Baryonic properties of neutron stars within pseudo‐complex General Relativity

Abstract

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.

Predictions of the pseudo‐complex general relativity

“…And this is the point! In pcGR there is no contradiction because one can have a neutron star and a large mass (Caspar et al ; Hess et al, ; Rodríguez et al ; ). However, with increasing mass it gets more and more difficult to see a pulsation because of the increase in the redshift, which mimics, for superheavy masses, a dark star similar to a real BH.…”

Kerr Black Holes within a Modified Theory of Gravity

“…In addition, neutron stars were studied in [18][19][20], in addition to [9]. Including the effects of the pc-GR, stars up to six solar masses were obtained in [18,20] and up to 200 solar masses in [19].…”