Parâmetros observáveis de inflação em modelos de inflação caótica

Abstract

Although the Hot Big Bang Theory (HBBT) in the context of Λ CDM, has great success in describing our universe, it still shows a series of gaps that needs to be fulfilled, which denotestheneedforamodificationofthetheory. Amongthesedifficulties,wecanhighlight the horizon problem, the flatness problem, and the relic particles problem, predicted by great unification models (GUT), which we have never been able to detect until today. Seeking to solve these problems, Alam Guth proposed the concept of inflation, the idea that the universe, in its first seconds of life, has undergone an exponential expansion. This mechanism would not only solve the above mentioned problems, but would also provide an explanation for the appearance of the small fluctuations observed in the CMB by the COBE, WMAP and PLANCK satellites, whose most recent results impose constraints on the tensor-scalar ratio and the spectral scalar index ns, which allows us to discard models inflation. But Guth’s model is not adequate, presenting several problems. Thus, Andrei Linde proposes a new inflation scenario, which is based on a slow evolution of a φ (Slow-Roll) field that would perform the role of the inflaton, to equilibrium point φ0. this model solves many of the inconveniences arising from the scenario proposed by Guth and makes it possible to establish an infinite number of potentials capable of playing the role of a cosmological constant that can be tested in light of the most recent experimental constraints obtained by the PLANCK mission. Initially chaotic potentials in the form V(φ) = λφn nMn−4 p , were considered excellent candidates for inflationary models, but only for n=1 they provide us with results compatible with the experimental constraints for the parameters r < 0.11 and ns ∼1, showing that they still need adjustments (possibly radioactive corrections) to correctly describe the data observed by PLANCK.