Cosmological Inflation from the dark Universe

Abstract

The present work deals with the cosmological consequences of the variable cosmological term $\Lambda (a)={\Lambda }_0+{\Lambda }_1{a}^{-r}+{\Lambda }_2{a}^{-s},$ where $a$ is the scale factor of the Robertson-Walker space-time. An analysis of the parameters ${\Lambda }_1,{\Lambda }_2,r,s$ and $\alpha ,$ which describes the interaction between the cosmological constant and non-relativistic matter/radiation, leads to an attractive density ${\rho }_{\text{dm}}\sim a^{-r}$ and a repulsive density ${\rho }_{\text{infl}}\sim a^{-s}.$ As already known from literature, an approach of the form $\Lambda (a)={\Lambda }_0+{\Lambda }_1{a}^{-r}$ and the identification of the energy density of space-time expansion with the zero-point density can avoid the scale discrepancy of the cosmological constant problem and solve the missing mass problem of dark matter. Furthermore, this works demonstrates that the additional term ${\Lambda }_2{a}^{-s}$ solves the flatness, the horizon and the magnetic-monopole problem without a hypothetical scalar field, which avoids speculations about the origin of this field. As a consequence, the imaginary time concept from Hartle and Hawking appears naturally.

References in corpus (3)

• The Case for a Positive Cosmological Lambda-term
• The Cosmological Constant
• De Sitter Space and the Swampland