{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2014:WLS7C3GULSIRGLGBKIAC2XPY5K","short_pith_number":"pith:WLS7C3GU","schema_version":"1.0","canonical_sha256":"b2e5f16cd45c91132cc152002d5df8ea82b66271f5e06790cc78d72502d88e7b","source":{"kind":"arxiv","id":"1402.6244","version":2},"attestation_state":"computed","paper":{"title":"Quasiuniversal properties of neutron star mergers","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"gr-qc","authors_text":"Alessandro Nagar, Maximiliano Ujevic, Sebastiano Bernuzzi, Simone Balmelli, Tim Dietrich","submitted_at":"2014-02-25T17:07:42Z","abstract_excerpt":"Binary neutron star mergers are studied using nonlinear 3+1 numerical relativity simulations and the analytical effective-one-body (EOB) model. The EOB model predicts quasiuniversal relations between the mass-rescaled gravitational wave frequency and the binding energy at the moment of merger, and certain dimensionless binary tidal coupling constants depending on the stars Love numbers, compactnesses and the binary mass ratio. These relations are quasiuniversal in the sense that, for a given value of the tidal coupling constant, they depend significantly neither on the equation of state nor on"},"verification_status":{"content_addressed":true,"pith_receipt":true,"author_attested":false,"weak_author_claims":0,"strong_author_claims":0,"externally_anchored":false,"storage_verified":false,"citation_signatures":0,"replication_records":0,"graph_snapshot":true,"references_resolved":false,"formal_links_present":false},"canonical_record":{"source":{"id":"1402.6244","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"gr-qc","submitted_at":"2014-02-25T17:07:42Z","cross_cats_sorted":["astro-ph.HE"],"title_canon_sha256":"8ebe41a93bc75ba0373d7381297ab2beff0245b6576b2878c0d59bda5e387f0a","abstract_canon_sha256":"6cedba9e8125cee194ffc60fbdca4d238eedaec6486bec32f733b2c83619f409"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:18:58.477428Z","signature_b64":"TzU1XPKeOQPslp1dv8uJcsLk6UYKOfr69PlDUzzsp6TMry5Z/voyoFo/aYcLfG7Bdcft2qHPfYB4MQBtpJ8gDQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"b2e5f16cd45c91132cc152002d5df8ea82b66271f5e06790cc78d72502d88e7b","last_reissued_at":"2026-05-18T02:18:58.476802Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:18:58.476802Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Quasiuniversal properties of neutron star mergers","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"gr-qc","authors_text":"Alessandro Nagar, Maximiliano Ujevic, Sebastiano Bernuzzi, Simone Balmelli, Tim Dietrich","submitted_at":"2014-02-25T17:07:42Z","abstract_excerpt":"Binary neutron star mergers are studied using nonlinear 3+1 numerical relativity simulations and the analytical effective-one-body (EOB) model. The EOB model predicts quasiuniversal relations between the mass-rescaled gravitational wave frequency and the binding energy at the moment of merger, and certain dimensionless binary tidal coupling constants depending on the stars Love numbers, compactnesses and the binary mass ratio. These relations are quasiuniversal in the sense that, for a given value of the tidal coupling constant, they depend significantly neither on the equation of state nor on"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1402.6244","kind":"arxiv","version":2},"verdict":{"id":null,"model_set":{},"created_at":null,"strongest_claim":"","one_line_summary":"","pipeline_version":null,"weakest_assumption":"","pith_extraction_headline":""},"references":{"count":0,"sample":[],"resolved_work":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57","internal_anchors":0},"formal_canon":{"evidence_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"},"aliases":[{"alias_kind":"arxiv","alias_value":"1402.6244","created_at":"2026-05-18T02:18:58.476913+00:00"},{"alias_kind":"arxiv_version","alias_value":"1402.6244v2","created_at":"2026-05-18T02:18:58.476913+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1402.6244","created_at":"2026-05-18T02:18:58.476913+00:00"},{"alias_kind":"pith_short_12","alias_value":"WLS7C3GULSIR","created_at":"2026-05-18T12:28:54.890064+00:00"},{"alias_kind":"pith_short_16","alias_value":"WLS7C3GULSIRGLGB","created_at":"2026-05-18T12:28:54.890064+00:00"},{"alias_kind":"pith_short_8","alias_value":"WLS7C3GU","created_at":"2026-05-18T12:28:54.890064+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2507.15951","citing_title":"Distinguishing Neutron Star vs. Low-Mass Black Hole Binaries with Late Inspiral & Postmerger Gravitational Waves $-$ Sensitivity to Transmuted Black Holes and Non-Annihilating Dark Matter","ref_index":101,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/WLS7C3GULSIRGLGBKIAC2XPY5K","json":"https://pith.science/pith/WLS7C3GULSIRGLGBKIAC2XPY5K.json","graph_json":"https://pith.science/api/pith-number/WLS7C3GULSIRGLGBKIAC2XPY5K/graph.json","events_json":"https://pith.science/api/pith-number/WLS7C3GULSIRGLGBKIAC2XPY5K/events.json","paper":"https://pith.science/paper/WLS7C3GU"},"agent_actions":{"view_html":"https://pith.science/pith/WLS7C3GULSIRGLGBKIAC2XPY5K","download_json":"https://pith.science/pith/WLS7C3GULSIRGLGBKIAC2XPY5K.json","view_paper":"https://pith.science/paper/WLS7C3GU","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1402.6244&json=true","fetch_graph":"https://pith.science/api/pith-number/WLS7C3GULSIRGLGBKIAC2XPY5K/graph.json","fetch_events":"https://pith.science/api/pith-number/WLS7C3GULSIRGLGBKIAC2XPY5K/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/WLS7C3GULSIRGLGBKIAC2XPY5K/action/timestamp_anchor","attest_storage":"https://pith.science/pith/WLS7C3GULSIRGLGBKIAC2XPY5K/action/storage_attestation","attest_author":"https://pith.science/pith/WLS7C3GULSIRGLGBKIAC2XPY5K/action/author_attestation","sign_citation":"https://pith.science/pith/WLS7C3GULSIRGLGBKIAC2XPY5K/action/citation_signature","submit_replication":"https://pith.science/pith/WLS7C3GULSIRGLGBKIAC2XPY5K/action/replication_record"}},"created_at":"2026-05-18T02:18:58.476913+00:00","updated_at":"2026-05-18T02:18:58.476913+00:00"}