<i>SO</i>
                    (1, 1) dark energy model and the universe transition

Wei, Yi-Huan; Tian, Yu

doi:10.1088/0264-9381/21/23/004

Cited by 63 publications

(32 citation statements)

References 56 publications

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“…This accelerated expansion of the universe was confirmed by the observations such as type I supernovae (SNeIa) [5][6][7], Sloan Digital Sky Survey [8], and Wilkinson Microwave Anisotropic Probe (WMAP) [9][10][11]. In the light of these observations, depending on the ideas of dark energy, cosmologist proposed many candidate for dark energy such as cosmological constant, quintessence [12][13], phantom [14][15], quintom [16][17], tachyons field [18][19], Chaplygin gas models [20][21] dark energy models. The cosmological constant candidate suffers from two well known problems namely the fine tuning and the cosmic coincident problems [22].…”

Section: Introductionmentioning

confidence: 86%

LRS Bianchi Type I Cosmological Models with Perfect Fluid and Dark Energy in Bimetric Theory of Gravitation

Borkar¹,

Charjan²,

Lepse³

2014

IOSRJM

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Section: Introductionmentioning

confidence: 86%

LRS Bianchi Type I Cosmological Models with Perfect Fluid and Dark Energy in Bimetric Theory of Gravitation

Borkar¹,

Charjan²,

Lepse³

2014

IOSRJM

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“…Here, we consider the case of time-dependent w X . Treating it as the approximate expression to a for a changing w X , then we conjecture for γ X = −W t −n with W > 0 and n > 1 two constants, |γ X t| = W t 1−n decreases with time so that the universe, as pointed out in [23], may escape future Big Rip.…”

mentioning

confidence: 84%

“…For late time, the matter density is much smaller than phantom energy density and equations (6)- (11) given in Ref. [23] reduce to…”

mentioning

confidence: 99%

Late-Time Phantom Universe in So(1, 1) Dark Energy Model With Exponential Potential

Wei

2005

Mod. Phys. Lett. A

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We discuss the late-time property of universe and phantom field in the SO(1, 1) dark energy model for the potential V = V 0 e −βΦ α with α and β two positive constants. We assume in advance some conditions satisfied by the late-time field to simplify equations, which are confirmed to be correct from the eventual results. For α < 2, the filed falls exponentially off and the phantom equation of state rapidly approaches −1. When α = 2, the kinetic energy ρ k and the coupling energy ρ c become comparable but there is always ρ k < −ρ c so that the phantom property of field proceeds to hold. The analysis on the perturbation to the late-time field Φ illustrates the square effective mass of the perturbation field is always positive and thus the phantom is stable. The universe considered currently may evade the future sudden singularity and will evolve to de Sitter expansion phase.

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“…Within the description of dark energy in terms of the EOS as defined in the preceding paragraph, it is possible to address a problem which has recently drawn a lot of attention of researchers in both observational [20] and theoretical cosmology [21,22,23,24,25,26,27]: a possible dark energy transition between quintessence and phantom regimes. The analyses of various cosmological data sets [20] mildly favor the evolution of the dark energy parameter of EOS from w > −1 to w < −1 at small redshift.…”

mentioning

confidence: 99%

“…A number of theoretical studies of the crossing of CC boundary have been undertaken so far. The approach of [21,22] (see also [23]) models the dark energy in terms of two fields, of which one is of quintessence and the other of phantom type. An interesting phenomenological model of oscillatory parameter w, named quintom [24], exhibits very interesting features in the evolution of the universe.…”

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confidence: 99%

Dark energy transition between quintessence and phantom regimes: An equation of state analysis

Štefančić

2005

Phys. Rev. D

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The dark energy transition between quintessence (w > −1) and phantom (w < −1) regimes (the crossing of the cosmological constant boundary) is studied using the dark energy equation of state. Models characterized by this type of transition are explicitly constructed and their equation of state is found to be implicitly defined. The behavior of the more general models with the implicitly defined equation of state, obtained by the generalization of the explicitly constructed models, is studied to gain insight into the necessary conditions for the occurrence of the transition, as well as to investigate the mechanism behind the transition. It is found that the parameters of the generalized models need to satisfy special conditions for the transition to happen and that the mechanism behind the transition is the cancellation of the contribution of the cosmological constant boundary. The aspects of the behavior of the generalized models which are not related to the transition are briefly discussed and the role of the implicitly defined dark energy equation of state in the description of the dark energy evolution is emphasized. One of the most important aspects of the present universe is its accelerated expansion. Numerous and complementary cosmological observations such as supernovae of the type Ia (SNIa) [1], the anisotropies of the cosmic microwave background radiation (CMBR) [2], large scale structure (LSS) [3], and others seem to reconfirm this characteristic of the small-redshift evolution of the universe with the arrival of each new set of cosmological data. Although the present acceleration of the universe expansion is well established observationally, the nature of the cause of the cosmic acceleration is much more uncertain. A large number of models assume the existence of the component of the universe with the negative pressure, named dark energy [4], which at late times dominates the total energy density of the universe and accelerates its expansion. Models of dark energy differ with respect to the size of the parameter w = p d /ρ d (p d and ρ d are the pressure and energy density of dark energy, respectively 1 ) of their equation of state (EOS) as well as the variation of the parameter w with redshift or cosmic time. The cosmological constant (CC), with w = −1, occupies the central place among the dark energy models, both in theoretical considerations and in data analysis [5]. The conceptual difficulties in the understanding of the measured size of the CC and its relation to other cosmological parameters motivated the study of the dynami- * On leave of absence from the Theoretical Physics Division, Rudjer Bošković Institute, Zagreb, Croatia. † Electronic address: stefancic@ecm.ub.es 1 Since only the dark energy component of the universe will be discussed furtheron, in the remainder of the paper the subscript d will be dropped.cal models of CC (such as renormalization group running models of CC and other relevant cosmological parameters [6,7,8,9]) and dynamical models of dark energy in general. The models of d...

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SO (1, 1) dark energy model and the universe transition

Cited by 63 publications

References 56 publications

LRS Bianchi Type I Cosmological Models with Perfect Fluid and Dark Energy in Bimetric Theory of Gravitation

LRS Bianchi Type I Cosmological Models with Perfect Fluid and Dark Energy in Bimetric Theory of Gravitation

Late-Time Phantom Universe in So(1, 1) Dark Energy Model With Exponential Potential

Dark energy transition between quintessence and phantom regimes: An equation of state analysis

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