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Proton Fraction in Hot Neutron Star Matter with a Chiral Hadronic Model |
| GUO Hua1,3;ZHOU Ran1; LIU Yu-Xin1,2,3,4 |
| 1Department of Technical Physics and MOE Laboratory of Heavy Ion Physics, Peking University, Beijing 100871
2Department of Physics, Peking University, Beijing 100871
3Center of Theoretical Nuclear Physics, National Laboratory of Heavy Ion Accelerator, Lanzhou 730000
4Institute of Theoretical Physics, Chinese Academy of Sciences, Beijing 100080 |
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| Cite this article: |
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GUO Hua, ZHOU Ran, LIU Yu-Xin 2002 Chin. Phys. Lett. 19 1432-1435 |
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Abstract In the framework of a chiral hadronic model it has been numerically proven that the parabolic expansion with respect to δ2 at finite density and temperature is a good approximation in the relativistic mean field theory. It is also shown that the proton fraction in the modified Urca process is considerably restrained in comparison with that of the direct Urca process. Then, we discuss the influences of the density-dependent and temperature-dependent asymmetry energy on the proton fraction in hot neutron star matter.
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| Keywords:
21.65.+f
05.70.Ce
21.30.Fe
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Published: 01 October 2002
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| PACS: |
21.65.+f
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05.70.Ce
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(Thermodynamic functions and equations of state)
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21.30.Fe
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(Forces in hadronic systems and effective interactions)
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