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The equations of state for neutron matter, strange and non-strange hadronicmatter in a chiral SU(3) quark mean field model are applied in the study ofslowly rotating neutron stars and hadronic stars. The radius, mass, moment ofinertia, and other physical quantities are carefully examined. The effect ofnucleon crust for the strange hadronic star is exhibited. Our results show therotation can increase the maximum mass of compact stars significantly. For bigenough mass of pulsar which can not be explained as strange hadronic star, thetheoretical approaches to increase the maximum mass are addressed.

Slowly rotating neutron stars and hadronic stars in chiral SU(3) quark mean field model