Effective field theory for neutron stars with WIMPS in the pc‐GR formalism

Abstract

The field equations of the pseudo‐complex general relativity (pc‐GR) have an extra term, of repulsive character, which may halt the gravitational attractive collapse of matter distributions in the evolution process of compact stars. This additional term simulates the presence of dark energy in the Universe. In this paper, we explore the presence of this additional term and study the role of dark energy in the structure of neutron stars composed by nucleons, hyperons, mesons, and weakly interacting massive fermion dark matter particles (WIMPs) held together by the nuclear force and the gravitational interaction superimposed on the repulsive background of dark energy. To describe the hadron–lepton sector, we consider three different effective models, Zimanyi–Moszkowski, Boguta–Bodmer, and the analytic parameterized coupling model, which we extend to consider, in the baryonic sector, the presence of the whole fundamental baryon octet. By solving the Tolman‐Oppenheimer‐Volkoff (TOV) equations, we estimate the maximum gravitational mass of neutron stars.