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Inner structure of neutron star ( From Prog. Part. Nucl. Phys. 54 (2005) 193 )PowerPoint Presentation

Inner structure of neutron star ( From Prog. Part. Nucl. Phys. 54 (2005) 193 )

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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.

Inner structure of neutron star (From Prog. Part. Nucl. Phys. 54 (2005) 193)

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

neutron

non-strange hadronic

The EoS in chiral SU(3) quark mean

field model (Phys. Rev. C 72 (2005) 045801)

strange hadronic

consider the relativistic rotation

effect on the stellar mass and radius

3

Linear order,

l=0 correction

of the spherical

harmonics

4

1

TOV Equation Metric

2

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.

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