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This paper mainly deals with the effects of eccentricity on the gravitational waveforms emitted by the non-conservative post-Newtonian (PN) Hamiltonian formulations of the spinning compact binaries. The numerical results show that the change of eccentricity has a slight influence on the time-domain gravitational waveforms from the conservative spinning compact binaries, but the frequency bands of gravitational waveforms is broadened with increasing eccentricity. Owing to the effects of dissipation from the gravitational radiation reaction, the separation and the eccentricity decrease gradually with time, and the gravitational waveforms emitted from the non-conservative PN spinning compact binaries are modulated by the eccentricity, meanwhile the amplitude of the waveforms enhances with the increase of eccentricity; the duration of the waveforms decreases.
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Keywords:
- non-conservative /
- gravitational radiation reaction /
- dissipation /
- eccentricity
[1] Kidder L E 1995 Phys. Rev. D 52 821
[2] Will C M, Wiseman A G 1996 Phys. Rev. D 54 4813
[3] Blanchet L, Faye G, Iyer B R, Sinha S 2008 Class. Quant. Grav. 25 165003
[4] Peters P C 1964 Phys. Rev. B 136 1224
[5] Peters P C, Mathews J, 1963 Phys. Rev. 131 435
[6] Gopakumar A, Iyer B R 1997 Phys. Rev. D 56 7708
[7] Gopakumar A, Iyer B R 2002 Phys. Rev. D 65 084011
[8] Brown D A, Zimmerman P J 2010 arXiv:0909.0066v2[gr-qc] 15Feb
[9] Hinder I, Herrmann F, Laguna P, Shoemaker D 2008 arXiv:0806.1037v1[gr-qc]
[10] Will C M 2005 Phys. Rev. D 71 08402
[11] Wang H, Will C M 2007 Phys. Rev. D 75 064017
[12] Konigsdorffer C, Faye G, Schafer G 2003 Phys. Rev. D 68 044004
[13] Levin J, McWillianms S C, Contreras H 2011 arXiv:1009.2533v3[gr-qc] 28 Jul 2011
[14] Thorne K S 1969 Astrophys. J. 158 997
[15] Mora T, Will C M 2004 Physical Rev. D 69 104021
[16] Zhong S Y, Liu S 2012 Acta. Phys. Sin. 61 120401 (in Chinese) [钟双英, 刘崧 2012 61 120401]
[17] Wang Y Z, Wu X, Zhong S Y 2012 Acta. Phys. Sin. 61 160401 (in Chinese) [王玉诏, 伍歆, 钟双英 2012 61 160401]
[18] Damour T 2001Phys. Rev. D 64 124013
[19] Zhong S Y, Wu X 2010 Phys. Rev. D 81 104037
[20] Zhong S Y, Wu X, Liu S Q, Deng X F 2010 Phys. Rev. D 82 124040
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[1] Kidder L E 1995 Phys. Rev. D 52 821
[2] Will C M, Wiseman A G 1996 Phys. Rev. D 54 4813
[3] Blanchet L, Faye G, Iyer B R, Sinha S 2008 Class. Quant. Grav. 25 165003
[4] Peters P C 1964 Phys. Rev. B 136 1224
[5] Peters P C, Mathews J, 1963 Phys. Rev. 131 435
[6] Gopakumar A, Iyer B R 1997 Phys. Rev. D 56 7708
[7] Gopakumar A, Iyer B R 2002 Phys. Rev. D 65 084011
[8] Brown D A, Zimmerman P J 2010 arXiv:0909.0066v2[gr-qc] 15Feb
[9] Hinder I, Herrmann F, Laguna P, Shoemaker D 2008 arXiv:0806.1037v1[gr-qc]
[10] Will C M 2005 Phys. Rev. D 71 08402
[11] Wang H, Will C M 2007 Phys. Rev. D 75 064017
[12] Konigsdorffer C, Faye G, Schafer G 2003 Phys. Rev. D 68 044004
[13] Levin J, McWillianms S C, Contreras H 2011 arXiv:1009.2533v3[gr-qc] 28 Jul 2011
[14] Thorne K S 1969 Astrophys. J. 158 997
[15] Mora T, Will C M 2004 Physical Rev. D 69 104021
[16] Zhong S Y, Liu S 2012 Acta. Phys. Sin. 61 120401 (in Chinese) [钟双英, 刘崧 2012 61 120401]
[17] Wang Y Z, Wu X, Zhong S Y 2012 Acta. Phys. Sin. 61 160401 (in Chinese) [王玉诏, 伍歆, 钟双英 2012 61 160401]
[18] Damour T 2001Phys. Rev. D 64 124013
[19] Zhong S Y, Wu X 2010 Phys. Rev. D 81 104037
[20] Zhong S Y, Wu X, Liu S Q, Deng X F 2010 Phys. Rev. D 82 124040
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