The paper by J. M. Lattimer and M. Prakash explores the structure of neutron stars from both theoretical and observational perspectives. They emphasize that the radius of a neutron star is primarily determined by the pressure of matter near nuclear matter equilibrium density. For equations of state (EOS) without extreme softening, the radius is nearly independent of mass and is determined by the pressure magnitude. However, for EOSs with extreme softening or self-bound properties, the radius becomes more sensitive to mass. Accurate measurements of neutron star radii, better than about 1 km, can significantly constrain the EOS. The pressure near nuclear matter density is primarily influenced by the density dependence of the nuclear symmetry energy, while the nuclear incompressibility and skewness parameters play secondary roles. The authors also show that the moment of inertia and binding energy of neutron stars are nearly universal functions of the star's compactness, based on analytic solutions to Einstein's equations by Buchdahl and Tolman. They derive useful approximations for the fraction of the moment of inertia residing in the crust, which depends on the stellar compactness and the pressure at the core-crust interface. The paper discusses various EOSs, including normal and self-bound EOSs, and their implications for neutron star properties. It highlights the importance of accurate measurements of neutron star radii and masses to constrain the EOS and understand the behavior of dense matter. The authors conclude by emphasizing the significance of these measurements in advancing our understanding of neutron star structure and the EOS of dense matter.The paper by J. M. Lattimer and M. Prakash explores the structure of neutron stars from both theoretical and observational perspectives. They emphasize that the radius of a neutron star is primarily determined by the pressure of matter near nuclear matter equilibrium density. For equations of state (EOS) without extreme softening, the radius is nearly independent of mass and is determined by the pressure magnitude. However, for EOSs with extreme softening or self-bound properties, the radius becomes more sensitive to mass. Accurate measurements of neutron star radii, better than about 1 km, can significantly constrain the EOS. The pressure near nuclear matter density is primarily influenced by the density dependence of the nuclear symmetry energy, while the nuclear incompressibility and skewness parameters play secondary roles. The authors also show that the moment of inertia and binding energy of neutron stars are nearly universal functions of the star's compactness, based on analytic solutions to Einstein's equations by Buchdahl and Tolman. They derive useful approximations for the fraction of the moment of inertia residing in the crust, which depends on the stellar compactness and the pressure at the core-crust interface. The paper discusses various EOSs, including normal and self-bound EOSs, and their implications for neutron star properties. It highlights the importance of accurate measurements of neutron star radii and masses to constrain the EOS and understand the behavior of dense matter. The authors conclude by emphasizing the significance of these measurements in advancing our understanding of neutron star structure and the EOS of dense matter.