Transcript Document

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
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.
Inner structure of neutron star (From Prog. Part. Nucl. Phys. 54 (2005) 193)
neutron
non-strange hadronic
strange hadronic
TOV Equation
Metric
The EoS in chiral SU(3) quark mean
field model (Phys. Rev. C 72 (2005) 045801)
Linear order,
l=0 correction
of the spherical
harmonics
consider the relativistic rotation
effect on the stellar mass and radius
M-R relation of
Strange hadronic
star under rotation
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.