LAUSR

In this paper, stellar hydrostatic equilibrium configuration of the compact stars (neutron stars and strange stars) has been studied for [Formula: see text] gravity model, with [Formula: see text] and [Formula: see text] being the Gauss–Bonnet invariant and the trace of energy–momentum tensor, respectively. After deriving the hydrostatic equilibrium equations for [Formula: see text] gravity, the fluid pressure for the neutron stars and the strange stars has been computed by implying two equation of state models corresponding to two different compact stars. For the [Formula: see text] gravity model, with [Formula: see text], [Formula: see text], and [Formula: see text] being some specific parameters, substantial change in the behavior of the physical attributes of the compact stars like the energy density, pressure, stellar mass, and total radius has been noted with the corresponding change in [Formula: see text] values. Meanwhile, it has been shown that for some fixed central energy density and with increasing values of [Formula: see text], the stellar mass both for the neutron stars and the strange stars increases, while the total stellar radius [Formula: see text] exhibits the opposite behavior for both of the compact stars. It is concluded that for this [Formula: see text] stellar model, the maximum stellar mass can be boosted above the observational limits.