Equation of State and Proton Ratio on the Inner Shell Layer of Neutron Stars

WEN Hai-Bao

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2024年10月30日

Chinese Physics C> 2005, Vol. 29> Issue(7) : 657-663

Equation of State and Proton Ratio on the Inner Shell Layer of Neutron Stars

WEN Hai-Bao ^,

Institute of High Energy Physics,Chinese Academy of Sciences,Beijing 100049Graduate School of the Chinese Academy of Sciences,Beijing 100049

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Abstract：
We calculate the energy spectra and eigenfunctions of nucleons in a constant magnetic field. Concrete solutions of the Dirac equation including the anomalous magnetic moment (AMM) of nucleons are provided in the chiral representation. They are then used to investigate the equation of state (EOS) and particle ratios on the inner shell layer of neutron stars. The results show that the magnetic energy of strong field will increase the inner shell layer of neutron stars,but the matter remains to be a neutron-rich matter. It is found that the AMM has evident effects on the proton polarization.

References

[1]

. Lattimer J M, Prakash M. Science, 2004, 304: 5362. Michel F C. Theory of Neut ron Star: Magnetospheres. Chicago: University of Chicago Press, 19913. Mazet s E P, Golenetskii S V, Ⅱ' inskii V N et al. Nature, 1979, 587:282.4. Rothschild R E, Kulkarni S R,Lingenfelt er R E.Nature, 1994, 432: 3685. Kouveliotou C et al. Nature, 1998, 235: 3936. Woods P M et al . Astrophys. J. , 1999, L139: 5197. Chakrabarty S, Bandyopadhyay D, Pal S. Phys. Rev. Lett. , 1997,7.: 28988. Schwinger J. Phys. Rev. , 1948, 73: 4169. Schwinger J. Phys. Rev. , 1951, 82: 66410. Duncan R C. Physics in Ultra strong Magnetic Fields. In:FifthHunt svil leGamma Ray Burst Symposium. Kippen R M, Mallozzi R S, Fishman GJ. New York: AIP, 2000. 830( Preprint: ast ro ph/ 0002442)11. Broderick A, Prakash M, Latt imer J M. Ast rophys. J. , 2000, 537:35112. Suh I S , Mathews G J. Astrophys. J. , 2001, 546: 112613. Kobayashi M, Sakamot o M. Prog. Theo. Phys. , 1983, 70( 5) : 137514. MAO G, Iwamoto A, LI Z. Chin. J. Astron. Astrophys. , 2003, 3:35915. Glendenning N K. Compact Stars. New York: Springer, 200016. Landau L D, Lifshitz EM, Pit aevski i L P. Electrodynamics of Cont inuous Media. New York: Pergamon, 198417. Potekhin A Y, Chabrier G. Astrophys. J. , 2003, 585: 95518. ZHANG F S, CHEN L W. Chin. Phys . Lett . , 2001, 18: 14219. MAO G, Kondratyev V N, Iwamoto A et al. Chin. Phys. Lett . , 2003,20: 123820. Potekhin A Y, Lai D, Chabrier G. Astrophys. J. , 2004, 612: 1034

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WEN Hai-Bao. Equation of State and Proton Ratio on the Inner Shell Layer of Neutron Stars[J]. Chinese Physics C, 2005, 29(7): 657-663.

WEN Hai-Bao. Equation of State and Proton Ratio on the Inner Shell Layer of Neutron Stars[J]. Chinese Physics C, 2005, 29(7): 657-663. shu

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Received: 2004-11-17
Revised: 1900-01-01

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沈阳化工大学材料科学与工程学院沈阳 110142

Equation of State and Proton Ratio on the Inner Shell Layer of Neutron Stars

WEN Hai-Bao ^,

Corresponding author: WEN Hai-Bao,

Institute of High Energy Physics,Chinese Academy of Sciences,Beijing 100049Graduate School of the Chinese Academy of Sciences,Beijing 100049

Received Date: 2004-11-17
Accepted Date: 1900-01-01
Available Online: 2005-07-05

Abstract: We calculate the energy spectra and eigenfunctions of nucleons in a constant magnetic field. Concrete solutions of the Dirac equation including the anomalous magnetic moment (AMM) of nucleons are provided in the chiral representation. They are then used to investigate the equation of state (EOS) and particle ratios on the inner shell layer of neutron stars. The results show that the magnetic energy of strong field will increase the inner shell layer of neutron stars,but the matter remains to be a neutron-rich matter. It is found that the AMM has evident effects on the proton polarization.