The equations of state for neutron matter, strange and non-strange hadronic matter in the chiral SU(3) quark mean-field model are applied in the study.

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The equations of state for neutron matter, strange and non-strange hadronic matter in the chiral SU(3) quark mean-field model are applied in the study of slowly rotating neutron stars and hadronic stars. It is shown that the rotation can increase the maximum mass of compact stars significantly, however the mass of the strange hadronic star is still not big enough to explain the observed extremely heavy pulsar, because of the weak equation of state of strange hadronic matter in this model. Slowly Rotating Neutron Stars and Hadronic Stars Shaoyu Yin, Jiadong Zang, and Ru-Keng Su Euro. Phys. Jour. A 43 (2010) 295-301 Physics Department, Fudan University, 220 Handan Road, 200433, Shanghai, China Inner structure of neutron star (From Prog. Part. Nucl. Phys. 54 (2005) 193) strange hadronic non-strange hadronic neutron The EoS in chiral SU(3) quark mean field model (Phys. Rev. C 72 (2005) 045801) consider the relativistic rotation effect on the stellar mass and radius M-R relation of Strange hadronic star under rotation TOV Equation Metric 1 2 3 4 Linear order, l=0 correction of the spherical harmonics Conclusion: The range of the mass is significantly enlarged when the rotation is considered. However, the maximum mass of the strange hadronic star is still not large enough to explain the mass of PSR J1903+0327. Possible future work: 1. Consider the non-uniform rotation with larger core speed. 2. Modify the too soft EoS of the strange hadronic matter.