Inflationary de Sitter solutions from superstrings

TL;DR

This paper demonstrates the existence of new inflationary solutions in superstring compactifications with broken supersymmetry, where key cosmological parameters remain constant during evolution, driven by special moduli fields.

Contribution

It introduces novel inflationary solutions within superstring theories involving specific moduli fields and shows how these solutions are dynamically generated and connected to phase transitions.

Findings

Existence of inflationary solutions with constant am and aT

Presence of special moduli fields influencing cosmological evolution

Different phase transition scenarios connecting inflation to other cosmological phases

Abstract

In the framework of superstring compactifications with N=1 supersymmetry spontaneously broken, (by either geometrical fluxes, branes or else), we show the existence of new inflationary solutions. The time-trajectory of the scale factor of the metric a, the supersymmetry breaking scale m=m(Phi) and the temperature T are such that am and aT remain constant. These solutions request the presence of special moduli-fields: i) The universal "no-scale-modulus" Phi, which appears in all N=1 effective supergravity theories and defines the supersymmetry breaking scale m(Phi). ii) The modulus Phi_s, which appears in a very large class of string compactifications and has a Phi-dependent kinetic term. During the time evolution, a^4 rho_s remains constant as well, (rho_s being the energy density induced by the motion of Phi_s). The cosmological term Lambda(am), the curvature term k(am, aT) and the radiation term c_R=a^4 rho are dynamically generated in a controllable way by radiative and temperature corrections; they are effectively constant during the time evolution. Depending on Lambda, k and c_R, either a first or second order phase transition can occur in the cosmological scenario. In the first case, an instantonic Euclidean solution exists and connects via tunneling the inflationary evolution to another cosmological branch. The latter starts with a big bang and, in the case the transition does not occur, ends with a big crunch. In the second case, the big bang and the inflationary phase are smoothly connected.