Spin-induced orbital precession and its modulation of the gravitational waveforms from merging binaries

Apostolatos, Theocharis A.; Cutler, Curt; Sussman, Gerald Jay; Thorne, Kip S.

doi:10.1103/physrevd.49.6274

Cited by 639 publications

(1,013 citation statements)

References 20 publications

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“…In general, the signal polarization may evolve as a function of time. For example, spinning black hole systems have slowly evolving, large polarization changes that track the precession of the orbital angular momentum [47]. Even nonspinning black hole systems have small, rapidly oscillating polarization changes as different multipolar orders interfere constructively and destructively [48].…”

Section: Methodsmentioning

confidence: 99%

Search for gravitational waves from intermediate mass binary black holes

Abadie¹,

Abbott²,

Abbott³

et al. 2012

Phys. Rev. D

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We present the results of a weakly modeled burst search for gravitational waves from mergers of non-spinning intermediate mass black holes (IMBH) in the total mass range 100-450 M and with the component mass ratios between 1:1 and 4:1. The search was conducted on data collected by the LIGO and Virgo detectors between November of 2005 and October of 2007. No plausible signals were observed by the search which constrains the astrophysical rates of the IMBH mergers as a function of the component masses. In the most efficiently detected bin centered on 88 + 88 M , for non-spinning sources, the rate density upper limit is 0.13 per Mpc 3 per Myr at the 90% confidence level.

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Section: Methodsmentioning

confidence: 99%

Search for gravitational waves from intermediate mass binary black holes

Abadie¹,

Abbott²,

Abbott³

et al. 2012

Phys. Rev. D

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show abstract

“…Indeed, for a binary in which only one object is spinning, BH is conserved [60] and changing the initial separation only modifies the phase of the precession of the binary.…”

Section: B Precessing Binariesmentioning

confidence: 99%

Black-hole–neutron-star mergers at realistic mass ratios: Equation of state and spin orientation effects

et al. 2013

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Black-hole-neutron-star mergers resulting in the disruption of the neutron star and the formation of an accretion disk and/or the ejection of unbound material are prime candidates for the joint detection of gravitational-wave and electromagnetic signals when the next generation of gravitational-wave detectors comes online. However, the disruption of the neutron star and the properties of the postmerger remnant are very sensitive to the parameters of the binary (mass ratio, black-hole spin, neutron star radius). In this paper, we study the impact of the radius of the neutron star and the alignment of the black-hole spin on black-hole-neutron-star mergers within the range of mass ratio currently deemed most likely for field binaries (M BH $ 7M NS ) and for black-hole spins large enough for the neutron star to disrupt (J BH =M 2 BH ¼ 0:9). We find that (i) In this regime, the merger is particularly sensitive to the radius of the neutron star, with remnant masses varying from 0:3M NS to 0:1M NS for changes of only 2 km in the NS radius; (ii) 0:01M -0:05M of unbound material can be ejected with kinetic energy * 10 51 ergs, a significant increase compared to low mass ratio, low spin binaries. This ejecta could power detectable postmerger optical and radio afterglows. (iii) Only a small fraction of the Advanced LIGO events in this parameter range have gravitational-wave signals which could offer constraints on the equation of state of the neutron star (at best $3% of the events for a single detector at design sensitivity). (iv) A misaligned black-hole spin works against disk formation, with less neutron-star material remaining outside of the black hole after merger, and a larger fraction of that material remaining in the tidal tail instead of the forming accretion disk. (v) Large kicks v kick * 300 km=s can be given to the final black hole as a result of a precessing black-hole-neutron-star merger, when the disruption of the neutron star occurs just outside or within the innermost stable spherical orbit.

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“…The model waveformĥ m , having the same physical parameters asĥ e , may not be identical tô h " m , since there may be a component of the waveform error tangent to the model waveform submanifold. The quantity FF ¼ hĥ e jĥ " m i 1 À FF is often referred to as the fitting factor [29]; MM ¼ hĥ " m jĥ b i ¼ 1 À MM is the minimal match [24]; and we refer to EFF ¼ hĥ e jĥ b i ¼ 1 À EFF as the ''effective fitting factor.'' The goal is to have any physical waveform match some model waveform in the template bank with a mismatch that is no greater than the chosen EFF (for example EFF ¼ 0:035).…”

Section: B Accuracy Requirements For Detectionmentioning

confidence: 99%

Model waveform accuracy standards for gravitational wave data analysis

2008

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Model waveforms are used in gravitational wave data analysis to detect and then to measure the properties of a source by matching the model waveforms to the signal from a detector. This paper derives accuracy standards for model waveforms which are sufficient to ensure that these data analysis applications are capable of extracting the full scientific content of the data, but without demanding excessive accuracy that would place undue burdens on the model waveform simulation community. These accuracy standards are intended primarily for broadband model waveforms produced by numerical simulations, but the standards are quite general and apply equally to such waveforms produced by analytical or hybrid analytical-numerical methods.

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Spin-induced orbital precession and its modulation of the gravitational waveforms from merging binaries

Cited by 639 publications

References 20 publications

Search for gravitational waves from intermediate mass binary black holes

Search for gravitational waves from intermediate mass binary black holes

Black-hole–neutron-star mergers at realistic mass ratios: Equation of state and spin orientation effects

Model waveform accuracy standards for gravitational wave data analysis

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