旋转致密双星的引力波特征

王玉诏; 伍歆; 钟双英

doi:10.7498/aps.61.160401

摘要

研究了轨道和旋转效果到2.5阶后牛顿旋转致密双星拉格朗日动力学与引力波的关系, 分析了有序和混沌轨道的引力波特征.发现当加速度不考虑辐射项时, 有序双星系统辐射的引力波具有周期或拟周期的特征, 而混沌双星系统辐射的引力波却具有明显的混沌特征.当加速度含有辐射项贡献时, 双星必会出现并合现象.此时, 原保守有序双星系统需较长时间才能完成并合过程, 引力波形在双星并合前仍保留拟周期的基本特点;然而, 原保守混沌双星系统仅在较短时间内就会并合, 但因并合时间太短, 无法获取足够的动力学信息导致引力波形的特征不易分辨.

关键词:

Abstract

Some characterizations of gravitational waves emitted from the 2.5 post-Newtonian order Lagrangian dynamics of spinning compact binaries including the next-order spin-orbit contribution and the radiative reaction are detailed. The relationship between the regular and chaotic dynamics and the gravitational waveforms is also described. When the radiative reaction term does not appear in the equations of motion, the gravitational waves are periodic/quasi-periodic for an order conservative binary system, but they seem to be typically irregular for a chaotic one. On the other hand, the binary systems become dissipative and should coalesce if the radiative reaction term is added to the equations of motion. In the dissipative case, the original ordered conservative system can still give regular gravitational waveforms in such a long time before the occurrence of the merging orbits. However, the coalescence time of the binary system corresponding to its original chaotic conservative system is too short to obtain enough information about the characterization of the gravitational waveforms.

Keywords:

作者及机构信息

1.
南昌大学物理系, 南昌 330031

基金项目: 国家自然科学基金(批准号: 10873007, 11173012, 11178002, 11165011)和南昌大学创新团队项目资助的课题.

Authors and contacts

1.
Department of Physics, Nanchang University, Nanchang 330031, China

Funds: Project supported by the National Natural Science Foundation of China (Grant Nos. 10873007, 11173012, 11178002, 11165011) and the Program for Innovative Research Team of Nanchang University, China.

参考文献

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[24]	Wu X, Xie Y 2010 Phys. Rev. D 81 084045
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[28]	Chen J H, Wang Y J 2004 Chin. Phys. 13 583
[29]	Chen J H, Wang Y J 2005 Chin. Phys. 14 1282
[30]	Chen J H, Wang Y J 2006 Chin. Phys. 15 1705
[31]	Wang Y, Wu X 2012 Chin. Phys. B 21 050504
[32]	Galaviz P, Brugmann 2011 Phys. Rev. D 83 084013
[33]	Wang Y, Wu X 2011 Class. Quantum Grav. 28 025010
[34]	Wu X, Zhong S Y 2011Gen. Relat. Gravit. 43 2185
[35]	Wu X, Huang T Y 2003 Phys. Lett. A 313 77
[36]	Froeschle C, Lega E, Gonczi R 1997 Celest. Mech. Dyn. Astron. 67 41
[37]	Wu X, Huang T Y, Zhang H 2006 Phys. Rev. D 74 083001
[38]	Li R, Wu X 2010 Acta Phys. Sin. 59 7135 (in Chinese) [李荣, 伍歆 2010 物理学报 59 7135]
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[40]	Di G H, Xu Y, Xu W, Gu R C 2011 Acta Phys. Sin. 60 020504 (in Chinese) [狄根虎, 许勇, 徐伟, 顾仁财 2011 物理学报 60 020504]
[41]	Sun K H, Liu X, Zhu C X 2010 Chin. Phys. B 19 110510
[42]	Baker J G, van Meter J R, McWilliams S T, Centrella J, Kelly B J 2007 Phys. Rev. Lett. 99 181101

施引文献

[1]	Kidder L E 1995 Phys. Rev. D 52 821
[2]	Will C M, Wiseman A G 1996 Phys. Rev. D 54 4813
[3]	Gopakumar A, Iyer B R 2002 Phys. Rev. D 65 084011
[4]	Blanchet L, Faye G, Iyer B R, Sinha S 2008 Class. Quant. Grav. 25 165003
[5]	Tagoshi H, Ohashi A, Owen B J 2001 Phys. Rev. D 63 044006
[6]	Faye G, Blanchet L, Buonanno A 2006 Phys. Rev. D 74 104033
[7]	Blanchet L, Buonanno A, Faye G 2006 Phys. Rev. D 74 104034
[8]	Buonanno A, Chen Y, Damour T 2006 Phys. Rev. D 74 104005
[9]	Hergt S, Schafer G 2008 Phys. Rev. D 78 101503
[10]	Kokubun F 1998 Phys. Rev. D 57 2610
[11]	Suzuki S, Maeda K I 1999 Phys. Rev. D 61 024005
[12]	Kiuchi K, Maeda K I 2004 Phys. Rev. D 70 064036
[13]	Kiuchi K, Koyama H, Maeda K I 2007 Phys. Rev. D 76 024018
[14]	Wang Y, Wu X 2011 Commun. Theor. Phys. 56 1045
[15]	Zhong S Y, Liu S 2012 Acta Phys. Sin. 61 120401 (in Chinese) [钟双英, 刘崧 2012 物理学报 61 120401]
[16]	Levin J 2000 Phys. Rev. Lett. 84 3515
[17]	Schnittman J D, Rasio F A 2001 Phys. Rev. Lett. 87 121101
[18]	Cornish N J, Levin J 2002 Phys. Rev. Lett. 89 179001
[19]	Konigsdorffer C, Gopakumar A 2005 Phys. Rev. D 71 024039
[20]	Hartl M D, Buonanno A 2005 Phys. Rev. D 71 024027
[21]	Levin J 2006 Phys. Rev. D 74 124027
[22]	Wu X, Xie Y 2007 Phys. Rev. D 76 124004
[23]	Wu X, Xie Y 2008 Phys. Rev. D 77 103012
[24]	Wu X, Xie Y 2010 Phys. Rev. D 81 084045
[25]	Zhong S Y, Wu X 2010 Phys. Rev. D 81 104037
[26]	Zhong S Y, Wu X 2011 Acta Phys. Sin. 60 090402 (in Chinese) [钟双英, 伍歆 2011 物理学报 60 090402]
[27]	Chen J H, Wang Y J 2003 Chin. Phys. 12 836
[28]	Chen J H, Wang Y J 2004 Chin. Phys. 13 583
[29]	Chen J H, Wang Y J 2005 Chin. Phys. 14 1282
[30]	Chen J H, Wang Y J 2006 Chin. Phys. 15 1705
[31]	Wang Y, Wu X 2012 Chin. Phys. B 21 050504
[32]	Galaviz P, Brugmann 2011 Phys. Rev. D 83 084013
[33]	Wang Y, Wu X 2011 Class. Quantum Grav. 28 025010
[34]	Wu X, Zhong S Y 2011Gen. Relat. Gravit. 43 2185
[35]	Wu X, Huang T Y 2003 Phys. Lett. A 313 77
[36]	Froeschle C, Lega E, Gonczi R 1997 Celest. Mech. Dyn. Astron. 67 41
[37]	Wu X, Huang T Y, Zhang H 2006 Phys. Rev. D 74 083001
[38]	Li R, Wu X 2010 Acta Phys. Sin. 59 7135 (in Chinese) [李荣, 伍歆 2010 物理学报 59 7135]
[39]	Li R, Wu X 2011 Eur. Phys. J. Plus 126 73
[40]	Di G H, Xu Y, Xu W, Gu R C 2011 Acta Phys. Sin. 60 020504 (in Chinese) [狄根虎, 许勇, 徐伟, 顾仁财 2011 物理学报 60 020504]
[41]	Sun K H, Liu X, Zhu C X 2010 Chin. Phys. B 19 110510
[42]	Baker J G, van Meter J R, McWilliams S T, Centrella J, Kelly B J 2007 Phys. Rev. Lett. 99 181101

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