The Equation of State of Neutron Star Matter in Uniform Strong Magnetic Fields

CHEN Wei; LIU Liang-Gang

Chinese Physics C> 2005, Vol. 29> Issue(2) : 119-123

The Equation of State of Neutron Star Matter in Uniform Strong Magnetic Fields

CHEN Wei ^, ,
LIU Liang-Gang

Department of Physics,Jinan University,Guangzhou 510632,China2 Department of Physics,Sun Yat-Sen University,Guangzhou 510275,China

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Abstract：
The Walecka model is extended to the neutron star matter, and in it's mean field approximation, the properties of neutron star matter consisted of proton, neutron and electron in uniform strong magnetic fields are studied. it is found that the ~equation of state (eos) becomes stiffer in some degree, and the ratio of neutron increase evidently while the one of proton and electron decrease with the magnetic field being stronger. the influence of the magnetic to the eos is smaller than the one to the fractions of the particles. the pressure of the neutron star matter is calculated by hydrodynamics and thermodynamics respectively. the stronger the magnetic field is, the more adjacent the curves of pressure depicted in these two ways are, and they are in superposition completely when the magnetic field is 10¹⁴T.

References

[1]

. Taylor J H, Manchest er R N, Lyne N G. ApJS, 1993, 88: 5292. Bhm-Vitense E. Introduction to Stellar Astrophysics, Vol. 1 ( Cambridge: Cambridge up) , 1989, Ch. 143. Duncan R C, Thompson C. ApJ, 1992, 392:L94. Usov V V. Nature, 1992, 357: 4725. Paczyn'ski B. Acta Astron, 1992, 42: 1456. Thompson C, Duncan R C. MNRAS, 1995, 275: 2557. Thompson C, Duncan R C. ApJ, 1996, 473: 3228. Vasisht G, Gotthelf E V. ApJ, 1997, 486: L1299. Kouveliotou C et al. Nature, 1998, 393: 23510. Kouveliotou C et al. ApJ, 1999, 510:L11511. Chatterjee P, Hernquist L, Narayan R. ApJ, 2000, 534: 37312. Heyl J S, Kulkarni S R. ApJ, 1998, 506: L6113. Kouveliotou C et al . Nature, 1994, 368: 12514. Bignami G F et al. Nature, 2003, 423: 72515. Michel F C. Theory of Neutron St arMagneto Spheres. Chicago: University of Chicago Press, 199116. LAI D, Wynn C G Ho. Phys. Rev. Lett. , 2003, 91: 07110117. Canuto V, Ventura J. Cosmic Phys. , 1977, 2: 20318. LAI D, Shapiro S L. Astrophys. J. , 1991, 383: 74519. Yakovlev D G, Kaminker A D. The Equation of States in Astrophysics.Ed. Chabrier G, Schatzman E. Cambridge: Cambridge University Press, 1994, 21420. Vshivtsev A S, Serebryakova. JETP, 1994, 79: 1721. Chakrabarty S, Bandyopadhyay, Pal Subrata. Phys. Rev. Lett . , 1997,78: 289822. Chakrabarty S. Phys. Rev. , 1996, D54: 130623. MAO G J, Iwamoto A, LI Zh X. Chin. J. Astron. Astrophys. , 2003,3: 359

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CHEN Wei and LIU Liang-Gang. The Equation of State of Neutron Star Matter in Uniform Strong Magnetic Fields[J]. Chinese Physics C, 2005, 29(2): 119-123.

CHEN Wei and LIU Liang-Gang. The Equation of State of Neutron Star Matter in Uniform Strong Magnetic Fields[J]. Chinese Physics C, 2005, 29(2): 119-123. shu

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Received: 2004-06-14
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

The Equation of State of Neutron Star Matter in Uniform Strong Magnetic Fields

Corresponding author: CHEN Wei,

Department of Physics,Jinan University,Guangzhou 510632,China2 Department of Physics,Sun Yat-Sen University,Guangzhou 510275,China

Received Date: 2004-06-14

Accepted Date: 1900-01-01

Available Online: 2005-02-05

Abstract: The Walecka model is extended to the neutron star matter, and in it's mean field approximation, the properties of neutron star matter consisted of proton, neutron and electron in uniform strong magnetic fields are studied. it is found that the ~equation of state (eos) becomes stiffer in some degree, and the ratio of neutron increase evidently while the one of proton and electron decrease with the magnetic field being stronger. the influence of the magnetic to the eos is smaller than the one to the fractions of the particles. the pressure of the neutron star matter is calculated by hydrodynamics and thermodynamics respectively. the stronger the magnetic field is, the more adjacent the curves of pressure depicted in these two ways are, and they are in superposition completely when the magnetic field is 10¹⁴T.

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The Equation of State of Neutron Star Matter in Uniform Strong Magnetic Fields

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