Warm inflation and its microphysical basis

Berera, Arjun; Moss, Ian G.; Ramos, Rudnei O.

doi:10.1088/0034-4885/72/2/026901

Cited by 293 publications

(462 citation statements)

References 152 publications

(341 reference statements)

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“…85 An effective field theory of dissipative inflation was constructed in [793]. Related work on warm inflation [794] is reviewed in [795] (see also [767,796]). …”

Section: Trapped Inflationmentioning

confidence: 99%

Inflation and String Theory

2015

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“…85 An effective field theory of dissipative inflation was constructed in [793]. Related work on warm inflation [794] is reviewed in [795] (see also [767,796]). …”

Section: Trapped Inflationmentioning

confidence: 99%

Inflation and String Theory

2015

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“…Therefore, warm inflation [12,13] (non-isentropic), as a * mmotaharfar2000@gmail.com † erfan.massaeli@gmail.com ‡ hr-sepangi@sbu.ac.ir complementary scenario, has been constructed to avoid such problems by introducing a supplementary viscose term having a dissipation coefficient which illustrates the rate of energy exchange between inflaton and radiation field. In fact, inflaton concurrently dissipates into radiation whereby primeval radiation will not heavily be diluted during inflation and smoothly enters the radiation era, for details see [14][15][16][17][18][19][20][21][22][23][24]. As a result, warm inflation not only inherits the features of conventional inflation but also removes disparities coming from the reheating phase and thus alleviates the initial condition [25], cures the overlarge amplitude of the inflaton field and circumvents the so-called eta-problem [26].…”

Section: Introductionmentioning

confidence: 99%

Power spectra in warm G inflation and its consistency: Stochastic approach

2017

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Recently, it has been realized that the so-called G-inflation model inspired by supplementing a generalized covariant Galileon-like non-linear derivative self-interacting term to the standard kinetic term should be ruled out from inflationary models. This is due to the fact that it suffers from lack of an oscillatory phase at the end of the inflationary regime which is typically accompanied by the appearance of a negative squared propagation speed of the scalar mode leading to instabilities of small-scale perturbations. In this regard, the warm G-inflation scenario is proposed where for G-inflation to survive, the Galileon scalar field is coupled to the radiation field through a dissipation term which results in removing the reheating period due to the characteristics of warm inflationary scenario. In so doing, a linear stability analysis is first performed to obtain the appropriate slowroll conditions in such a proposal. Cosmological perturbations of the model are then investigated by utilizing fluctuation-dissipation theorem and analytical expressions are derived for observable quantities; the power spectrum, tilt spectral index and tensor-to-scalar ratio in terms of P SR parameters and Galileon flow functions. Finally, the model is solved for chaotic self-interacting potentials, particularly the renormalizable Higgs potential λ 4 φ 4 , and shown to be consistent with observations in the weak dissipation Q 1 + 3and G-dominant 3 δ GX δ X 1 regime despite its large self-coupling, since the energy scale at the horizon crossing is depressed by the synergy of Galileon and thermal effects.

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“…Other attempts involve a mixture of a scalar field interacting with the radiation bath [18,19], as in the so-called warm inflationary model [20,21,22,23], or still based on the quantum mechanics probability of unstable states [24]. Although interesting and highly promising to understand the decaying vacuum problem in the evolving Universe, none of them can at present be considered definitive and/or widely accepted by the community.…”

Section: Introductionmentioning

confidence: 99%

Primordial gravitational waves in running vacuum cosmologies

Tamayo

Lima

Alves

et al. 2017

Astroparticle Physics

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We investigate the cosmological production of gravitational waves in a nonsingular flat cosmology powered by a "running vacuum" energy density described by ρ Λ ≡ ρ Λ (H), a phenomenological expression potentially linked with the renormalization group approach in quantum field theory in curved spacetimes. The model can be interpreted as a particular case of the class recently discussed by Perico et al. (Phys. Rev. D 88, 063531, 2013) which is termed complete in the sense that the cosmic evolution occurs between two extreme de Sitter stages (early and late time de Sitter phases). The gravitational wave equation is derived and its time-dependent part numerically integrated since the primordial de Sitter stage. The generated spectrum of gravitons is also compared with the standard calculations where an abrupt transition, from the early de Sitter to the radiation phase, is usually assumed. It is found that the stochastic background of gravitons is very similar to the one predicted by the cosmic concordance model plus inflation except at higher frequencies (ν 100 kHz). This remarkable signature of a "running vacuum" cosmology combined with the proposed high frequency gravitational wave detectors and measurements of the CMB polarization (Bmodes) may provide a new window to confront more conventional models of inflation.

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Warm inflation and its microphysical basis

Cited by 293 publications

References 152 publications

Inflation and String Theory

Inflation and String Theory

Power spectra in warm G inflation and its consistency: Stochastic approach

Primordial gravitational waves in running vacuum cosmologies

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