Neutron Stars In f(R,T) Theory: Slow Rotation Approximation

In this paper, we study the slowly rotating neutron stars in f(R, T) gravity based on Hartle-Thorne formalism. We consider the simplest matter-geometry coupled modified gravity, namely f(R, T)=R+2χ T. We compute the mass, radius, moment of inertia, change in radius and binding energy due to rotation, eccentricity, quadrupole moment and the tidal love number. The quantities, which are of the second order in angular velocity, like, change in radius and binding energy due to rotation, eccentricity and quadrupole moment, deviate more from their corresponding general relativistic counterparts in lighter neutron stars than heavier ones. Whereas the moment of inertia, which is of the first order in angular velocity, in f(R, T) gravity, barely diverges from the general relativistic one. The Equation of state-independent I-Love-Q relation retains in f(R, T) gravity, and it coincides with the general relativistic ones within less than one percent even for the maximum allowed coupling parameters.