Structures of rotating traditional neutron stars and hyperon stars in the relativistic $sigma-omega$ model |
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| Authors: | De-hua?Wen,Wei?Chen,Xian-ju?Wang,Bao-quan?Ai,Guo-tao?Liu,Dong-qiao?Dong,Liang-gang?Liu author-information" > author-information__contact u-icon-before" > mailto:stdp@zsu.edu.cn" title=" stdp@zsu.edu.cn" itemprop=" email" data-track=" click" data-track-action=" Email author" data-track-label=" " >Email author |
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| Affiliation: | (1) Department of Physics, Zhongshan University, 510275 Guangzhou, PRC;(2) Department of Physics, South China University of Technology, 510641 Guangzhou, PRC;(3) Department of Physics, Jinan University, 510632 Guangzhou, PRC |
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| Abstract: | 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  - 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 Hartles 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.Received: 7 November 2003, Revised: 17 February 2004, Published online: 31 August 2004PACS: 04.40.Dg Relativistic stars: structure, stability, and oscillations - 95.30.Sf Relativity and gravitation - 97.10.Kc Stellar rotation - 97.60.Jd Neutron stars |
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