The properties of neutron stars within the theory of pseudo-complex general relativity are studied. The pc-Tolman-Oppenheimer-Volkoff equations are numerically integrated in order to understand the structure of these objects. The interior Λ-term energy density ε Λi has been linearly coupled to the respective baryonic quantity ε m . Two models for the exterior region have been analyzed attending the continuity of the energy density at the boundary. Energy conditions have been studied for both regions. Solutions have been presented for different values of the coupling parameter. It is shown that accumulation of the Λ-term component allows the theoretical existence of larger and more massive neutron stars.

Applying semi-classical Quantum Mechanics, the vacuum fluctuations within a star are determined, assuming a constant mass density and applying a monopole approximation. It is found that the density for the vacuum fluctuations does not only depend linearly on the mass density, as assumed in a former publication, where neutron stars up to 6 solar masses were obtained. This is used to propose a simple model on the dependence of the dark energy to the mass density, as a function of the radial distance r. It is shown that stars with up to 200 solar masses can, in principle, be obtained. Though, we use a simple model, it shows that in the presence of vacuum fluctuations stars with large masses can be stabilized and probably stars up to any mass can exist, which usually are identified as black holes.

The baryonic properties of neutron stars within the theory of pseudo-complex General Relativity (pc-GR) are studied. The pc-Tolman-Oppenheimer-Volkoff equations are numerically integrated in order to understand the structure of these objects. The pc-component energy density εΛ has been linearly coupled to the respective baryonic quantity εm. Solutions have been presented for different values of the coupling parameter. It is shown that accumulation of the Λ-component allows the theoretical existence of larger and more massive neutron stars.