Generalized DBI quintessence

Gumjudpai, Burin; Ward, John

doi:10.1103/physrevd.80.023528

Cited by 54 publications

(41 citation statements)

References 76 publications

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“…In the presence of a non-Bogomolnyi-Prasad-Sommerfield (BPS) brane or multiple D 3 -branes, the DBI action acquires an additional potential U multiplying the DBI term [49,50]. U can arise in different places within the theory.…”

Section: The New General Lagrangian Of Dbi Inflationmentioning

confidence: 99%

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The Dark Energy Properties of the Dirac–Born–Infeld Action

Zhang

Huang

2012

Entropy

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Introducing a new potential, we deduce a general Lagrangian for Dirac-BornInfeld (DBI) inflation, in which the determinant of the induced metric naturally includes the kinetic energy and the potential energy. In particular, the potential energy and kinetic energy can convert into each other at any same order, which is in agreement with the limit of classical physics. We also present a general sound speed in the evolutions of the universe, and the exact expressions of energy-momentum tensor, pressure and density. Furthermore, from the results we obtain the new equation of states. The analytic form of the action that is consistent with data turns out to be surprisingly simple and easy to categorize. Finally, we examine properties of the dark energy and introduce a novel mechanism for realizing either quintessence or phantom dark energy dominated phases within a string theoretical context.

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Section: The New General Lagrangian Of Dbi Inflationmentioning

confidence: 99%

“…For U (φ) = 1, the Equation (51) can be reduced into the Klein-Gordon equation in [49]. Let us consider the scenario by using Equations (22), (23) and the general DBI inflation Lagrangian Equation (10), we deduce the equation of states…”

Section: Dark Energy With Dbi Inflationmentioning

confidence: 99%

The Dark Energy Properties of the Dirac–Born–Infeld Action

Zhang

Huang

2012

Entropy

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“…Within the context of string theory there is a model for the early-time accelerated expansion of the Universe associated with inflation. This string-theorymotivated model for inflation is called Dirac-Born-Infield (DBI) inflation [6][7][8][9][10][11], and it is driven by the open string sector through dynamical Dp-branes. DBI inflation is a special case of K-inflation models [12].…”

mentioning

confidence: 99%

“…DBI inflation is a special case of K-inflation models [12]. It was originally thought that DBI inflation models would yield large non-Gaussian perturbations which could be used to verify or falsify these models and by extension to test string theory [11,13]. However, subsequent work has shown that this may not be the case, and that the simplest DBI models are effectively indistinguishable from standard fieldtheoretic slow-roll models of inflation [14].In the present work we examine variants of these DBI models as a mechanism, not for the early-time acceleration of inflation, but for the observed late-time accel-…”

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confidence: 99%

Dynamics of Dirac-Born-Infeld dark energy interacting with dark matter

et al. 2012

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We study the dynamics of Dirac-Born-Infeld (DBI) dark energy interacting with dark matter. The DBI dark energy model considered here has a scalar field with a nonstandard kinetic energy term, and has potential and brane tension that are power-law functions. The new feature considered here is an interaction between the DBI dark energy and dark matter through a phenomenological interaction between the DBI scalar field and the dark matter fluid. We analyze two different types of interactions between the DBI scalar field and the dark matter fluid. In particular we study the phase-space diagrams of and look for critical points of the phase space that are both stable and lead to accelerated, late-time expansion. In general we find that the interaction between the two dark components does not appear to give rise to latetime accelerated expansion. However, the interaction can make the critical points in the phase space of the system stable. Whether such stabilization occurs or not depends on the form of the interaction between the two dark components.

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“…These usually include k-essence, dilaton, DBIessence, Hessence, tachyon, Chaplygin gas, etc. [8][9][10][11][12][13][14][15][16].…”

Section: Introductionmentioning

confidence: 99%

Accretion of dark energy onto higher dimensional charged BTZ black hole

Debnath

2015

Eur. Phys. J. C

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In this work, we have studied the accretion of the (n + 2)-dimensional charged BTZ black hole (BH). The critical point and square speed of sound have been obtained. The mass of the BTZ BH has been calculated and we have observed that the mass of the BTZ BH is related with the square root of the energy density of the dark energy which accretes onto the BH in our accelerating FRW universe. We have assumed modified Chaplygin gas (MCG) as a candidate of dark energy which accretes onto the BH and we have found the expression of BTZ BH mass. Since in our solution of MCG, this model generates only quintessence dark energy (not phantom) and so BTZ BH mass increases during the whole evolution of the accelerating universe. Next we have assumed five kinds of parametrizations of well-known darkenergy models. These models generate both quintessence and phantom scenarios i.e., phantom crossing models. So if these dark energies accrete onto the BTZ BH, then in the quintessence stage, the BH mass increases up to a certain value (finite value) and then decreases to a certain finite value for the phantom stage during the whole evolution of the universe. We have shown these results graphically.

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Generalized DBI quintessence

Cited by 54 publications

References 76 publications

The Dark Energy Properties of the Dirac–Born–Infeld Action

The Dark Energy Properties of the Dirac–Born–Infeld Action

Dynamics of Dirac-Born-Infeld dark energy interacting with dark matter

Accretion of dark energy onto higher dimensional charged BTZ black hole

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