Acceleration due to gravity on a rapidly rotating neutron sta

In this thesis I am going to calculate the acceleration due to gravity on axisymmetric neutron stars using the rapidly rotating neutron star code (RNS). I modified the original RNS code so that it can compute the acceleration at different latitudes of the star. I am calculating different stellar models, and I was able to get physical quantities like the maximum mass for each spin frequency.;The code that I am using solves for the geometry of an axisymmetric rotating neutron star described by Komatsu, Eriguchi and Hachisu (1989). The metric of the star has four potentials which are used in the calculation of acceleration due to gravity. The code numerically solves the four field equations and the integrated equation of hydrostatic equilibrium. I find the acceleration due to gravity for different equation of states (EOS). The EOS range from the soft EOS BBB2, stiff (using equation of state L) and intermediate stiffness (using equation of state APR). Lastly I will plot the equatorial and polar acceleration due to gravity for the different equations of state. I will attempt empirical fit for those curves based on the stars' physical parameters such as mass, radius and spin. I show also the acceleration gradient at stellar latitudes at different spin frequencies for the three different equations of states.