The properties of massive compact stars using a geometrically deduced equation of state

To construct models of relativistic compact stars, it is vitally important to know exact composition and behaviour of particle interactions at exceptionally high density regime. When studying neutron stars, it is interesting to study the relation between the mass and the radius of the star. To find this relation, equation for the stellar structure is needed specifically to the underlying equation of state. It has recently been pointed out that the stiffest detainment to the mass-radius relation of neutron stars, the largest mass, the largest radius, and the maximum surface gravity are provided by the observations for pulsars. An attempt is made here to obtain the mass-radius relation using the geometrical EoS deduced from geometrically, adopted for the core-envelope model of compact objects