Can dark energy evolve to the phantom?

Vikman, Alexander

doi:10.1103/physrevd.71.023515

Cited by 532 publications

(569 citation statements)

References 35 publications

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“…That is, expressed in terms of the equation-of-state parameter w, the w < −1 phase must be succeeded by a w > −1 era, corresponding to the inflaton. But this crossing of the "phantom divide" is highly non-trivial, since it can lead to various unphysical effects [40]. Indeed, it seems that no model based on a single scalar field can perform this feat.…”

Section: The Global Formulation Of String Gas Spacetimesmentioning

confidence: 99%

The phantom divide in string gas cosmology

McInnes

2005

Nuclear Physics B

102

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One of the main virtues of string gas cosmology is that it resolves cosmological singularities. Since the Universe can be approximated by a locally asymptotically de Sitter spacetime by the end of the inflationary era, a singularity theorem implies that these cosmologies effectively violate the Null Energy Condition [not just the Strong Energy Condition]. We stress that this is an extremely robust result, which does not depend on assuming that the spatial sections remain precisely flat in the early Universe. This means, however, that it must be possible for string cosmologies to cross the recently much-discussed phantom divide [from w < −1 to w > −1, where w is the equation-ofstate parameter]. This naturally raises the question as to whether the phantom divide can be crossed again, to account for recent observations suggesting that w < −1 at the present time. We argue that non-perturbative string effects rule out this possibility, even if the NEC violation in question is only "effective".

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Section: The Global Formulation Of String Gas Spacetimesmentioning

confidence: 99%

The phantom divide in string gas cosmology

McInnes

2005

Nuclear Physics B

102

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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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“…If a DE evolves from one regime to another, this is called phantom crossing, but [27], e.g., showed that this is impossible for a purely kinetic k-essence. We refer to [28,29] for a discussion of phantom crossing in the context of other DE models.…”

Section: The Modelmentioning

confidence: 99%

Kinetic k-essence and quintessence

Putter

Linder

2007

Astroparticle Physics

126

113

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Dark energy models with non-canonical kinetic energy terms, k-essence, can have dynamical and sound speed properties distinct from canonical scalar fields, quintessence. Concentrating on purely kinetic term Lagrangians, which can be technically natural, we investigate limits on the equation of state dynamics and sound speed behaviors and the extent to which these models can be separated from quintessence.

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Can dark energy evolve to the phantom?

Cited by 532 publications

References 35 publications

The phantom divide in string gas cosmology

The phantom divide in string gas cosmology

Beyond the cosmological standard model

Kinetic k-essence and quintessence

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