Higher dimensional phantom dark energy model ending at a de-Sitter phase

In this work, using a spherically symmetric metric, we investigate a minimally interacting holographic dark energy model within the framework of the Saez-Ballester Theory. We predict that the dark energy component dominating the universe is of phantom type, which will lead the model universe to cosmic doomsday (big rip singularity). As the big rip singularity and holographic dark energy are incompatible with each other, we employ a higher dimensional scenario so that the cosmic doomsday is replaced by a de-Sitter phase. The model expands with a slow and uniform change of size during the early evolution, whereas the change becomes faster and faster, agreeing with the present observation of the accelerated expansion. The present values of the Hubble parameter and the dark energy EoS parameter are found to be H = 67 and lambda = 1.00011, which agree with the respective values H-0 = 67.36 +/- 0.54 kms(- 1)Mpc(- 1)and lambda = -1.03 +/- 0.03 of the most recent Planck 2018 result.

Automated summary

In this work, a minimally interacting holographic dark energy model is investigated within the framework of the Saez-Ballester Theory, using a spherically symmetric metric. The prediction suggests that the dominant dark energy component in the universe is of phantom type, leading to cosmic doomsday. However, to resolve the incompatibility between the big rip singularity and holographic dark energy, a higher dimensional scenario is employed, replacing the cosmic doomsday with a de-Sitter phase. The model exhibits a slow and uniform change of size during early evolution, which accelerates as time progresses, consistent with current observations of accelerated expansion. The measured values of the Hubble parameter and the dark energy EoS parameter are found to be in agreement with the most recent Planck 2018 result.