Overtaking collisions of solitons on superfluid<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:mmultiscripts><mml:mrow><mml:mi mathvariant="normal">He</mml:mi></mml:mrow><mml:mprescripts /><mml:mrow /><mml:mrow><mml:mn>4</mml:mn></mml:mrow><mml:mrow /><mml:mrow /></mml:mmultiscripts></mml:mrow></mml:math>films

Gopakumar, A.; Sreekumar, J.

doi:10.1103/physrevb.49.4323

Cited by 9 publications

(11 citation statements)

References 9 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…For the spinning cases, when spins are aligned with the orbital angular momentum, fits for final remnant mass from Ref. [78,79] yield E S = 0.673±0.035, E ∆ = −0.36± 0.37, E A = −0.014 ± 0.021, and E D = 0.26 ± 0.44. The source of these large errors is the difference in correcting for the normalization of the results in the papers.…”

Section: B Remnant Massmentioning

confidence: 99%

Statistical studies of spinning black-hole binaries

et al. 2010

View full text Add to dashboard Cite

We study the statistical distributions of the spins of generic black-hole binaries during the inspiral and merger, as well as the distributions of the remnant mass, spin, and recoil velocity. For the inspiral regime, we start with a random uniform distribution of spin directions S1 and S2 over the sphere and magnitudes | S1/m 2 1 | = | S2/m 2 2 | = 0.97 for different mass ratios, where Si and mi are the spin-angular momentum and mass of the ith black hole. Starting from a fiducial initial separation of ri = 50M , we perform 3.5-post-Newtonian-order evolutions down to a separation of r f = 5M , where M = m1 + m2, the total mass of the system. At this final fiducial separation, we compute the angular distribution of the spins with respect to the final orbital angular momentum, L. We perform 16 4 = 65536 simulations for six mass ratios between q = 1 and q = 1/16 and compute

show abstract

Section: B Remnant Massmentioning

confidence: 99%

Statistical studies of spinning black-hole binaries

et al. 2010

View full text Add to dashboard Cite

show abstract

“…The eccentricity is measured with respect to the frequency of the orbital motion, as in all of our past work on eccentricity removal [37][38][39][40], and also discussed in [41,42] and references therein. The eccentricity is estimated as the extrema of e ω (t) = (ω(t) − ω QC (t))/(2ω QC (t)), where ω is the frequency of the ( = 2, m = 2) mode of the waveform, and ω QC (t) is an estimate of the frequency evolution for a noneccentric binary, calculated by a smooth curve fit through the numerical data.…”

Section: Numerical Methods and Simulationsmentioning

confidence: 99%

Tracking the precession of compact binaries from their gravitational-wave signal

et al. 2011

View full text Add to dashboard Cite

We present a simple method to track the precession of a black-hole-binary system during the inspiral, using only information from the gravitational-wave (GW) signal. Our method consists of locating the frame from which the magnitudes of the ( = 2, |m| = 2) modes are maximized, which we denote the "quadrupole-aligned" frame. We demonstrate the efficacy of this method when applied to waveforms from numerical simulations. In the test case of an equal-mass nonspinning binary, our method locates the direction of the orbital angular momentum to within (∆θ , ∆ϕ) = (0.05 • , 0.2 • ). We then apply the method to a q = M 2 /M 1 = 3 binary that exhibits significant precession. In general, a spinning binary's orbital angular momentum L is not orthogonal to the orbital plane. Evidence that our method locates the direction of L rather than the normal of the orbital plane is provided by comparison with post-Newtonian (PN) results. Also, we observe that it accurately reproduces similar higher-mode amplitudes to a comparable non-precessing binary, and that the frequency of the ( = 2, |m| = 2) modes is consistent with the "total frequency" of the binary's motion. The simple form of the quadrupole-aligned waveform may be useful in attempts to analytically model the inspiral-merger-ringdown signal of precessing binaries, and in standardizing the representation of waveforms for studies of accuracy and consistency of source modelling efforts, both numerical and analytical.

show abstract

“…This can be done over the (relatively small) number of GW cycles for which we have both PN and NR waveforms. PN-NR comparisons of phase and amplitude have been performed over ∼ 10 orbits prior to merger [21,36,[42][43][44]. Comparisons for the cases we consider here are given in [22].…”

Section: Hybrid Inspiral-merger-ringdown Waveformsmentioning

confidence: 99%

“…Direct comparisons between the phase and amplitude of PN approximants and NR waveforms have been made in [21,36,[42][43][44][45][46], and we refer the reader to [22] for PN-NR comparisons of the binary configurations studied here. In this section we reframe those comparisons in the context of hybrid waveforms and mismatches.…”

Section: Comparison Between Pn and Nr During The Late Inspiralmentioning

confidence: 99%

Length requirements for numerical-relativity waveforms

et al. 2010

View full text Add to dashboard Cite

One way to produce complete inspiral-merger-ringdown gravitational waveforms from black-hole-binary systems is to connect post-Newtonian (PN) and numerical-relativity (NR) results to create ``hybrid'' waveforms. Hybrid waveforms are central to the construction of some phenomenological models for GW search templates, and for tests of GW search pipelines. The dominant error source in hybrid waveforms arises from the PN contribution, and can be reduced by increasing the number of NR GW cycles that are included in the hybrid. Hybrid waveforms are considered sufficiently accurate for GW detection if their mismatch error is below 3% (i.e., a fitting factor about 0.97). We address the question of the length requirements of NR waveforms such that the final hybrid waveforms meet this requirement, considering nonspinning binaries with q = M_2/M_1 \in [1,4] and equal-mass binaries with \chi = S_i/M_i^2 \in [-0.5,0.5]. We conclude that for the cases we study simulations must contain between three (in the equal-mass nonspinning case) and ten (the \chi = 0.5 case) orbits before merger, but there is also evidence that these are the regions of parameter space for which the least number of cycles will be needed

show abstract

Overtaking collisions of solitons on superfluidHe4films

Cited by 9 publications

References 9 publications

Statistical studies of spinning black-hole binaries

Statistical studies of spinning black-hole binaries

Tracking the precession of compact binaries from their gravitational-wave signal

Length requirements for numerical-relativity waveforms

Contact Info

Product

Resources

About