Mass density perturbations from inflation with thermal dissipation

Lee, Wolung; Fang, Li

doi:10.1103/physrevd.59.083503

Cited by 38 publications

(26 citation statements)

References 26 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…More accurate treatments of density perturbations have followed [30,32,33,34,35], which use the cosmological perturbation equations. Following our recent results [39], working in the zero-shear gauge with perturbed metric…”

Section: Observational Testsmentioning

confidence: 99%

“…In [29] an order of magnitude estimate of density perturbations during warm inflation was computed by matching the thermally produced fluctuations to gauge invariant parameters when the fluctuations cross the horizon (for other phenomenological treatments of warm inflation see [30,31,32,33,34,35]). This work provided a clear statement of the consistency condition.…”

Section: Observational Testsmentioning

confidence: 99%

See 1 more Smart Citation

Warm inflation solution to the eta problem

Berera¹

2003

Proceedings of International Workshop on Astroparticle and High Energy Physics — PoS(AHEP2003)

View full text Add to dashboard Cite

Warm inflationary dynamics is shown to satisfy both the slow-roll and density perturbation constraints for m φ H or equivalently η 1 and for inflaton field amplitudes much below the Planck scale, φ < m pl . I start by reviewing the two types of inflation dynamics, isentropic or cold inflation and nonisentropic or warm inflation.In the former, inflation occurs without radiation production, whereas in the latter both radiation production and inflation occur concurrently. I then discuss recent, detailed, quantum field theory calculations showing that many generic inflation models, including hybrid inflation, which were believed only to have cold inflation regimes, in fact have regimes of both warm and cold inflation. These results dispel many foregone assumptions generally made up to now about inflation models and bring to the fore various elementary issues that must be addressed to do reliable calculations from inflation models. I also discuss density perturbations and observational consequences of warm inflation, especially related to WMAP. Finally I show that warm inflation has intrinsic features that make the "eta problem" nonexistent, and field amplitudes are below the Planck scale.

show abstract

Section: Observational Testsmentioning

confidence: 99%

Section: Observational Testsmentioning

confidence: 99%

Warm inflation solution to the eta problem

Berera¹

2003

Proceedings of International Workshop on Astroparticle and High Energy Physics — PoS(AHEP2003)

View full text Add to dashboard Cite

show abstract

“…This technique should be good for order of magnitude estimates. For more accurate treatment of the density perturbations it is nessesary to use the cosmological perturbation equations, which can be found in the literature [28,29,30].…”

Section: Introductionmentioning

confidence: 99%

Scalar perturbation spectra from warm inflation

2004

View full text Add to dashboard Cite

We present a numerical integration of the cosmological scalar perturbation equations in warm inflation. The initial conditions are provided by a discussion of the thermal fluctuations of an inflaton field and thermal radiation using a combination of thermal field theory and thermodynamics. The perturbation equations include the effects of a damping coefficient Γ and a thermodynamic potential V . We give an analytic expression for the spectral index of scalar fluctuations in terms of a new slow-roll parameter constructed from Γ. A series of toy models, inspired by spontaneous symmetry breaking and a known form of the damping coefficient, lead to a spectrum with ns > 1 on large scales and ns < 1 on small scales.

show abstract

“…For later works, see [9] and [24] and references in these articles. Further developments are found in the articles [25][26][27][28][29][30][31][32][33][34][35][36][37][38][39][40][41][42][43].…”

Section: Introductionmentioning

confidence: 99%

Warm Inflation

Grøn

2016

Universe

View full text Add to dashboard Cite

I show here that there are some interesting differences between the predictions of warm and cold inflation models focusing in particular upon the scalar spectral index n s and the tensor-to-scalar ratio r. The first thing to be noted is that the warm inflation models in general predict a vanishingly small value of r. Cold inflationary models with the potential V = M 4 (φ/M P ) p and a number of e-folds N = 60 predict δ nsC ≡ 1 − n s ≈ (p + 2) /120, where n s is the scalar spectral index, while the corresponding warm inflation models with constant value of the dissipation parameter Γ predict δ nsW = [(20 + p) / (4 + p)] /120. For example, for p = 2 this gives δ nsW = 1.1δ nsC . The warm polynomial model with Γ = V seems to be in conflict with the Planck data. However, the warm natural inflation model can be adjusted to be in agreement with the Planck data. It has, however, more adjustable parameters in the expressions for the spectral parameters than the corresponding cold inflation model, and is hence a weaker model with less predictive force. However, it should be noted that the warm inflation models take into account physical processes such as dissipation of inflaton energy to radiation energy, which is neglected in the cold inflationary models.

show abstract

Mass density perturbations from inflation with thermal dissipation

Cited by 38 publications

References 26 publications

Warm inflation solution to the eta problem

Warm inflation solution to the eta problem

Scalar perturbation spectra from warm inflation

Warm Inflation

Contact Info

Product

Resources

About