Eccentric pairs: Analytic gravitational waves from binary black holes in elliptic orbits

Buskirk, Dillon; Babiuc-Hamilton, M.

doi:10.1142/s0218271822501383

Cited by 3 publications

(3 citation statements)

References 93 publications

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“…We conclude our findings by endorsing the BoB model because it depends only indirectly on the numerical data, through the analytical approximations used to estimate the mass, spin and quality factor of the final black hole. The greatest strength of this model is that it provides the initial time for the merger, which is invaluable when building complete analytical waveforms as we showed in [93].…”

Section: Jcap03(2023)005mentioning

confidence: 99%

“…We also need the slope of this initial frequency Ωi , for which we do not have an analytical expression. Instead, we make an informed choice for this quantity, corresponding to the value for Ω i from our previous post-Newtonian implementation (see [93]). Table 1 contains the calculated mean values for the final spin and mass, the ringdown frequency, quality factor and damping time, together with the initial frequency and its derivative, used as initial data necessary to implement the BoB and IRS models.…”

Section: Before the Beginningmentioning

confidence: 99%

“…Again, we do not calculate Ωi , but use the same value provided in table 1 for the equal-mass binary, choice informed by our post-Newtonian evolution [93]. We recognize this ambiguity introduced by the choice in the time derivative of the initial frequency as the highest source of error in our implementation.…”

Section: Spinning It Upmentioning

confidence: 99%

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Merging black holes: assessing the performance of two analytic gravitational waves models

Buskirk

Hamilton

2023

J. Cosmol. Astropart. Phys.

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Merging black holes produce the loudest signal in the detectors. However, this is the most difficult signal to accurately predict with analytical techniques. Only computer simulations can account for the nonlinear physics during the collision, but they are inherently complex, costly, and affected by numerical errors. In order to bypass this problem, two analytical models for the merger have been developed: the Implicit Rotating Source (IRS) and the newer Backwards one Body (BoB). In this work, we assess the performance of the BoB model by comparing it with the older IRS model and with the numerical data, identifying its strengths and weaknesses. Our main finding reveals discrepancies in amplitude, but overall excellent accord in frequency. The BoB model is comparable with the IRS and NR simulations, having the added advantage that it depends only indirectly on numerical data, it accounts for spin, and it offers a seamless fit with the analytical formalisms for the inspiral. By independently evaluating and testing those models, we bring evidence of their reproducibility, thus upholding high scientific standards, and make available our implementation, enabling readers to evaluate our results themselves.

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Section: Jcap03(2023)005mentioning

confidence: 99%

Section: Before the Beginningmentioning

confidence: 99%

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Merging black holes: assessing the performance of two analytic gravitational waves models

Buskirk

Hamilton

2023

J. Cosmol. Astropart. Phys.

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Gravitational waves from mergers of Population III binary black holes: roles played by two evolution channels

Liu,

Hartwig,

Sartorio

et al. 2024

Monthly Notices of the Royal Astronomical Society

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The gravitational wave (GW) signal from binary black hole (BBH) mergers is a promising probe of Population III (Pop III) stars. To fully unleash the power of the GW probe, one important step is to understand the relative importance and features of different BBH evolution channels. We model two channels, isolated binary stellar evolution (IBSE) and nuclear star cluster-dynamical hardening (NSC-DH), in one theoretical framework based on the semi-analytical code a-sloth, under various assumptions on Pop III initial mass function (IMF), initial binary statistics and high-z nuclear star clusters (NSCs). The NSC-DH channel contributes $\sim 8-95{{\%}}$ of Pop III BBH mergers across cosmic history, with higher contributions achieved by initially wider binary stars, more top-heavy IMFs, and more abundant high-z NSCs. The dimensionless stochastic GW background (SGWB) produced by Pop III BBH mergers has peak values $\Omega ^{\rm peak}_{\rm GW}\sim 10^{-11}-8\times 10^{-11}$ around observer-frame frequencies $\nu \sim 10-100\ \rm Hz$. The Pop III contribution can be a non-negligible ($\sim 2-32{{\%}}$) component in the total SGWB at $\nu \lesssim 10\ \rm Hz$. The estimated detection rates of Pop III BBH mergers by the Einstein Telescope are $\sim 6-230\ \rm yr^{-1}$ and $\sim 30-1230\ \rm yr^{-1}$ for the NSC-DH and IBSE channels, respectively. Pop III BBH mergers in NSCs are more massive than those from IBSE, so they dominate the Pop III SGWB below 20 Hz in most cases. Besides, the detection rate of Pop III BBH mergers involving at least one intermediate-mass BH above $100\ \rm M_\odot$ by the Einstein Telescope is $\sim 0.5-200\ \rm yr^{-1}$ in NSCs but remains below $0.1\ \rm yr^{-1}$ for IBSE.

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RisingTides: An Analytic Modeling Code of Tidal Effects in Binary Neutron Star Mergers

O’Dell,

Hamilton

2024

Astronomy

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Gravitational waves produced by binary neutron star mergers offer a unique window into matter behavior under extreme conditions. In this context, we analytically model the effect of matter on gravitational waves from binary neutron star mergers. We start with a binary black hole system, leveraging the post-Newtonian formalism for the inspiral and the Backwards-one-Body model for the merger. We combine the two methods to generate a baseline waveform and we validate our results against numerical relativity simulations. Next, we integrate tidal effects in phase and amplitude to account for matter and spacetime interaction using the NRTidal model and test its accuracy against numerical relativity predictions for two equations of state, finding a mismatch around the merger. Subsequently, we lift the restriction on the coefficients to be independent of the tidal deformability and recalibrate them using the numerical relativity predictions. We obtain better fits for phase and amplitude around the merger and are able to extend the phase modeling beyond the merger. We implement our method in new open-source, user-friendly Python code, steered by a Jupyter Notebook, named RisingTides. Our research offers new perspectives on analytically modeling the effect of tides on the gravitational waves from binary neutron star mergers.

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Eccentric pairs: Analytic gravitational waves from binary black holes in elliptic orbits

Cited by 3 publications

References 93 publications

Merging black holes: assessing the performance of two analytic gravitational waves models

Merging black holes: assessing the performance of two analytic gravitational waves models

Gravitational waves from mergers of Population III binary black holes: roles played by two evolution channels

RisingTides: An Analytic Modeling Code of Tidal Effects in Binary Neutron Star Mergers

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