On the Eccentricity Distribution of Coalescing Black Hole Binaries Driven by the Kozai Mechanism in Globular Clusters

By LinQing Wen. 2002

296 citations recorded by the source corpus.

In a globular cluster, hierarchical triple black hole systems can be produced through binary-binary interaction. It has been proposed recently that the Kozai mechanism could drive the inner binary of the triple system to merge before it is interrupted by interactions with other field stars. We investigate qualitatively and numerically the evolution of the eccentricities in these binaries under gravitational radiation (GR) reaction. We predict that ~30% of the systems will possess eccentricities greater than 0.1 when their emitted gravitational waves pass through 10 Hz frequency. The implications for gravitational wave detection, especially the relevance to data analyses for broadband laser interferometer gravitational wave detectors, are discussed.

Subfields: Astronomy and Astrophysics, Geophysics

View Paper: https://www.semanticscholar.org/paper/ce927836c22d0043b9c739794fa547a9f73d13f6

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Citations in the corpus

The Eccentric Kozai-Lidov Effect and Its Applications (2016, methodology): “This perhaps can lead to a detectable signal using LIGO5 and VIRGO6 (e.g., Wen (2003) and Naoz et al. (2013b), but see Mandel et al. (2008) and O’Leary et al. (2006)).”
Lidov–Kozai Cycles with Gravitational Radiation: Merging Black Holes in Isolated Triple Systems (2016, background): “Wen (2003) gives an expression for the peak frequency of emission from an eccentric orbit: ( ) ( ) ( ) ( ) p = +f e GM e a 1 1 , 36mGW in in in 1.1954 in 1.5 where = - e1 in 2 .”
Timescales of Kozai-Lidov oscillations at quadrupole and octupole order in the test particle limit (2015, background): “In the general case of three massive bodies this component of angular momentum is not conserved, although other, more complicated, integrals of motion may be derived from the geometrical relation instead (e.g., Wen 2003).”
Eccentric Black Hole Gravitational-wave Capture Sources in Galactic Nuclei: Distribution of Binary Parameters (2017, background): “Further, BH binaries can capture triple companions via dynamical encounters in dense stellar systems such as globular clusters (GCs; Wen 2003; Thompson 2011; Aarseth 2012; Antonini et al. 2014, 2016; Breivik et al. 2016; Rodriguez et al. 2016a, 2016b) and in isolated triples in the field (Silsbee &…”
Eccentric Black Hole Mergers in Dense Star Clusters: The Role of Binary–Binary Encounters (2018, methodology): “…eccentricity at a particular GW frequency, we numerically solve for the orbital properties of the binary at a given eccentric peak frequency as in Wen (2003): a(e) = 1 1 − e2 [ GM π (1 + e)1.1954 fGW ]2/3 , (19) 4 In recent work, this category of GW inspirals is often referred to as “three-body…”
The astrophysics of nanohertz gravitational waves (2018, background): “Eccentric systems emit at the orbital frequency itself as well as at higher harmonics (e. g., Wen 2003).”
SECULAR EVOLUTION OF COMPACT BINARIES NEAR MASSIVE BLACK HOLES: GRAVITATIONAL WAVE SOURCES AND OTHER EXOTICA (2012, methodology): “Wen (2003) showed that, in the contest of stellar black hole triples that might form in the core of globular clusters, for some particular configurations it is possible that the inner bi- nary GW frequency enters the LIGO observational band before the maximum eccentricity expected for the Kozai…”
Black Hole Mergers From Globular Clusters Observable by LISA I: Eccentric Sources Originating From Relativistic N-body Dynamics (2018, methodology): “For this we used the approximation fGW = π −1 √ 2Gm/r3p , where rp is the pericentre distance at the time of formation of the merging BBH (e.g., Wen 2003; Samsing 2017).”
Rapid Eccentricity Oscillations and the Mergers of Compact Objects in Hierarchical Triples (2013, background): “Although the orbit will have substantially circularized by the time the two objects of the inner binary come within 10 RSch of each other, the orbit nevertheless retains a non-negligible eccentricity (e1 ∼ 0.1) in most systems (Wen 2003; Gould 2011).”
Formation and Evolution of Compact-object Binaries in AGN Disks (2019, background): “Figure 18 shows the dominant hardening mechanism as a function of distance from the SMBH and the peak GW frequency fGW (Wen 2003) at two snapshots, 1Myr (top panel) and 10Myr (bottom panel), for the fiducial model assuming an eccentricity of 0.7.”
BLACK HOLE TRIPLE DYNAMICS: A BREAKDOWN OF THE ORBIT AVERAGE APPROXIMATION AND IMPLICATIONS FOR GRAVITATIONAL WAVE DETECTIONS (2013, methodology): “The lower limit of 0.2 AU corresponds roughly to the minimum value of the semi-major axis distribution of BH binaries obtained via Monte Carlo simulations in Downing et al. (2010); the upper limit of 30 AU is the same adopted in Wen (2003).”
THE FORMATION OF ECCENTRIC COMPACT BINARY INSPIRALS AND THE ROLE OF GRAVITATIONAL WAVE EMISSION IN BINARY–SINGLE STELLAR ENCOUNTERS (2013, methodology): “To quantify the number of eccentric binary mergers in our scattering experiments, we use an approximate form for the gravitational peak frequency (Wen 2003), fGW = 1 π √ Gmtot a3 (1 + e)1.1954 (1 − e2)1.5 , (43) where √ a3/Gmtot is the orbital time, Torb.”
BLACK HOLE MERGERS AND BLUE STRAGGLERS FROM HIERARCHICAL TRIPLES FORMED IN GLOBULAR CLUSTERS (2015, methodology): “Interestingly, such mergers have been suggested as a channel for the formation of compact-object mergers (Miller & Hamilton 2002; Wen 2003; Arca-Sedda 2016), and more recently as a channel for the formation of BSSs through mass transfer and merger (Perets & Fabrycky 2009; Leigh & Sills 2011; Geller…”
Secular Dynamics in Hierarchical Three-Body Systems (2011, background): “ddition, Kozai-Lidov cycling has been suggested to play an important role in both the growth of black holes at the centers of dense star clusters and the formation of short-period binary black holes (Wen 2003; Miller and Hamilton 2002; Blaes etal. 2002). Recently, Ivanova etal. (2010) showed that th”
Binary Black Hole Mergers from Field Triples: Properties, Rates, and the Impact of Stellar Evolution (2017, methodology): “…binaries emit a GW signal with a broad spectrum of frequencies; we compute a proxy for the GW frequency of our merging binaries as the frequency corresponding to the harmonic which leads to the maximal emission of GW radiation (Wen 2003): fGW = √ G(m1 +m2) π (1 + e1) 1.195 [a1 (1− e21)] 1.5 .”
Gravitational waves from scattering of stellar-mass black holes in galactic nuclei (2008, background): “Their calculations also included secular effects which could result in mergers with higher eccentricity (Wen 2003).”