Cosmological evolution of a quintom model of dark energy

Guo, Zong-Kuan; Piao, Yun-Song; Zhang, Xinmin; Zhang, Yuan‐Zhong

doi:10.1016/j.physletb.2005.01.017

Cited by 733 publications

(475 citation statements)

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“…There has also been a lot of interest in constructing quintessence models which can produce an equation of state of the "phantom" type (w φ < −1) [93][94][95][96][97][98][99][100][101][102][103][104][105][106]. Similar to natural inflation [107], it has been proposed that the flatness of the quintessnce potential could be protected by the field being a pseudo-Nambu-Goldstone boson [108,109].…”

Section: (23)mentioning

confidence: 99%

Beyond the cosmological standard model

et al. 2015

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After a decade and a half of research motivated by the accelerating universe, theory and experiment have a reached a certain level of maturity. The development of theoretical models beyond Λ or smooth dark energy, often called modified gravity, has led to broader insights into a path forward, and a host of observational and experimental tests have been developed. In this review we present the current state of the field and describe a framework for anticipating developments in the next decade. We identify the guiding principles for rigorous and consistent modifications of the standard model, and discuss the prospects for empirical tests.We begin by reviewing recent attempts to consistently modify Einstein gravity in the infrared, focusing on the notion that additional degrees of freedom introduced by the modification must "screen" themselves from local tests of gravity. We categorize screening mechanisms into three broad classes: mechanisms which become active in regions of high Newtonian potential, those in which first derivatives of the field become important, and those for which second derivatives of the field are important. Examples of the first class, such as f (R) gravity, employ the familiar chameleon or symmetron mechanisms, whereas examples of the last class are galileon and massive gravity theories, employing the Vainshtein mechanism. In each case, we describe the theories as effective theories and discuss prospects for completion in a more fundamental theory. We describe experimental tests of each class of theories, summarizing laboratory and solar system tests and describing in some detail astrophysical and cosmological tests. Finally, we discuss prospects for future tests which will be sensitive to different signatures of new physics in the gravitational sector.The review is structured so that those parts that are more relevant to theorists vs. observers/experimentalists are clearly indicated, in the hope that this will serve as a useful reference for both audiences, as well as helping those interested in bridging the gap between them.

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Section: (23)mentioning

confidence: 99%

Beyond the cosmological standard model

et al. 2015

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“…Alternative models of dark energy suggest a dynamical form of dark energy, which at least in an effective level, can originate from a variable cosmological constant [24,25], or from various fields, such as a canonical scalar field [26][27][28][29][30] (quintessence), a phantom field [31][32][33][34][35][36][37][38] or the quintom [39][40][41][42][43][44][45][46][47][48][49][50][51]. By using some basic of quantum gravitational principles, we can formulate several other models for dark energy and in literature they are known as holographic dark energy paradigm [52][53][54][55][56][57][58][59][60][61][62][63] and agegraphic dark energy models [64][65][66].…”

Section: Tachyonic Fluidmentioning

confidence: 99%

Phenomenological Fluids from Interacting Tachyonic Scalar Fields

et al. 2014

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“…Obviously, the most natural way is to consider a model with two real scalar fields. A lot of people have studied the so-called quintom model [14,15], which is a hybrid of quintessence and phantom (thus the name quintom). Naively, we consider the action…”

Section: Introductionmentioning

confidence: 99%

“…The cosmological evolution of the quintom model without direct coupling between 1 and 2 was studied in Ref. [15]. They showed that the transition from !…”

Section: Introductionmentioning

confidence: 99%

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Quintom models with an equation of state crossing−1

2006

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In this paper, we investigate a kind of special quintom model, which is made of a quintessence field 1 and a phantom field 2 , and the potential function has the form of V 2 1 ÿ 2 2 . This kind of quintom field can be separated into two kinds: the hessence model, which has the state of 2 1 > 2 2 , and the hantom model with the state 2 1 < 2 2 . We discuss the evolution of these models in the !-! 0 plane (! is the state equation of the dark energy, and ! 0 is its time derivative in units of Hubble time), and find that according to ! > ÿ1 or < ÿ 1, and the potential of the quintom being climbed up or rolled down, the !-! 0 plane can be divided into four parts. The late time attractor solution, if existing, is always quintessencelike or -like for hessence field, so the big rip does not exist. But for hantom field, its late time attractor solution can be phantomlike or -like, and sometimes, the big rip is unavoidable. Then we consider two special cases: one is the hessence field with an exponential potential, and the other is with a power law potential. We investigate their evolution in the !-! 0 plane. We also develop a theoretical method of constructing the hessence potential function directly from the effective equation-of-state function ! z . We apply our method to five kinds of parametrizations of equation-of-state parameter, where ! crossing ÿ1 can exist, and find they all can be realized. At last, we discuss the evolution of the perturbations of the quintom field, and find the perturbations of the quintom Q and the metric are all finite even at the state of ! ÿ1 and ! 0 Þ 0.

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Cosmological evolution of a quintom model of dark energy

Cited by 733 publications

References 30 publications

Beyond the cosmological standard model

Beyond the cosmological standard model

Phenomenological Fluids from Interacting Tachyonic Scalar Fields

Quintom models with an equation of state crossing−1

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