Scalar perturbation spectra from warm inflation

Hall, Lisa M.; Moss, Ian G.; Berera, Arjun

doi:10.1103/physrevd.69.083525

Cited by 290 publications

(561 citation statements)

References 52 publications

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“…These effects will alter predictions for density perturbations. In fact, as shown in [29] temperature dependent effects could introduce qualitatively new features to the scalar power spectrum, such as oscillations. Thus a more accurate treatment of density perturbations and a thorough examination of their evolution is important to consider in future work.…”

Section: Discussionmentioning

confidence: 99%

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Determining the regimes of cold and warm inflation in the supersymmetric hybrid model

Bastero-Gil

Berera

2005

Phys. Rev. D

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The SUSY hybrid inflation model is found to dissipate radiation during the inflationary period. Analysis is made of parameter regimes in which these dissipative effects are significant. The scalar spectral index, its running, and the tensor-scalar ratio are computed in the entire parameter range of the model. A clear prediction for strong dissipative warm inflation is found for nS − 1 ≃ 0.98 and a low tensor-scalar ratio much below 10 −6 . The strong dissipative warm inflation regime also is found to have no η-problem and the field amplitude much below the Planck scale. As will be discussed, this has important theoretical implications in permitting a much wider variety of SUGRA extensions to the basic model.

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Section: Discussionmentioning

confidence: 99%

“…Given the different "thermal" origin of spectrum, the spectral index also changes with respect to the cold inflationary scenario [28,29,30,31], even in the weak dissipative warm inflation regime when the evolution of the inflaton field is practically unchanged. Again, for the different regimes, it is obtained:…”

Section: Dissipative Dynamics During Inflationmentioning

confidence: 99%

Determining the regimes of cold and warm inflation in the supersymmetric hybrid model

Bastero-Gil

Berera

2005

Phys. Rev. D

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“…Hall, Moss and Berera [9] have calculated the spectral index in warm inflation for the strong dissipative regime with Q >> 1 or Γ >> 3H. We shall here follow Visinelli [47] and permit arbitrary values of Q. Differentiating the first of the Equation (3.4) and using Equation (3.6) gives…”

Section: Optical Parameters In Warm Inflationmentioning

confidence: 99%

“…Introductions to warm inflation models and references to works prior to 2009 on warm inflation are found in [8] and [23]. 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%

“…This produces heat and viscosity, which make the inflationary phase last longer. Warm inflation models were introduced and developed by Berera and coworkers [1][2][3][4][5][6][7][8][9][10][11][12][13][14]. However, even earlier inflation models with dissipation of inflaton energy to radiation and particles had been considered [15][16][17][18][19][20][21][22].…”

Section: Introductionmentioning

confidence: 99%

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Warm Inflation

Grøn

2016

Universe

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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.

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Numerical analysis of magnetogenesis' primordial mechanism

Garrison

2019

Astron Nachr

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We present the results of Relativistic Magnetohydrodynamic simulations utilizing initial conditions from both the Electroweak and quantum chromodynamics phase transitions to see if seed magnetic fields may be generated via the Biermann battery mechanism of magnetogensis. These simulations occur in a simulated early universe between 10 −11 s and 10 -3 s after the Big Bang. We find that magnetic fields on the order of 10 −19 G are generated on small scales and magnetic fields of 10 −25 G are generated on the Mpc scale. Further work is needed to understand how these fields may have impacted the large-scale structures we observe today. KEYWORDSBiermann battery -magnetogenesis -phase transition -relativistic plasma 1

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Scalar perturbation spectra from warm inflation

Cited by 290 publications

References 52 publications

Determining the regimes of cold and warm inflation in the supersymmetric hybrid model

Determining the regimes of cold and warm inflation in the supersymmetric hybrid model

Warm Inflation

Numerical analysis of magnetogenesis' primordial mechanism

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