Physics-Informed Priors Improve Gravitational-Wave Constraints on Neutron-Star Matter
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arXiv
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| Autori principali: | , , , , |
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| Natura: | Preprint |
| Pubblicazione: |
2025
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| _version_ | 1866909597752623104 |
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| author | Magnall, Spencer J. Ecker, Christian Rezzolla, Luciano Lasky, Paul D. Goode, Simon R. |
| author_facet | Magnall, Spencer J. Ecker, Christian Rezzolla, Luciano Lasky, Paul D. Goode, Simon R. |
| contents | Gravitational-wave astronomy shows great promise in determining nuclear physics in a regime not accessible to terrestrial experiments. We introduce physics-informed priors constrained by nuclear theory and perturbative Quantum Chromodynamics calculations, as well as astrophysical measurements of neutron-star masses and radii. When these priors are used in gravitational-wave astrophysical inference, we show a significant improvement on nuclear equation of state constraints. Applying these to the first observed gravitational-wave binary neutron-star merger GW170817, the constraints on the radius of a $1.4\,M_\odot$ neutron star improve from $R_{1.4} ={12.54^{+1.05}_{-1.54}} \, {\rm km}$ to $R_{1.4} = 12.11^{+0.91}_{-1.11} \,{\rm km}$ and those on the tidal deformability from $\tildeΛ_{1.186} < 720$ to $\tildeΛ_{1.186} = 384^{+306}_{-158}$ ($90\%$ confidence intervals) at the events measured chirp mass $\mathcal{M}=1.186\,M_\odot$. We also show these priors can be used to perform model selection between binary neutron star and neutron star-black hole mergers; in the case of GW190425, the results provide only marginal evidence with a Bayes factor $\mathcal{BF}=1.33$ in favour of the binary neutron star merger hypothesis. Given their ability to improve the astrophysical inference of binary mergers involving neutron stars, we advocate for these physics-informed priors to be used as standard in the literature and provide open-source code for reproducibility and adaptation of the method. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2504_21526 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Physics-Informed Priors Improve Gravitational-Wave Constraints on Neutron-Star Matter Magnall, Spencer J. Ecker, Christian Rezzolla, Luciano Lasky, Paul D. Goode, Simon R. High Energy Astrophysical Phenomena General Relativity and Quantum Cosmology Nuclear Theory Gravitational-wave astronomy shows great promise in determining nuclear physics in a regime not accessible to terrestrial experiments. We introduce physics-informed priors constrained by nuclear theory and perturbative Quantum Chromodynamics calculations, as well as astrophysical measurements of neutron-star masses and radii. When these priors are used in gravitational-wave astrophysical inference, we show a significant improvement on nuclear equation of state constraints. Applying these to the first observed gravitational-wave binary neutron-star merger GW170817, the constraints on the radius of a $1.4\,M_\odot$ neutron star improve from $R_{1.4} ={12.54^{+1.05}_{-1.54}} \, {\rm km}$ to $R_{1.4} = 12.11^{+0.91}_{-1.11} \,{\rm km}$ and those on the tidal deformability from $\tildeΛ_{1.186} < 720$ to $\tildeΛ_{1.186} = 384^{+306}_{-158}$ ($90\%$ confidence intervals) at the events measured chirp mass $\mathcal{M}=1.186\,M_\odot$. We also show these priors can be used to perform model selection between binary neutron star and neutron star-black hole mergers; in the case of GW190425, the results provide only marginal evidence with a Bayes factor $\mathcal{BF}=1.33$ in favour of the binary neutron star merger hypothesis. Given their ability to improve the astrophysical inference of binary mergers involving neutron stars, we advocate for these physics-informed priors to be used as standard in the literature and provide open-source code for reproducibility and adaptation of the method. |
| title | Physics-Informed Priors Improve Gravitational-Wave Constraints on Neutron-Star Matter |
| topic | High Energy Astrophysical Phenomena General Relativity and Quantum Cosmology Nuclear Theory |
| url | https://arxiv.org/abs/2504.21526 |