“…--HTML-->In this talk, we discuss the significance for inflation of the Swampland Distance Conjecture, a proposal for a quantum gravity constraint acting at infinite distances.…”
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“…All the different wavelengths can be initialized on the same space-like hypersurface at the onset of inflation but this strategy and the related conclusions are plausible only for classical inhomogeneities. …”
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“…We single out the Starobinsky model and its extensions among generic <math altimg="si1.svg"><mi>f</mi><mo stretchy="false">(</mo><mi>R</mi><mo stretchy="false">)</mo></math> gravity as attractors at large field values for chaotic inflation. Treating a <math altimg="si2.svg"><msup><mrow><mi>R</mi></mrow><mrow><mn>3</mn></mrow></msup></math> curvature term as a perturbation of the Starobinsky model, we impose the phenomenological bounds on the additional term satisfying the successful inflationary predictions. …”
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“…We propose a non-oscillatory no-scale supergravity model of inflation (NO-NO inflation) in which the inflaton does not oscillate at the end of the inflationary era. …”
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“…Afterwards, with a super-Planckian field value at the global minimum, the inflation commences at a false vacuum region lying between true vacuum regions and hence the name “topological inflation.” …”
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“…While such positivity bounds have been applied in a wide array of physical contexts to obtain useful constraints, their application to inflationary EFTs is subtle since Lorentz invariance is spontaneously broken during cosmic inflation. One path forward is to employ a Breit parameterization to ensure a crossing-symmetric and analytic S-matrix in theories with broken boosts. …”
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“…We compute the rate with which super-Hubble cosmologicalfluctuations are decohered during inflation, by their gravitationalinteractions with unobserved shorter-wavelength scalar and tensormodes. …”
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“…We apply these techniques to two different scenarios: 1. Warm inflation, for which we compute the inflationary CMB observables of several models. …”
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“…The prototype hybrid SUSY SU(5) inflation models, while well motivated from particle physics, and while allowing an acceptable inflationary phase with little or no fine tuning, are shown to have two fundamental phenomenological problems. (1) They inevitably result in the wrong vacuum after inflation is over; and (2) they do not solve the monopole problem. …”
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“…In this talk I will concentrate on the preheating part, putting emphasis on the differences between preheating in chaotic and in hybrid inflation.…”
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“…We consider the possibility that higher-curvature corrections in some variant of $M$ theory could drive inflation after the compactification to four dimensions. …”
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“…We consider vacuum quantum effects in the Early Universe, which may lead to inflation. The inflation is a direct consequence of the supposition that, at high energies, all the particles can be described by the weakly interacting, massless, conformally invariant fields. …”
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“…The Davis Meeting on Cosmic Inflation marked an exciting milestone on the road to precision cosmology. …”
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“…In quintessential inflationary model, the same master field that drives inflation becomes, later on, the dynamical source of the (present) accelerated expansion. …”
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“…In this lecture I will review the present status of inflation within string-based brane-world scenarios. …”
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