Efficient effective one body time-domain gravitational waveforms
| Autor: | Alessandro Nagar, Piero Rettegno |
|---|---|
| Přispěvatelé: | Institut des Hautes Etudes Scientifiques (IHES), IHES |
| Jazyk: | angličtina |
| Rok vydání: | 2019 |
| Předmět: |
Gravitational waves
effective-one-body Differential equation Phase (waves) spin angular momentum 01 natural sciences Gravitational waves 0103 physical sciences black hole Waveform Time domain 010306 general physics orbit Physics 010308 nuclear & particles physics Gravitational wave Mathematical analysis gravitational radiation differential equations binary: compact Black hole Ordinary differential equation gravitational radiation: emission Orbit (dynamics) neutron star: binary: coalescence [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc] effective-one-body |
| Zdroj: | Phys.Rev.D Phys.Rev.D, 2019, 99 (2), pp.021501. ⟨10.1103/PhysRevD.99.021501⟩ Physical Review D Physical Review D, American Physical Society, 2019, 99 (2), pp.021501. ⟨10.1103/PhysRevD.99.021501⟩ |
| ISSN: | 1550-7998 1550-2368 |
| DOI: | 10.1103/PhysRevD.99.021501⟩ |
| Popis: | International audience; Computationally efficient waveforms are of central importance for gravitational wave data analysis of inspiraling and coalescing compact binaries. We show that the postadiabatic (PA) approximation to the effective one-body (EOB) description of the binary dynamics, when pushed to high order, allows one to accurately and efficiently compute the waveform of coalescing binary neutron stars (BNSs) or black holes (BBHs) up to a few orbits before merger. This is accomplished bypassing the usual need of numerically solving the relative EOB dynamics described by a set of ordinary differential equations (ODEs). Under the assumption that radiation reaction is small, Hamilton’s equations for the momenta can be solved analytically for given values of the relative separation. Time and orbital phase are then recovered by simple numerical quadratures. For the least adiabatic BBH case, equal-mass, quasiextremal spins antialigned with the orbital angular momentum, 6PA/8PA orders are able to generate waveforms that accumulate less than 10-3 rad of phase difference with respect to the complete EOB ones up to ∼3 orbits before merger. Analogous results hold for BNSs. The PA waveform generation is extremely efficient: for a standard BNS system from 10 Hz, a nonoptimized Matlab implementation of the TEOBResumS EOB model in the PA approximation is almost 100 times faster (∼0.09 s) than the corresponding C++ code based on a standard ODE solver. Once optimized further, our approach will allow us to (i) avoid the use of the fast, but often inaccurate, post-Newtonian inspiral waveforms, drastically reducing the impact of systematics due to inspiral waveform modeling, and (ii) alleviate the need of constructing EOB waveform surrogates to be used in parameter estimation codes. |
| Databáze: | OpenAIRE |
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