Running vacuum and H^4-inflation
Joan Sol`a Peracaula, Cristian Moreno-Pulido, Alex Gonz’alez-Fuentes
arXiv:2503.01041v2 Announce Type: replace-cross
Abstract: Recent studies of QFT in cosmological spacetime indicate that the speeding up of the present universe may not just be associated with a rigid cosmological term but with a running one that evolves with the expansion rate: $Lambda=Lambda(H)$. This running is inherited from the cosmic evolution of the vacuum energy density (VED), $rho_{rm vac}$, which is sensitive to quantum effects in curved spacetime that ultimately trigger that running. The VED is a function of the Hubble rate and its time derivatives: $rho_{rm vac}=rho_{rm vac}(H, dot{H},ddot{H},…)$. Two nearby points of the cosmic evolution during the FLRW epoch are smoothly related as $deltarho_{rm vac}sim {cal O}(H^2)$. In the very early universe, in contrast, the higher powers of the Hubble rate take over and bring about a period of fast inflation. They originate from quantum effects on the effective action of vacuum, which we compute. Herein we focus on the lowest possible power for inflation to occur: $H^4$. During the inflationary phase, $H$ remains approximately constant and very large. Subsequently, the universe enters the usual FLRW radiation epoch. This new mechanism (`RVM-inflation’) is not based on any supplementary `inflaton’ field, it is fueled by pure QFT effects on the dynamical background and is different from Starobinsky’s inflation, in which $H$ is never constant.arXiv:2503.01041v2 Announce Type: replace-cross
Abstract: Recent studies of QFT in cosmological spacetime indicate that the speeding up of the present universe may not just be associated with a rigid cosmological term but with a running one that evolves with the expansion rate: $Lambda=Lambda(H)$. This running is inherited from the cosmic evolution of the vacuum energy density (VED), $rho_{rm vac}$, which is sensitive to quantum effects in curved spacetime that ultimately trigger that running. The VED is a function of the Hubble rate and its time derivatives: $rho_{rm vac}=rho_{rm vac}(H, dot{H},ddot{H},…)$. Two nearby points of the cosmic evolution during the FLRW epoch are smoothly related as $deltarho_{rm vac}sim {cal O}(H^2)$. In the very early universe, in contrast, the higher powers of the Hubble rate take over and bring about a period of fast inflation. They originate from quantum effects on the effective action of vacuum, which we compute. Herein we focus on the lowest possible power for inflation to occur: $H^4$. During the inflationary phase, $H$ remains approximately constant and very large. Subsequently, the universe enters the usual FLRW radiation epoch. This new mechanism (`RVM-inflation’) is not based on any supplementary `inflaton’ field, it is fueled by pure QFT effects on the dynamical background and is different from Starobinsky’s inflation, in which $H$ is never constant.