Properties of Neutron Stars Rotating at Kepler Frequency with Uniform Strong Magnetic Field
WEN De-Hua1, CHEN Wei2, LU Yi-Gang1, LIU Liang-Gang3
1School of Physics, South China University of Technology, Guangzhou 5106412Department of Physics, Jinan University, Guangzhou 5106323The Faculty of Information Technology, Macau University of Science and Technology, Macao
Properties of Neutron Stars Rotating at Kepler Frequency with Uniform Strong Magnetic Field
WEN De-Hua1;CHEN Wei2;LU Yi-Gang1;LIU Liang-Gang3
1School of Physics, South China University of Technology, Guangzhou 5106412Department of Physics, Jinan University, Guangzhou 5106323The Faculty of Information Technology, Macau University of Science and Technology, Macao
摘要A uniform strong magnetic field is considered in calculating the properties of neutron star rotating at the Kepler frequency. The results show that the effect of the magnetic field on the properties of neutron star is evident, and the properties of the neutron stars rotating at the Kepler frequency can be used as a criterion to the equations of states of the neutron star matters.
Abstract：A uniform strong magnetic field is considered in calculating the properties of neutron star rotating at the Kepler frequency. The results show that the effect of the magnetic field on the properties of neutron star is evident, and the properties of the neutron stars rotating at the Kepler frequency can be used as a criterion to the equations of states of the neutron star matters.
WEN De-Hua;CHEN Wei;LU Yi-Gang;LIU Liang-Gang. Properties of Neutron Stars Rotating at Kepler Frequency with Uniform Strong Magnetic Field[J]. 中国物理快报, 2007, 24(3): 628-631.
WEN De-Hua, CHEN Wei, LU Yi-Gang, LIU Liang-Gang. Properties of Neutron Stars Rotating at Kepler Frequency with Uniform Strong Magnetic Field. Chin. Phys. Lett., 2007, 24(3): 628-631.
[1]Wood P M, Kouveliotou C, ban Paradijs J, Hurley K, Kippen R M,Finger M H, Briggs M S, Dieter S and Fishman F J 1999 Astrophys. J. 519 L139 [2]Chatterfee P, Hernquist L and Narayan R 2000 Astrophys. J. 34 373 [3]Bocquet M, Bonazzola S, Gourgoulhon E and Noak J 1995 Astron. Astrophys. 301 757 [4]Cardaa C Y, Prakash M and Lattimer J M 2001 Astrophys. J.554 322 [5]Bai H and Peng Q H 2004 Chin. Phys. Lett. 21 2117 [6]Hartle J B 1967 Astrophys. J. 150 1005 [7] Hartle J B and Thorne K S 1968 Astrophys. J. 153 807 [8] Oyamatsu K and Iida K 2003 Prog. Theor. Phys. 109 631 [9] Friedman J L, Ipser J R and Parker L 1986 Astrophys. J.304 115 [10] Weber F 2002 http://xxx.lanl.gov/abs/astro-ph/0207053 [11] Backer K C, Kulkarni S R, Heiles C, Davis M M and Goss W M1982 Nature 300 615 [12] Barziv O, Kaper L, van Kerkwijk M H, Telting J H and van ParadijsJ 2001 Astron. Astrophys. 377 925 [13]Wen D H, Chen W, Wang X J, Ai B Q, Liu G T, Dong D Q and Liu LG 2004 Eur. Phys. J. A 21 349 [14]WenD H, Chen W and Liu L G 2005 Chin. Phys. Lett.22 1604
2007, Vol. 24 
