{"paper":{"title":"Inferring neutron-star Love-Q relations from gravitational waves in the hierarchical Bayesian framework","license":"http://creativecommons.org/licenses/by/4.0/","headline":"A linear relation in log space between tidal deformability and quadrupole moment describes the neutron-star Love-Q relation well enough for next-generation gravitational wave detectors.","cross_cats":["astro-ph.HE"],"primary_cat":"gr-qc","authors_text":"Jinwen Deng, Lijing Shao, Yiming Dong, Zhihao Zheng, Ziming Wang","submitted_at":"2025-10-25T03:18:25Z","abstract_excerpt":"Despite the large uncertainties in the equation of state for neutron stars (NSs), a tight universal ``Love-Q'' relation exists between their dimensionless tidal deformability, $\\Lambda$, and the dimensionless quadrupole moment, $Q$. However, this relation has not yet been directly measured through observations. Gravitational waves (GWs) emitted from binary NS (BNS) coalescences provide an avenue for such a measurement. In this study, we adopt a hierarchical Bayesian framework and combine multiple simulated GW events to measure the Love-Q relation. We simulate 1000 GW sources and select 20 even"},"claims":{"count":4,"items":[{"kind":"strongest_claim","text":"A linear relation between lnΛ and lnQ is practically sufficient to describe the Love-Q relation with the precision expected from next-generation GW detectors; the characteristic length in dynamical Chern-Simons gravity can be constrained to 10 km or less.","source":"verdict.strongest_claim","status":"machine_extracted","claim_id":"C1","attestation":"unclaimed"},{"kind":"weakest_assumption","text":"The simulated gravitational wave signals and noise properties accurately represent what real detectors will observe, and the selection of the 20 highest-SNR events with highest NS spins does not introduce bias into the recovered relation parameters.","source":"verdict.weakest_assumption","status":"machine_extracted","claim_id":"C2","attestation":"unclaimed"},{"kind":"one_line_summary","text":"Hierarchical Bayesian inference on 20 high-SNR simulated binary neutron star events shows a linear lnΛ-lnQ relation suffices and constrains dynamical Chern-Simons gravity length scale to ≤10 km.","source":"verdict.one_line_summary","status":"machine_extracted","claim_id":"C3","attestation":"unclaimed"},{"kind":"headline","text":"A linear relation in log space between tidal deformability and quadrupole moment describes the neutron-star Love-Q relation well enough for next-generation gravitational wave detectors.","source":"verdict.pith_extraction.headline","status":"machine_extracted","claim_id":"C4","attestation":"unclaimed"}],"snapshot_sha256":"c7e940f37320f7dd5d7ba611aba4ec8d562691a96f208d02e5f8a5f34b246c09"},"source":{"id":"2510.22137","kind":"arxiv","version":2},"verdict":{"id":"ddb9a552-f4b2-459b-aa22-11bb74b32d4d","model_set":{"reader":"grok-4.3"},"created_at":"2026-05-18T04:59:16.728288Z","strongest_claim":"A linear relation between lnΛ and lnQ is practically sufficient to describe the Love-Q relation with the precision expected from next-generation GW detectors; the characteristic length in dynamical Chern-Simons gravity can be constrained to 10 km or less.","one_line_summary":"Hierarchical Bayesian inference on 20 high-SNR simulated binary neutron star events shows a linear lnΛ-lnQ relation suffices and constrains dynamical Chern-Simons gravity length scale to ≤10 km.","pipeline_version":"pith-pipeline@v0.9.0","weakest_assumption":"The simulated gravitational wave signals and noise properties accurately represent what real detectors will observe, and the selection of the 20 highest-SNR events with highest NS spins does not introduce bias into the recovered relation parameters.","pith_extraction_headline":"A linear relation in log space between tidal deformability and quadrupole moment describes the neutron-star Love-Q relation well enough for next-generation gravitational wave detectors."},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/2510.22137/integrity.json","findings":[],"available":true,"detectors_run":[],"snapshot_sha256":"c28c3603d3b5d939e8dc4c7e95fa8dfce3d595e45f758748cecf8e644a296938"},"references":{"count":106,"sample":[{"doi":"","year":1946,"title":"L. Shao and K. Yagi, Sci. Bull.67, 1946 (2022), arXiv:2209.03351 [gr-qc]","work_id":"eb507d33-99f8-4b95-a965-849e8d892478","ref_index":1,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":2010,"title":"The Massive Pulsar PSR J1614-2230: Linking Quantum Chromodynamics, Gamma-ray Bursts, and Gravitational Wave Astronomy","work_id":"9c524ff4-761f-4c07-af0d-f62b5264ab31","ref_index":2,"cited_arxiv_id":"1010.5790","is_internal_anchor":true},{"doi":"","year":2013,"title":"Equation of state and neutron star properties constrained by nuclear physics and observation","work_id":"eca52225-f640-4b66-ba64-b348f40c3935","ref_index":3,"cited_arxiv_id":"1303.4662","is_internal_anchor":true},{"doi":"","year":2013,"title":"A Massive Pulsar in a Compact Relativistic Binary","work_id":"874c07aa-9e65-42e1-95db-da4b0ad68e75","ref_index":4,"cited_arxiv_id":"1304.6875","is_internal_anchor":true},{"doi":"","year":2007,"title":"Neutron Star Observations: Prognosis for Equation of State Constraints","work_id":"075de14b-8608-4eaf-8d9b-d1b4c9d4a655","ref_index":5,"cited_arxiv_id":"astro-ph/0612440","is_internal_anchor":true}],"resolved_work":106,"snapshot_sha256":"b9af9aa81379befccaedb0a376d0e7bad802e08367024d7f053ecfb18b077e4c","internal_anchors":59},"formal_canon":{"evidence_count":2,"snapshot_sha256":"d4813b2d632ff60fecb516e762ccd349de93f712681a9f1afa744a6eb3b8a6b7"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"}