Gravitational radiation from point masses in elliptical orbits: spectral analysis and orbital parameters

Moreno-Garrido, C.; Mediavilla, E.; Buitrago, J.

doi:10.1093/mnras/274.1.115

Cited by 47 publications

(83 citation statements)

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“…(6.12) is different from that obtained in Refs. [39,40], in that the above equation does not lead to periastronprecession side-bands in the GW spectrum. In Refs.…”

Section: Pn Correctionsmentioning

confidence: 95%

“…where the ℓ = 1 coefficients are This expansion resembles that of [40], but it differs in that we are here allowing for arbitrary binary inclinations via the angles (ι, β) and we are consistently expanding to the same order in eccentricity, without keeping prefactors of (1 − e) −1 . We have checked that our results in Eqs.…”

Section: Post-circular Expansion Of Time-domain Eccentric Inspirmentioning

confidence: 99%

“…We shall employ the quadrupole formalism, similar to that presented by Moreno-Garrido, Buitrago and Mediavilla [39,40], but improved through the techniques introduced by Pierro and Pinto [41,42].…”

Section: Post-circular Expansion Of Time-domain Eccentric Inspirmentioning

confidence: 99%

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Post-circular expansion of eccentric binary inspirals: Fourier-domain waveforms in the stationary phase approximation

et al. 2009

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We lay the foundations for the construction of analytic expressions for Fourier-domain gravitational waveforms produced by eccentric, inspiraling compact binaries in a post-circular or smalleccentricity approximation. The time-dependent, "plus" and "cross" polarizations are expanded in Bessel functions, which are then self-consistently re-expanded in a power series about zero initial eccentricity to eighth order. The stationary phase approximation is then employed to obtain explicit analytic expressions for the Fourier transform of the post-circular expanded, time-domain signal. We exemplify this framework by considering Newtonian-accurate waveforms, which in the post-circular scheme give rise to higher harmonics of the orbital phase and amplitude corrections both to the amplitude and the phase of the Fourier domain waveform. Such higher harmonics lead to an effective increase in the inspiral mass reach of a detector as a function of the binary's eccentricity e0 at the time when the binary enters the detector sensitivity band. Using the largest initial eccentricity allowed by our approximations (e0 < 0.4), the mass reach is found to be enhanced up to factors of approximately 5 relative to that of circular binaries for Advanced LIGO, LISA, and the proposed Einstein Telescope at a signal-to-noise ratio of ten. A post-Newtonian generalization of the post-circular scheme is also discussed, which holds the promise to provide "ready-to-use" Fourier-domain waveforms for data analysis of eccentric inspirals.

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“…(6.12) is different from that obtained in Refs. [39,40], in that the above equation does not lead to periastronprecession side-bands in the GW spectrum. In Refs.…”

Section: Pn Correctionsmentioning

confidence: 95%

Section: Post-circular Expansion Of Time-domain Eccentric Inspirmentioning

confidence: 99%

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Post-circular expansion of eccentric binary inspirals: Fourier-domain waveforms in the stationary phase approximation

et al. 2009

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“…The time-dependent waveform is computed with the help of Fourier-Bessel method in Ref. [12] and the waveform in Fourier space for arbitrary eccentricity was given in Ref [13].…”

Section: Introductionmentioning

confidence: 99%

First order post-Newtonian gravitational waveforms of binaries on eccentric orbits with Hansen coefficients

2015

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The inspiral and merger of supermassive black hole binary systems with high orbital eccentricity are among the promising sources of the advanced gravitational wave observatories. In this paper we derive analytic ready-to-use first post-Newtonian eccentric waveform in Fourier domain with the use of Hansen coefficients. Introducing generic perturbations of celestial mechanics we have generalized the Hansen expansion to the first post-Newtonian order which are then used to express the waveforms. Taking into account the high eccentricity of the orbit leads to the appearance of secular terms in the waveform which are eliminated with the introduction of a phase shift. The waveforms have a systematic structure and as our main result these are expressed in a tabular form.

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“…So far this study has been mainly focused on such sources as supernovae explosions, pulsars and compact binaries. In particular these latter sources have been widely investigated throughout all the stages of their evolution [3][4][5][6][7].…”

Section: Introductionmentioning

confidence: 99%

Gravitational Radiation From Triple Star Systems

Montanari

Calura

Fortini

1999

Int. J. Mod. Phys. A

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We have studied the main features of the gravitational radiation generated by an astrophysical system constituted of three compact objects attracting one another (only via gravitational interaction) in such a manner that stable orbits do exist. We have limited our analysis to systems that can be treated with perturbative methods. We show the profile of the gravitational waves emitted by such systems. These results can be useful within the framework of the new gravitational astronomy which will be made feasible by means of the new generation of gravitational detectors such as LISA in a no longer far future. PACS number(s): 04.30. Db,

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Gravitational radiation from point masses in elliptical orbits: spectral analysis and orbital parameters

Cited by 47 publications

References 0 publications

Post-circular expansion of eccentric binary inspirals: Fourier-domain waveforms in the stationary phase approximation

Post-circular expansion of eccentric binary inspirals: Fourier-domain waveforms in the stationary phase approximation

First order post-Newtonian gravitational waveforms of binaries on eccentric orbits with Hansen coefficients

Gravitational Radiation From Triple Star Systems

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