx.doi.org/10.1088/1742-6596/2576/1/012016.

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Abstract Due to the gravitational attraction of all the matter in the universe, the expansion rate of the cosmos has changed over time, decreasing (decelerating) in past, and more recently speeding up (accelerating). The hypothesis that the Universe is expanding quickly and is spatially nearing its limit now has a lot of cosmological evidence to back it up (assuming the density is at least somewhat time-independent). The majority of cosmologists believe that “dark energy” is to blame for the accelerated cosmological expansion that has been witnessed. The cosmological constant, an additional co

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32

Astashenok, Artyom V. "Effective dark energy models and dark energy models with bounce in frames of F(T) gravity." Astrophysics and Space Science 351, no. 1 (2014): 377–83. http://dx.doi.org/10.1007/s10509-014-1846-6.

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33

Dil, Emre. "Couplingq-Deformed Dark Energy to Dark Matter." Advances in High Energy Physics 2016 (2016): 1–20. http://dx.doi.org/10.1155/2016/9753208.

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We propose a novel coupled dark energy model which is assumed to occur as aq-deformed scalar field and investigate whether it will provide an expanding universe phase. We consider theq-deformed dark energy as coupled to dark matter inhomogeneities. We perform the phase-space analysis of the model by numerical methods and find the late-time accelerated attractor solutions. The attractor solutions imply that the coupledq-deformed dark energy model is consistent with the conventional dark energy models satisfying an acceleration phase of universe. At the end, we compare the cosmological parameter

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34

COPELAND, EDMUND J., M. SAMI, and SHINJI TSUJIKAWA. "DYNAMICS OF DARK ENERGY." International Journal of Modern Physics D 15, no. 11 (2006): 1753–935. http://dx.doi.org/10.1142/s021827180600942x.

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We review in detail a number of approaches that have been adopted to try and explain the remarkable observation of our accelerating universe. In particular we discuss the arguments for and recent progress made towards understanding the nature of dark energy. We review the observational evidence for the current accelerated expansion of the universe and present a number of dark energy models in addition to the conventional cosmological constant, paying particular attention to scalar field models such as quintessence, K-essence, tachyon, phantom and dilatonic models. The importance of cosmologica

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35

Mena, Olga. "Low redshift probes and coupled dark matter-dark energy models." Journal of Physics: Conference Series 259 (November 1, 2010): 012084. http://dx.doi.org/10.1088/1742-6596/259/1/012084.

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36

ONO, HIROYUKI, and HIDEYUKI SUZUKI. "DARK ENERGY MODELS AND SUPERNOVA RELIC NEUTRINOS." Modern Physics Letters A 22, no. 12 (2007): 867–82. http://dx.doi.org/10.1142/s0217732307022876.

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Recent cosmological observations show that the unknown energy element called dark energy dominates in the universe. In this letter, we investigate to what extent dark energy models influence supernova relic neutrino (SRN) spectra when the supernova rate could be determined by direct counting and discuss the possibility to distinguish dark energy models using future observation of SRN. We found that the total number of SRN events in GCG model will be larger than those in ΛCDM and holographic dark energy models by 20%. As a result, we find a possibility to distinguish GCG model from ΛCDM and hol

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37

TSUJIKAWA, SHINJI. "RECENT STATUS OF DARK ENERGY." Modern Physics Letters A 25, no. 11n12 (2010): 843–58. http://dx.doi.org/10.1142/s0217732310000010.

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We review a number of approaches that have been adopted to explain the origin of dark energy responsible for the late-time cosmic acceleration. This includes the cosmological constant and dynamical dark energy models such as quintessence, k -essence, Chaplygin gas, f(R) gravity, scalar-tensor theories, and braneworld models. We also discuss observational and local gravity constraints on those models and clarify which models are favored or ruled out in current observations.

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38

SUN, CHENG-YI, and YU SONG. "INCONSISTENCES IN INTERACTING AGEGRAPHIC DARK ENERGY MODELS." Modern Physics Letters A 26, no. 40 (2011): 3055–66. http://dx.doi.org/10.1142/s0217732311037285.

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It is found that the origin agegraphic dark energy tracks the matter in the matter-dominated epoch and then the subsequent dark-energy-dominated epoch becomes impossible. It is argued that the difficulty can be removed when the interaction between the agegraphic dark energy and dark matter is considered. In the note, by discussing three different interacting models, we find that the difficulty still stands even in the interacting models. Furthermore, we find that in the interacting models, there exists the other serious inconsistence that the existence of the radiation/matter-dominated epoch c

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39

LING, YI, and WEN-JIAN PAN. "(m, n)-TYPE HOLOGRAPHIC DARK ENERGY MODELS." Modern Physics Letters A 28, no. 31 (2013): 1350128. http://dx.doi.org/10.1142/s0217732313501289.

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We construct (m, n)-type holographic dark energy models at a phenomenological level, which can be viewed as a generalization of agegraphic models with the conformal-like age as the holographic characteristic size. For some values of (m, n) the holographic dark energy can automatically evolve across ω = -1 into a phantom phase even without introducing an interaction between the dark energy and background matter. Our construction is also applicable to the holographic dark energy with generalized future event horizon as the characteristic size. Finally, we address the issue on the stability of ou

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40

Pace, Francesco, and Carlo Schimd. "Tidal virialization of dark matter haloes with clustering dark energy." Journal of Cosmology and Astroparticle Physics 2022, no. 03 (2022): 014. http://dx.doi.org/10.1088/1475-7516/2022/03/014.

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Abstract We extend the analysis of Pace et al. [1] by considering the virialization process in the extended spherical collapse model for clustering dark-energy models, i.e., accounting for dark-energy fluctuations. Differently from the standard approach, here virialization is naturally achieved by properly modelling deviations from sphericity due to shear and rotation induced by tidal interactions. We investigate the time evolution of the virial overdensity Δvir in seven clustering dynamical dark energy models and compare the results to the ΛCDM model and to the corresponding smooth dark-energ

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41

Bolotin, Yuri L., Alexander Kostenko, Oleg A. Lemets, and Danylo A. Yerokhin. "Cosmological evolution with interaction between dark energy and dark matter." International Journal of Modern Physics D 24, no. 03 (2015): 1530007. http://dx.doi.org/10.1142/s0218271815300074.

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In this review we consider in detail different theoretical topics associated with interaction in the dark sector. We study linear and nonlinear interactions which depend on the dark matter and dark energy densities. We consider a number of different models (including the holographic dark energy and dark energy in a fractal universe), with interacting dark energy and dark matter, have done a thorough analysis of these models. The main task of this review was not only to give an idea about the modern set of different models of dark energy, but to show how much can be diverse dynamics of the univ

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42

Edmonds, Douglas, Djordje Minic, and Tatsu Takeuchi. "Dark matter, dark energy and fundamental acceleration." International Journal of Modern Physics D 29, no. 14 (2020): 2043030. http://dx.doi.org/10.1142/s0218271820430300.

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We discuss the existence of an acceleration scale in galaxies and galaxy clusters and its relevance for the nature of dark matter. The presence of the same acceleration scale found at very different length scales, and in very different astrophysical objects, strongly supports the existence of a fundamental acceleration scale governing the observed gravitational physics. We comment on the implications of such a fundamental acceleration scale for constraining cold dark matter models as well as its relevance for structure formation to be explored in future numerical simulations.

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43

Albarran, Imanol, Mariam Bouhmadi-López, and João Morais. "Cosmological Perturbations in Phantom Dark Energy Models." Universe 3, no. 1 (2017): 22. http://dx.doi.org/10.3390/universe3010022.

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44

Linton, Mark S., Robert Crittenden, and Alkistis Pourtsidou. "Momentum transfer models of interacting dark energy." Journal of Cosmology and Astroparticle Physics 2022, no. 08 (2022): 075. http://dx.doi.org/10.1088/1475-7516/2022/08/075.

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Abstract We consider two models of interacting dark energy, both of which interact only through momentum exchange. One is a phenomenological one-parameter extension to wCDM, and the other is a coupled quintessence model described by a Lagrangian formalism. Using a variety of high and low redshift data sets, we perform a global fitting of cosmological parameters and compare to ΛCDM, uncoupled quintessence, and wCDM. We find that the models are competitive with ΛCDM, even obtaining a better fit when certain data sets are included.

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45

Khalifeh, Ali Rida, and Raul Jimenez. "Distinguishing Dark Energy models with neutrino oscillations." Physics of the Dark Universe 34 (December 2021): 100897. http://dx.doi.org/10.1016/j.dark.2021.100897.

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46

Szydłowski, Marek. "Cosmological zoo—accelerating models with dark energy." Journal of Cosmology and Astroparticle Physics 2007, no. 09 (2007): 007. http://dx.doi.org/10.1088/1475-7516/2007/09/007.

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47

Vereshchagin, G. V., and G. Yegorian. "Cosmological models with Gurzadyan–Xue dark energy." Classical and Quantum Gravity 23, no. 15 (2006): 5049–61. http://dx.doi.org/10.1088/0264-9381/23/15/020.

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48

Gong, Yungui, and Chang-Kui Duan. "Constraints on alternative models to dark energy." Classical and Quantum Gravity 21, no. 15 (2004): 3655–63. http://dx.doi.org/10.1088/0264-9381/21/15/003.

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49

Jawad, Abdul, Shamaila Rani, Ines G. Salako, and Faiza Gulshan. "Pilgrim dark energy models in fractal universe." International Journal of Modern Physics D 26, no. 06 (2016): 1750049. http://dx.doi.org/10.1142/s0218271817500493.

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We discuss the cosmological implications of interacting pilgrim dark energy (PDE) models (with Hubble, Granda–Oliveros and generalized ghost cutoffs) with cold dark matter ([Formula: see text]CDM) in fractal cosmology by assuming the flat universe. We observe that the Hubble parameter lies within observational suggested ranges while deceleration parameter represents the accelerated expansion behavior of the universe. The equation of state (EoS) parameter ([Formula: see text]) corresponds to the quintessence region and phantom region for different cases of [Formula: see text]. Further, we can s

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50

Paliathanasis, Andronikos, Supriya Pan, and Weiqiang Yang. "Dynamics of nonlinear interacting dark energy models." International Journal of Modern Physics D 28, no. 12 (2019): 1950161. http://dx.doi.org/10.1142/s021827181950161x.

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We investigate the cosmological dynamics of interacting dark energy models in which the interaction function is nonlinear in terms of the energy densities. Considering explicitly the interaction between a pressureless dark matter and a scalar field, minimally coupled to Einstein gravity, we explore the dynamics of the spatially flat FLRW universe for the exponential potential of the scalar field. We perform the stability analysis for three nonlinear interaction models of our consideration through the analysis of critical points and we investigate the cosmological parameters and discuss the phy

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