The equations of state for neutron matter, strange and non-strange hadronic matter in the chiral SU(...
Download
1 / 1

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


  • 65 Views
  • Uploaded on

loader
I am the owner, or an agent authorized to act on behalf of the owner, of the copyrighted work described.
capcha
Download Presentation

PowerPoint Slideshow about ' Inner structure of neutron star ( From Prog. Part. Nucl. Phys. 54 (2005) 193 )' - libby-meadows


An Image/Link below is provided (as is) to download presentation

Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author.While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server.


- - - - - - - - - - - - - - - - - - - - - - - - - - E N D - - - - - - - - - - - - - - - - - - - - - - - - - -
Presentation Transcript
Inner structure of neutron star from prog part nucl phys 54 2005 193

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.