MG15 - Talk detail

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There are various models that were proposed as scalar fields for inflation, some of these with an ‘attractor solutions’ to which the system evolves. In Universes with vanishing spatial curvature, the field variables φ and Dφ specify the system completely, defining an effective phase space. For each of these models, we have a different evolution of the energy density for relativistic matter and dark matter, which were created during the reheating period, at the end of inflation in the early Universe, as a result of the ‘inflaton’ decay. Furthermore, the temperature at which the reheating takes place also depends on the type of scalar field. In this work, we consider the polynomial scalar field (chaotic inflation) of the sixth degree, and we study it with numerical methods varying the coefficients a, b, c, obtaining the attractor behavior in particular conditions, and we compare these results with the known case of the quadratic potential. Finally, we calculate the reheating temperature, establishing, for this case, that we are in the regime of good reheating.

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