Detecting Triple Systems With Gravitational Wave Observations

Meiron, Yohai; Kocsis, Bence; Loeb, Abraham

doi:10.3847/1538-4357/834/2/200

Cited by 103 publications

(86 citation statements)

References 94 publications

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“…Doppler shifts naturally arise in a variety of circumstances. For example, if the GW-emitting binary * katiechambe@email.arizona.edu † christopher.moore@tecnico.ulisboa.pt ‡ Einstein Fellow; dgerosa@caltech.edu § nicolas.yunes@montana.edu is in the neighborhood of, or in orbit around, a third body [15][16][17], its motion in the companion's gravitational potential will be encoded in the emitted GW as a Doppler shift [18][19][20]. Another possibility is for the host galaxy of the binary to possess a peculiar acceleration due to either gravitational attraction to another neighboring galaxy [21] or the expansion of the Universe [22][23][24].…”

Section: Introductionmentioning

confidence: 99%

Frequency-domain waveform approximants capturing Doppler shifts

et al. 2019

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Gravitational wave astrophysics has only just begun, and as current detectors are upgraded and new detectors are built, many new, albeit faint, features in the signals will become accessible. One such feature is the presence of time-dependent Doppler shifts, generated by the acceleration of the center of mass of the gravitational-wave emitting system. We here develop a generic method that takes a frequency-domain, gravitational-wave model devoid of Doppler shifts and introduces modifications that incorporate them. Building upon a perturbative expansion that assumes the Doppler-shift velocity is small relative to the speed of light, the method consists of the inclusion of a single term in the Fourier phase and two terms in the Fourier amplitude. We validate the method through matches between waveforms with a Doppler shift in the time domain and waveforms constructed with our method for two toy problems: constant accelerations induced by a distant third body and Gaussian accelerations that resemble a kick profile. We find mismatches below ∼ 10 −6 for all of the astrophysically relevant cases considered, and improve further at smaller velocities. The work presented here will allow for the use of future detectors to extract new, faint features in the signal from the noise. arXiv:1809.04799v2 [gr-qc]

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Section: Introductionmentioning

confidence: 99%

Frequency-domain waveform approximants capturing Doppler shifts

et al. 2019

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“…In addition, we find that constant (ρ, z) can be a solution to Eqs. (10) and (11) when its position corresponds to an extremum of V :…”

Section: Conditions For Stable Circular Orbits In the Majumdar-pamentioning

confidence: 99%

“…As traditional problems in Newtonian gravity, there are Poincaré's three-body problem and the Kozai mechanism. In recent years, some problems related to these topics have been considered in the framework of the relativistic three body problem [5,6], in the context of resonance in a compound extreme mass ratio inspiral/massive black hole binary [7], and in gravitational wave emission induced by a third body [8][9][10][11]. If a third body itself is the target of observation, we can view it as a test body in a fixed background.…”

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confidence: 99%

Effect of a second compact object on stable circular orbits

Nakashi

Igata

2019

Phys. Rev. D

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We investigate how stable circular orbits around a main compact object appear depending on the presence of a second one by using the Majumudar-Papapetrou dihole spacetime, which consists of the two extremal Reissner-Nordström black holes with different masses. While the parameter range of the separation of the two objects is divided due to the appearance of stable circular orbits, this division depends on its mass ratio. We show that the mass ratio range separates into four parts, and we find three critical values as the boundaries. I. INTRODUCTIONRecent progress in the observation of gravitational waves supports the existence of binary black hole systems. The LIGO Scientific and Virgo collaborations have already detected gravitational waves ten times from binary black hole mergers and once from a binary neutron star merger so far [1][2][3][4]. Furthermore, since they have started the third observation run, the number of detections will increase in the future. These results imply that binary black hole systems are a quite common phenomenon in our Universe.A pure binary black hole system is a highly idealized model, around which a third object or matter distribution usually exists in realistic situations. Therefore, one of the next issues is clarifying perturbative interactions with a third body around them. As traditional problems in Newtonian gravity, there are Poincaré's three-body problem and the Kozai mechanism. In recent years, some problems related to these topics have been considered in the framework of the relativistic three body problem [5,6], in the context of resonance in a compound extreme mass ratio inspiral/massive black hole binary [7], and in gravitational wave emission induced by a third body [8][9][10][11]. If a third body itself is the target of observation, we can view it as a test body in a fixed background. As a traditional problem in Newtonian gravity, there is Euler's three-body problem, test particle motion in two fixed centers. The corresponding relativistic system is the main topic of this paper.The study of test body motion is significant for the predictions of astrophysical phenomena around a gravitational system such as a binary. In particular, the circular orbit of a test body plays some essential roles in both theory and observations. In the black hole spacetime, for instance, the bending of light due to strong gravity makes a photon orbit circular near the horizon. If the circular photon orbit is unstable, it relates to the formation of the black hole shadow. On the other hand, the sequence of stable circular massive particle orbits is relevant to accretion disks and a binary system. The innermost stable circular orbit (ISCO) radius is a distinctive one because it is identified as the inner edge of a standard accretion disk model and a compact binary switches the stage of the evolution from the inspiraling phase to the merging phase there [12,13].Actual binary black hole systems exist as highly dynamical systems so that one needs to use the numerical method to analyze the phenomen...

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“…The environment of the merger can also affect the observed waveform without directly affecting the inspiral. Such a situation arises through frame-dependent effects caused by relative motion of the GW source or an intervening gravitational potential resulting in relativistic Doppler boosting and gravitational lensing of the rest-frame GWs, as well as timedependent gravitational redshift and the Shapiro-delay [9]. In this work we consider such frame-dependent modulations, focusing on gravitational lensing of GWs.…”

Section: Introductionmentioning

confidence: 99%

Repeated gravitational lensing of gravitational waves in hierarchical black hole triples

D’Orazio

Loeb

2020

Phys. Rev. D

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We consider binary black holes (BBHs) in a hierarchical triple system where a more compact, less-massive binary is emitting detectable gravitational waves (GWs), and the tertiary is a supermassive BH at the center of a nuclear star cluster. As previous works have shown, the orbital motion of the outer binary can generate a detectable relativistic Doppler boost of the GWs emitted by the orbiting inner binary. We show here that for outer-binary orbits with a period of order one year, there can be a non-negligible probability for repeated gravitational lensing of the GWs emitted by the inner binary. Repeating gravitational lensing events could be detected by the LISA observatory as periodic GW amplitude spikes before the BBH enters the LIGO band. Such a detection would confirm the origin of some BBH mergers in nuclear star clusters while non-detection could constrain such formation channels. GW lensing also offers new testing grounds for strong gravity.

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Detecting Triple Systems With Gravitational Wave Observations

Cited by 103 publications

References 94 publications

Frequency-domain waveform approximants capturing Doppler shifts

Frequency-domain waveform approximants capturing Doppler shifts

Effect of a second compact object on stable circular orbits

Repeated gravitational lensing of gravitational waves in hierarchical black hole triples

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