Kinetic k-essence ghost dark energy model

Rozas-Fernández, Alberto

doi:10.1016/j.physletb.2012.02.030

Cited by 65 publications

(37 citation statements)

References 141 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…(21) were previously postulated in [43,44] (admittedly, with very little understanding of what is behind this formula 3 ) to describe the dark energy as a result of the QCD dynamics. Most importantly, this postulate has been (successfully) confronted with observations; see [48][49][50][51][52][53][54][55][56] and many references therein, where it has been claimed that this model is consistent with all presently available data. 4 Our second comment is as follows.…”

Section: B Inflationary De Sitter Phasementioning

confidence: 99%

“…(21) [which eventually leads to the de Sitter behavior (33)] has been postulated as the driving force for the dark energy; see footnotes 3 and 4 for some comments. The model has been (successfully) confronted with observations; see [48][49][50][51][52][53][54][55][56] and many references therein, where it has been claimed that this proposal is consistent with all presently available data. Our comment here is that history of the evolution of the Universe may repeat itself by realizing the de Sitter behavior twice in its history.…”

Section: Related Effectsmentioning

confidence: 99%

See 1 more Smart Citation

Inflaton as an auxiliary topological field in a QCD-like system

Zhitnitsky

2014

Phys. Rev. D

View full text Add to dashboard Cite

We propose a new scenario for early cosmology, where inflationary de Sitter phase dynamically occurs. The effect emerges as a result of dynamics of the topologically nontrivial sectors in expanding universe. Technically the effect can be described in terms of the auxiliary fields which effectively describe the dynamics of the topological sectors in a gauge theory. Inflaton in this framework is an auxiliary topological non-propagating field with no canonical kinetic term, similar to known topologically ordered phases in condensed matter systems. We explain many deep questions in this framework using the so-called weakly coupled "deformed QCD" toy model.While this theory is weakly coupled gauge theory, it preserves all the crucial elements of strongly interacting gauge theory, including confinement, nontrivial $\theta$ dependence, degeneracy of the topological sectors, etc. We discuss a specific realization of these ideas using a scaled up version of QCD, coined as \qcd, with the scale M_{PL}\gg \Lbar\gg \sqrt[3]{M_{EW}^2M_{PL}}\sim 10^8 {\mathrm{GeV}}. If no other fields are present in the system de Sitter phase will be the final destination of evolution of the universe. If other interactions are present in the system, the inflationary de Sitter phase lasts for a finite period of time. The inflation starts from the thermal equilibrium state long after the \qcd -confinement phase transition at temperature T_{i}\sim \Lbar\sqrt{\frac{\Lbar}{M_{PL}}}. The end of inflation is triggered by the coupling with gauge bosons from the Standard Model. The corresponding interaction is unambiguously fixed by the triangle anomaly. Number of e-folds in the \qcd-inflation framework is determined by the gauge coupling constant at the moment of inflation, and estimated as N_{\rm inf}\sim \alpha_s^{-2}\sim 10^2.Comment: new references and comment

show abstract

Section: B Inflationary De Sitter Phasementioning

confidence: 99%

Section: Related Effectsmentioning

confidence: 99%

Inflaton as an auxiliary topological field in a QCD-like system

Zhitnitsky

2014

Phys. Rev. D

View full text Add to dashboard Cite

show abstract

“…79 Combining Eqs. (59) and (60) with the time derivative of Friedmann equation (9), and using the time derivative of Eq. (47) leads to…”

Section: Thermodynamical Description Of the Interacting Ggdementioning

confidence: 99%

Thermodynamical description of the ghost dark energy model

Honarvaryan

Sheykhi

Moradpour

2015

Int. J. Mod. Phys. D

View full text Add to dashboard Cite

In this paper, we point out thermodynamical description of ghost dark energy and its generalization to the early universe. Thereinafter, we find expressions for the entropy changes of these dark energy candidates. In addition, considering thermal fluctuations, thermodynamics of the dark energy component interacting with a dark matter sector is addressed. {We will also find the effects of considering the coincidence problem on the mutual interaction between the dark sectors, and thus the equation of state parameter of dark energy.} Finally, we derive a relation between the mutual interaction of the dark components of the universe, accelerated with the either ghost dark energy or its generalization, and the thermodynamic fluctuations.Comment: 11 page

show abstract

“…It is also investigated that this model also helps in alleviating two major problems of DE called fine tuning and cosmic coincidence problem [27][28][29][30][31]34]. Many authors have investigated/tested this model through different cosmological parameters theoretically [35][36][37][38][39] and different observational schemes [40].…”

Section: Non-flat Frw Universe and Basic Equationsmentioning

confidence: 99%

Analysis of generalized ghost pilgrim dark energy in non-flat FRW universe

Jawad

2014

Eur. Phys. J. C

View full text Add to dashboard Cite

This work is based on pilgrim dark energy conjecture which states that phantom-like dark energy possesses the enough resistive force to preclude the formation of black hole. The non-flat geometry is considered which contains the interacting generalized ghost pilgrim dark energy with cold dark matter. Some well-known cosmological parameters (evolution parameter (ω ) and squared speed of sound) and planes (ω -ω and statefinder) are constructed in this scenario. The discussion of these parameters is totally done through pilgrim dark energy parameter (u) and interacting parameter (d 2 ). It is interesting to mention here that the analysis of evolution parameter supports the conjecture of pilgrim dark energy. Also, this model remains stable against small perturbation in most of the cases of u and d 2 . Further, the cosmological planes correspond to CDM limit as well as different well-known dark energy models.

show abstract

Kinetic k-essence ghost dark energy model

Cited by 65 publications

References 141 publications

Inflaton as an auxiliary topological field in a QCD-like system

Inflaton as an auxiliary topological field in a QCD-like system

Thermodynamical description of the ghost dark energy model

Analysis of generalized ghost pilgrim dark energy in non-flat FRW universe

Contact Info

Product

Resources

About