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

Abstract
HTML
Reference
Related

PDF

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

[1]	ZHAO Xian-Feng , WANG Shun-Jin , ZHANG Hua , JIA Huan-Yu . Effect of σ*,φ Mesons on the Neutron Star Matter at Finite Temperature. Chinese Physics C, 2007, 31(6): 532-537.
[2]	ZHAO Xian-Feng , WANG Shun-Jin , ZHANG Hua , JIA Huan-Yu . Effect of f₀(975) and φ(1020) Mesons on Neutron Star Mater. Chinese Physics C, 2007, 31(4): 345-349.
[3]	ZUO Wei , LI Ang , LUO Pei-Yan , YONG Gao-Chan . Properties of Proto-Neutron Star and Effect of Three-Body Forces. Chinese Physics C, 2006, 30(10): 956-960.
[4]	CHEN Wei . Thermal Property of Protoneutron Star Matter. Chinese Physics C, 2006, 30(2): 118-122.
[5]	DING Wen-Bo , LIU Guang-Zhou . Condensations of K^－ and K⁰ in Neutron Star Matter. Chinese Physics C, 2006, 30(S2): 249-251.
[6]	ZUO Wei , LI Ang , CHEN Ji-Yan , LI Zeng-Hua . Kaon Condensation in Neutron Star Matter and Nuclear Three-Body Force Effect. Chinese Physics C, 2005, 29(7): 632-638.
[7]	WEN Hai-Bao . Equation of State and Proton Ratio on the Inner Shell Layer of Neutron Stars. Chinese Physics C, 2005, 29(7): 657-663.
[8]	ZHU Zhao-Huan , BAN Shu-Fang , LI Jun , MENG Jie . Pesponse of the Neutron Star Properties to the Equation of State at Low Density. Chinese Physics C, 2005, 29(6): 565-569.
[9]	LI Jun , BAN Shu-Fang , JIA Huan-Yu , SANG Jian-Ping , MENG Jie . Description of the Nuclear Matter and Neutron Star in Relativistic Mean Field Theory with Density-Dependent Interactions. Chinese Physics C, 2004, 28(2): 140-147.
[10]	SHEN Gang , MENG Jie , Hillhouse G . Direct URCA Process in Neutron Stars. Chinese Physics C, 2004, 28(S1): 99-101.
[11]	JIA Huan-Yu , MENG Jie , ZHAO En-Guang , LI Jun , SANG Jian-Ping . Effect of Temperature on Hyperon Neutron Star. Chinese Physics C, 2003, 27(3): 200-205.
[12]	LIU Bo , GUO Hua . In-Medium Effects on Neutron Stars. Chinese Physics C, 2003, 27(8): 683-687.
[13]	LI Zeng-Hua , LU Guang-Cheng , ZUO Wei . Properties of Isospin Asymmetric Nuclear Matter and Extended BHF Approach (Ⅶ) Proton and Neutron ¹S₀ Superfluidity in Neutron Star Matter. Chinese Physics C, 2003, 27(12): 1084-1088.
[14]	GUO Hua , LIU Bo , LI Xi-Guo , CHEN Yan-Jun . Kaon Condensation in Neutron Star Matter. Chinese Physics C, 2003, 27(2): 113-117.
[15]	YANG Shu-Hua , ZHENG Xiao-Ping . Consistent Thermodynamics of SQM and EOS of Strange Stars in Quasi-Particle Description. Chinese Physics C, 2002, 26(11): 1172-1177.
[16]	LI Wen-Fei , 2< sup> , ZHANG Feng-Shou , CHEN Lie-Wen . Density Dependence of Proton Fraction in Neutron Stars. Chinese Physics C, 2001, 25(8): 759-764.
[17]	LI Wen-Fei , ZHANG Feng-Shou , CHEN Lie-Wen . Study on Mass and Radius of Neutron Star Using Asymmetry Equation of State of Nuclear Matter. Chinese Physics C, 2001, 25(9): 877-883.
[18]	CHEN Wei , AI Bao-Quan , ZHENG Xiao-Ping , LIU Liang-Gang . Influence of Self-Interaction ofσ Meson to the Equation of State of Nuclear Matter. Chinese Physics C, 2001, 25(1): 23-30.
[19]	SUN Bao-Xi , JIA Huan-Yu , MENG Jie , ZHAO En-Guang . Neutron Star in Relativistic Mean-field Approximation. Chinese Physics C, 2000, 24(S1): 69-72.
[20]	Chen Wei , Mei Zhonghao , Liu Lianggang . Study of the Equation of State of Nuclear Matter. Chinese Physics C, 1999, 23(7): 681-688.

Access

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

RIS(for EndNote,Reference Manager,ProCite)

BibTex

Txt

Milestone

Received: 2004-06-14
Revised: 1900-01-01

Article Metric

Article Views(4017)
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

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.

HTML

Reference (1)

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

Abstract：

References

Access

Article Metrics

Metrics

通讯作者: 陈斌, bchen63@163.com

Email This Article