Structures of rotating traditional neutron stars and hyperon stars in the relativistic \sigma-\omega model

Research paper by De-hua Wen, Wei Chen, Xian-ju Wang, Bao-quan Ai, Guo-tao Liu, Dong-qiao Dong, Liang-gang Liu

Indexed on: 01 Aug '04Published on: 01 Aug '04Published in: The European Physical Journal A


The influence of rotation on the total masses and radii of neutron stars is calculated by Hartle’s slow-rotation formalism, while the equation of state is considered in a relativistic \(\sigma\)-\(\omega\) model. As the changes of the mass and radius of a real neutron star caused by rotation are very small in comparison with the total mass and radius, one can see that Hartle’s approximate method is rational to deal with the rotating neutron stars. If three property values, mass, radius and period, are observed for the same neutron star, then the EOS of this neutron star could be decided entirely.