Assisted inflation in Friedmann-Robertson-Walker and Bianchi spacetimes

Aguirregabiria, J. M.; Chamorro, A.; Chimento, Luis P.; Zuccalá, Norberto A.

doi:10.1103/physrevd.62.084029

Cited by 17 publications

(18 citation statements)

References 17 publications

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“…The dynamical properties of the positive exponential potentials leading to inflation in the Friedmann-Robertson-Walker (FRW) model have been widely studied [7][8][9][10][11][12][13][14][15][16][17][18][19]. 1 In the forward evolution in the expanding branch, for sufficiently flat potentials, exponential potentials yield a scaling solution which is a late time attractor [7][8][9].…”

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confidence: 99%

Nonsingular power-law and assisted inflation in loop quantum cosmology

Ranken

Singh

2012

Phys. Rev. D

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We investigate the dynamics of single and multiple scalar fields with exponential potentials, leading to power-law and assisted inflation, in loop quantum cosmology. Unlike in the classical theory, dynamical trajectories in loop quantum cosmology are generically nonsingular, with a big bounce replacing classical big bang in the Planck regime. Post bounce, after a phase of super-inflation, dynamical trajectories evolve towards the classical attractor in the inflationary scenarios. Depending on the initial conditions, bounce is shown to occur in kinetic as well as potential dominated regimes. We analyze the number of e-foldings resulting from the phase of super-inflation, and find the dependence of the maximum possible number of e-foldings on the equation of state at the bounce and on the steepness of the potential.We find that if the potential is not steep, this phase can lead to large number of e-foldings in power-law inflation. For the assisted inflation scenario, an increase in the number of fields can yield a significant increase in the number of e-foldings during super-inflation.

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confidence: 99%

Nonsingular power-law and assisted inflation in loop quantum cosmology

Ranken

Singh

2012

Phys. Rev. D

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“…We look for situations in which the dynamics allows the ratios of the individual kinetic energies of the fields to approach constant values. This situation has been studied in the literature in the context of power-law inflation and it was dubbed, assisted inflation [14,15,16,17,18,19,20,21]. It has the interesting property that the cooperative evolution of all the fields can lead to inflation even if the individual logarithmic slopes of the fields are too step to provide inflation when the fields are rolling in isolation.…”

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confidence: 99%

Dynamics of “logamediate” inflation

2007

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A computation of the inflationary observables ns and r is made for 'logamediate' inflation where the cosmological scale factor expands as a = exp(A(ln t) λ ), and is compared to their predicted values in the intermediate inflationary theory, where a = exp(Bt f ). Both versions prove to be consistent with observational measurements of the cosmic background radiation. It is shown that the dynamics of a single inflaton field can be mimicked by a system of several fields in an analogous manner to that created by the joint evolution of the fields in assisted power-law inflation.

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“…It was studied for quadratic and quartic potentials in the context of higher dimensional reduction in Ref. [7][8][9], for Bianchi models [10,11], for an ensemble of tachyon fields [12][13][14][15], in braneworld models [16,17], in particular string theory realisations [18][19][20] and taking into account Loop Quantum Cosmology corrections [21]. A multi-field dynamics was also studied in the context of Logamediate inflation [22] and k-inflation [23].…”

Section: Introductionmentioning

confidence: 99%

Multifield coupled quintessence

2014

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We study models of quintessence consisting of a number of scalar fields coupled to several dark matter components. In the case of exponential potentials the scaling solutions can be described in terms of a single field. The corresponding effective logarithmic slope and effective coupling can be written in a simple form in terms of the individual slopes and couplings of the original fields. We also investigate solutions where the scalar potential is negligible, in particular those leading to transient matter dominated solutions. Finally, we compute the evolution equations for the linear perturbations which will allow these models to be tested against current and future observational data.PACS numbers: 98.80.-k,98.80.Jk

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Assisted inflation in Friedmann-Robertson-Walker and Bianchi spacetimes

Cited by 17 publications

References 17 publications

Nonsingular power-law and assisted inflation in loop quantum cosmology

Nonsingular power-law and assisted inflation in loop quantum cosmology

Dynamics of “logamediate” inflation

Multifield coupled quintessence

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