Introduction

This module is designed to compute the gravitational properties of slowly rotating neutron stars using the Hartle-Thorne approximation. Assuming the user provides a barotropic equation of state, the module computes two types of gravitational properties: global quantities and local functions. The global quantities include mass, radius, moment of inertia, tidal Love number, quadrupole moment, and the effects of rotation on mass and radius. The local functions provide internal profiles as a function of the radial coordinate, including pressure, energy density, chemical potential, baryon density, and relevant metric functions.

The importance of this module lies in its ability to help researchers test equations of state (EoS) models against observational data, which is crucial for understanding the behavior of neutron stars. By enabling users to optimize the running of a wide range of equations of state, the module serves as a powerful tool for exploring the relationship between theoretical predictions and experimental findings in neutron star astrophysics.

This documentation will guide users through the functionality of the module, starting with a quick-start section for a rapid introduction on how to run it. It will also provide a physics overview detailing the theoretical framework and numerical methods used, followed by an explanation of the code architecture. Further sections will outline detailed execution instructions and include practical examples to facilitate user understanding.