Inflation from a tachyon fluid?

Fairbairn, Malcolm; Tytgat, Michel H. G.

doi:10.1016/s0370-2693(02)02638-2

Cited by 249 publications

(218 citation statements)

References 28 publications

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“…In case of no codimension, we are dealing with a cosmological setting, all possible "energy release" takes the form of deforming the background metric in an uniform way. Besides, due to the form of the tachyon potential, it is difficult to get reheating in the rolling-tachyon driven inflation scenario [11]. If there is no transverse direction, the reheating problem remains.…”

Section: Resultsmentioning

confidence: 99%

“…After integrating out the k 0 we get 10) and choose the spherical polar coordinates such that 11) and k · x = kr cos θ . (3.12) Then the Green's function becomes…”

Section: Instantaneous Radiation Powermentioning

confidence: 99%

“…For 0 < n < 3 the brane curves the transverse directions, so the asymptotic consideration will break down, one may follow the treatment in [10] for the cases with one or two transverse directions. For n = 0 there is no transverse directions, instead one can follow the consideration of the tachyon cosmology [5,11] where the rolling tachyon matters act as the source to the evolution of the background geometry.…”

Section: Jhep11(2002)050mentioning

confidence: 99%

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Gravitational Radiation of Rolling Tachyon

Chen

Lin

2002

J. High Energy Phys.

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In this paper we compute the radiation of the massless closed string states due to the non-vanishing coupling to the rolling open string tachyon with co-dimensions larger than 2, and discuss the effect of back reaction to the motion of the rolling tachyon. We find that for small string coupling, the tachyonic matter remains in the late time, but it will completely evaporate away over a short time of few string scales if the string coupling is huge. Comment on the implication of our results to the g-theorem of boundary conformal field theory is given.

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Section: Resultsmentioning

confidence: 99%

“…After integrating out the k 0 we get 10) and choose the spherical polar coordinates such that 11) and k · x = kr cos θ . (3.12) Then the Green's function becomes…”

Section: Instantaneous Radiation Powermentioning

confidence: 99%

Section: Jhep11(2002)050mentioning

confidence: 99%

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Gravitational Radiation of Rolling Tachyon

Chen

Lin

2002

J. High Energy Phys.

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“…(3.22), i.e., 6) and the scalar spectral index from Eq. (3.16) reads p. Fig.10 shows the variation of the scalar spectral index n s versus the number of e-folds for different values of the conformal anomaly coefficient for α = 0.6 × 10 −5m p and for r = 0.08.…”

Section: Exponential Potentialmentioning

confidence: 99%

Constraints on tachyon inflationary models with an AdS/CFT correspondence

et al. 2016

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In order to study the effect of the anti de Sitter/ conformal field theory correspondence (AdS/CFT) on the primordial inflationary era, we consider a universe filled with a tachyon field in a slow-roll regime. In this context, the background and perturbative parameters characterising the inflationary era are related to the standard one by correction terms. We show a clear agreement between the theoretical prediction and the observational data for the above mentioned model. The main results of our work are illustrated for an exponential potential. We show that, for a suitable conformal anomaly coefficient, AdS/CFT correspondence might leave its imprints on the spectrum of the gravitational waves amplitude with a tensor to scalar ratio, r, of the perturbations compatible with Planck data.

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“…One reason is that the tachyon field perturbations around the unstable vacuum must contain an unstable mode whose (negative) eigenvalue is the tachyon mass squared, which is of order the string scale. This leads to an η-problem in tachyonic inflation [6,11].…”

Section: Introductionmentioning

confidence: 99%

Perturbations and moduli space dynamics of tachyon kinks

Hindmarsh

2008

Phys. Rev. D

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The dynamic process of unstable D-branes decaying into stable ones with one dimension lower can be described by a tachyon field with a Dirac-Born-Infeld effective action. In this paper we investigate the fluctuation modes of the tachyon field around a two-parameter family of static solutions representing an array of brane-antibrane pairs. Besides a pair of zero modes associated with the parameters of the solution, and instabilities associated with annihilation of the brane-antibrane pairs, we find states corresponding to excitations of the tachyon field around the brane and in the bulk. In the limit that the brane thickness tends to zero, the support of the eigenmodes is limited to the brane, consistent with the idea that propagating tachyon modes drop out of the spectrum as the tachyon field approaches its ground state. The zero modes, and other low-lying excited states, show a 4-fold degeneracy in this limit, which can be identified with some of the massless superstring modes in the brane-antibrane system. Finally, we also discuss the slow motion of the solution corresponding to the decay process in the moduli space, finding a trajectory which oscillates periodically between the unstable D-brane and the brane-antibrane pairs of one dimension lower.

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Inflation from a tachyon fluid?

Cited by 249 publications

References 28 publications

Gravitational Radiation of Rolling Tachyon

Gravitational Radiation of Rolling Tachyon

Constraints on tachyon inflationary models with an AdS/CFT correspondence

Perturbations and moduli space dynamics of tachyon kinks

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