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

  • 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.
  • 加载中
  • [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
  • 加载中

Get Citation
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
Milestone
Received: 2004-06-14
Revised: 1900-01-01
Article Metric

Article Views(3745)
PDF Downloads(597)
Cited by(0)
Policy on re-use
To reuse of subscription content published by CPC, the users need to request permission from CPC, unless the content was published under an Open Access license which automatically permits that type of reuse.
通讯作者: 陈斌, bchen63@163.com
  • 1. 

    沈阳化工大学材料科学与工程学院 沈阳 110142

  1. 本站搜索
  2. 百度学术搜索
  3. 万方数据库搜索
  4. CNKI搜索

Email This Article

Title:
Email:

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

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.

    HTML

Reference (1)

目录

/

DownLoad:  Full-Size Img  PowerPoint
Return
Return