Non-adiabatic dynamics of eccentric black-hole binaries in post-Newtonian theory
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arXiv
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| Auteurs principaux: | , , , |
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| Format: | Preprint |
| Publié: |
2025
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| _version_ | 1866911583029952512 |
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| author | Fumagalli, Giulia Loutrel, Nicholas Gerosa, Davide Boschini, Matteo |
| author_facet | Fumagalli, Giulia Loutrel, Nicholas Gerosa, Davide Boschini, Matteo |
| contents | Eccentric black-hole binaries are among the most awaited sources of gravitational waves, yet their dynamics lack a consistent framework that provides a detailed and physically robust evolutionary description due to gauge issues. We present a new set of non-orbit-averaged equations, free from radiation-reaction gauge ambiguities, that accurately describe the evolution of orbital elements for eccentric, non-spinning black-hole binaries. We derive these equations by mapping the Keplerian orbital elements to a new set of characteristic parameters using energy and angular momentum definitions combined with near-identity transformations. The resulting framework is valid for arbitrary eccentricities, including parabolic and hyperbolic limits. Using this framework, we demonstrate the strictly observable effects of the non-adiabatic emission of gravitational waves -- characteristic of eccentric binaries -- on the orbital parameters. Furthermore, we assess the regime of validity of the widely used orbit-averaged equations first derived by Peters in 1964. Importantly, their breakdown becomes evident at the first pericenter passage, implying that the validity of the orbit-averaged approximation cannot be inferred solely from binary initial conditions. The formalism we introduce, accurate up to 2.5 post-Newtonian order, aims to provide a robust tool for making reliable astrophysical predictions and accurately interpreting current and future gravitational wave data, paving the way for deeper insights into the dynamics of eccentric black hole binaries. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2502_06952 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Non-adiabatic dynamics of eccentric black-hole binaries in post-Newtonian theory Fumagalli, Giulia Loutrel, Nicholas Gerosa, Davide Boschini, Matteo General Relativity and Quantum Cosmology High Energy Astrophysical Phenomena Eccentric black-hole binaries are among the most awaited sources of gravitational waves, yet their dynamics lack a consistent framework that provides a detailed and physically robust evolutionary description due to gauge issues. We present a new set of non-orbit-averaged equations, free from radiation-reaction gauge ambiguities, that accurately describe the evolution of orbital elements for eccentric, non-spinning black-hole binaries. We derive these equations by mapping the Keplerian orbital elements to a new set of characteristic parameters using energy and angular momentum definitions combined with near-identity transformations. The resulting framework is valid for arbitrary eccentricities, including parabolic and hyperbolic limits. Using this framework, we demonstrate the strictly observable effects of the non-adiabatic emission of gravitational waves -- characteristic of eccentric binaries -- on the orbital parameters. Furthermore, we assess the regime of validity of the widely used orbit-averaged equations first derived by Peters in 1964. Importantly, their breakdown becomes evident at the first pericenter passage, implying that the validity of the orbit-averaged approximation cannot be inferred solely from binary initial conditions. The formalism we introduce, accurate up to 2.5 post-Newtonian order, aims to provide a robust tool for making reliable astrophysical predictions and accurately interpreting current and future gravitational wave data, paving the way for deeper insights into the dynamics of eccentric black hole binaries. |
| title | Non-adiabatic dynamics of eccentric black-hole binaries in post-Newtonian theory |
| topic | General Relativity and Quantum Cosmology High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2502.06952 |