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 StarsShaoyu 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 meanfield 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

TO

V E

quat

ion

Met

ric

Linear order, l=0 correction of the sphericalharmonics

Conclusion: The range of themass is significantly enlarged

when the rotation is considered.However, the maximum massof the strange hadronic star is

still not large enough to explainthe mass of PSR J1903+0327.

Possible future work: 1. Consider the non-uniform

rotation with larger core speed.2. Modify the too soft EoS ofthe strange hadronic matter.