摘要The neutron star motions are based on the undisturbed finitely thick galactic disk gravitational potential model. Two initial conditions, i.e. the locations and velocities, are considered. The Monte Carlo method is employed to separate rich diversities of the orbits of neutron stars into several sorts. The Poincaré section has the potential to play an important role in the diagnosis of the neutron star motion. It has been observed that the increasing ratio of the motion range vertical to the galactic plane to that parallel to the galactic plane results in the irregularity of neutron star motion.
Abstract：The neutron star motions are based on the undisturbed finitely thick galactic disk gravitational potential model. Two initial conditions, i.e. the locations and velocities, are considered. The Monte Carlo method is employed to separate rich diversities of the orbits of neutron stars into several sorts. The Poincaré section has the potential to play an important role in the diagnosis of the neutron star motion. It has been observed that the increasing ratio of the motion range vertical to the galactic plane to that parallel to the galactic plane results in the irregularity of neutron star motion.
WEI Ying-Chun;A. Taani**;PAN Yuan-Yue;WANG Jing;CAI Yan;LIU Gao-Chao;LUO A-Li;ZHANG Hong-Bo;ZHAO Yong-Heng
. Neutron Star Motion in the Disk Galaxy[J]. 中国物理快报, 2010, 27(11): 119801-119801.
WEI Ying-Chun, A. Taani**, PAN Yuan-Yue, WANG Jing, CAI Yan, LIU Gao-Chao, LUO A-Li, ZHANG Hong-Bo, ZHAO Yong-Heng
. Neutron Star Motion in the Disk Galaxy. Chin. Phys. Lett., 2010, 27(11): 119801-119801.
[1] Jenet F, Finn L S, Lazio J et al 2009 astro-ph.IM arXiv:0909.1058v1
[2] Paczyński B 1990 Astrophys. J. 348 485
[3] Sale S E, Drew J E, Kingge C et al 2009 arXiv:0909.3857v1
[4] Winnberg A 1996 ASP Conference Series 102
[5] Miyamoto M and Nagai R 1975 Publ. Astron. Soc. Jpn. 27 533
[6] Luo X L and Peng Q H 1999 Chin. Phys. Lett. 16 931
[7] Peng F and Peng Q H 2000 Chin. Phys. Lett. 17 382
[8] Peng Q H, Peng F, Chou C K, et al 2002 Astrophys. Space Sci. 282 499
[9] Peng Q H, Chou C K et al 2004 New Astron. 10 17
[10] Lin Y H, Peng Q H, Chou C K et al 2005 Chin. Phys. Lett. 22 776
[11] Hu T, Peng Q H and Zhao Y H 2006 Astron. Astrophys. 446 L5
[12] Zhao Y H, Peng Q H and Hu T 2006 Astron. Astrophys. 452 451
[13] Wei Y C, Wu X J, Peng Q H et al 2005 Chin. J. Astron. Astrophys. 5 610
[14] Wei Y C, Peng Q H, Wu X J et al 2007 Chin. Astron. As\-trophys. 31 11
[15] Lorimer D R 2008 Living Rev. Relativity 11
[16] Fux R 1997 Astron. Astrophys. 327 983
[17] Lyne A, et al 2004 Science 303 1153
[18] Sun X H and Han J L 2004 Mon. Not. R. Astron. Soc. 350 232
[19] Binney J and Tremaine S 1994 Galactic Dynamics (Princeton: Princeton University)
[20] Henon M and Heiles C 1964 Astron. J. 69 73
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