{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2009:ITJZBVCM3FCP4CN2U7RLVEHK4D","short_pith_number":"pith:ITJZBVCM","schema_version":"1.0","canonical_sha256":"44d390d44cd944fe09baa7e2ba90eae0f26e9264c367dbdbe83a07daac94f02f","source":{"kind":"arxiv","id":"0911.3535","version":1},"attestation_state":"computed","paper":{"title":"Tidal deformability of neutron stars with realistic equations of state and their gravitational wave signatures in binary inspiral","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["gr-qc"],"primary_cat":"astro-ph.HE","authors_text":"Benjamin D. Lackey, Jocelyn S. Read, Ryan N. Lang, Tanja Hinderer","submitted_at":"2009-11-18T18:09:22Z","abstract_excerpt":"The early part of the gravitational wave signal of binary neutron star inspirals can potentially yield robust information on the nuclear equation of state. The influence of a star's internal structure on the waveform is characterized by a single parameter: the tidal deformability lambda, which measures the star's quadrupole deformation in response to the companion's perturbing tidal field. We calculate lambda for a wide range of equations of state and find that the value of lambda spans an order of magnitude for the range of equation of state models considered.\n  An analysis of the feasibility"},"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":"0911.3535","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2009-11-18T18:09:22Z","cross_cats_sorted":["gr-qc"],"title_canon_sha256":"67a998c701ab9ecaf41f4f032b2742bc38541e05429bbb819e8dfd46fe562c4e","abstract_canon_sha256":"442a13580c20f0b20ca9956785882152dd6a53aa1838acddbce39796682e4a15"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T04:27:57.248940Z","signature_b64":"HYBP+NOt6ImZunCvTMFILNGRwHz5CZAGvkNZ967UP8pLg8dqJ53Qi7OEOqf86Wb/0ePVDV496deGdMgvKeW6Cg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"44d390d44cd944fe09baa7e2ba90eae0f26e9264c367dbdbe83a07daac94f02f","last_reissued_at":"2026-05-18T04:27:57.248159Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T04:27:57.248159Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Tidal deformability of neutron stars with realistic equations of state and their gravitational wave signatures in binary inspiral","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["gr-qc"],"primary_cat":"astro-ph.HE","authors_text":"Benjamin D. Lackey, Jocelyn S. Read, Ryan N. Lang, Tanja Hinderer","submitted_at":"2009-11-18T18:09:22Z","abstract_excerpt":"The early part of the gravitational wave signal of binary neutron star inspirals can potentially yield robust information on the nuclear equation of state. The influence of a star's internal structure on the waveform is characterized by a single parameter: the tidal deformability lambda, which measures the star's quadrupole deformation in response to the companion's perturbing tidal field. We calculate lambda for a wide range of equations of state and find that the value of lambda spans an order of magnitude for the range of equation of state models considered.\n  An analysis of the feasibility"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"0911.3535","kind":"arxiv","version":1},"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":"0911.3535","created_at":"2026-05-18T04:27:57.248279+00:00"},{"alias_kind":"arxiv_version","alias_value":"0911.3535v1","created_at":"2026-05-18T04:27:57.248279+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.0911.3535","created_at":"2026-05-18T04:27:57.248279+00:00"},{"alias_kind":"pith_short_12","alias_value":"ITJZBVCM3FCP","created_at":"2026-05-18T12:26:00.592388+00:00"},{"alias_kind":"pith_short_16","alias_value":"ITJZBVCM3FCP4CN2","created_at":"2026-05-18T12:26:00.592388+00:00"},{"alias_kind":"pith_short_8","alias_value":"ITJZBVCM","created_at":"2026-05-18T12:26:00.592388+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":12,"internal_anchor_count":7,"sample":[{"citing_arxiv_id":"1907.04654","citing_title":"Phase transitions in neutron stars and their links to gravitational waves","ref_index":209,"is_internal_anchor":true},{"citing_arxiv_id":"1907.05921","citing_title":"Matter And Gravitation In Collisions of heavy ions and neutron stars: equation of state","ref_index":59,"is_internal_anchor":true},{"citing_arxiv_id":"2508.06245","citing_title":"Generalized Perturbed Kepler Problem: Gravitational Wave Imprints from Eccentric Compact Binaries","ref_index":39,"is_internal_anchor":true},{"citing_arxiv_id":"2511.19626","citing_title":"Universal Relations with Dynamical Tides","ref_index":15,"is_internal_anchor":true},{"citing_arxiv_id":"2512.02484","citing_title":"Properties of Stable Massive Quark Stars in Holography","ref_index":78,"is_internal_anchor":true},{"citing_arxiv_id":"2605.14447","citing_title":"Bayesian analysis of density profile of light dark matter elucidating the properties of dark matter admixed neutron stars in the presence of hyperons","ref_index":112,"is_internal_anchor":true},{"citing_arxiv_id":"2603.22467","citing_title":"High-order effective-one-body tidal interactions and gravitational scattering","ref_index":14,"is_internal_anchor":true},{"citing_arxiv_id":"2605.09206","citing_title":"Neutron stars in a conservative $f(R,T)$ gravity","ref_index":44,"is_internal_anchor":false},{"citing_arxiv_id":"2604.24949","citing_title":"A Physics Informed Bayesian Neural Network for the Neutron Star Equation of State","ref_index":50,"is_internal_anchor":false},{"citing_arxiv_id":"2604.20159","citing_title":"A Poincar\\'e-covariant study of strange quark stars","ref_index":52,"is_internal_anchor":false},{"citing_arxiv_id":"2604.04560","citing_title":"Neutron star with dark matter using vector portal","ref_index":25,"is_internal_anchor":false},{"citing_arxiv_id":"2605.02633","citing_title":"Axial tidal Love numbers of black holes in matter environments","ref_index":10,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/ITJZBVCM3FCP4CN2U7RLVEHK4D","json":"https://pith.science/pith/ITJZBVCM3FCP4CN2U7RLVEHK4D.json","graph_json":"https://pith.science/api/pith-number/ITJZBVCM3FCP4CN2U7RLVEHK4D/graph.json","events_json":"https://pith.science/api/pith-number/ITJZBVCM3FCP4CN2U7RLVEHK4D/events.json","paper":"https://pith.science/paper/ITJZBVCM"},"agent_actions":{"view_html":"https://pith.science/pith/ITJZBVCM3FCP4CN2U7RLVEHK4D","download_json":"https://pith.science/pith/ITJZBVCM3FCP4CN2U7RLVEHK4D.json","view_paper":"https://pith.science/paper/ITJZBVCM","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=0911.3535&json=true","fetch_graph":"https://pith.science/api/pith-number/ITJZBVCM3FCP4CN2U7RLVEHK4D/graph.json","fetch_events":"https://pith.science/api/pith-number/ITJZBVCM3FCP4CN2U7RLVEHK4D/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/ITJZBVCM3FCP4CN2U7RLVEHK4D/action/timestamp_anchor","attest_storage":"https://pith.science/pith/ITJZBVCM3FCP4CN2U7RLVEHK4D/action/storage_attestation","attest_author":"https://pith.science/pith/ITJZBVCM3FCP4CN2U7RLVEHK4D/action/author_attestation","sign_citation":"https://pith.science/pith/ITJZBVCM3FCP4CN2U7RLVEHK4D/action/citation_signature","submit_replication":"https://pith.science/pith/ITJZBVCM3FCP4CN2U7RLVEHK4D/action/replication_record"}},"created_at":"2026-05-18T04:27:57.248279+00:00","updated_at":"2026-05-18T04:27:57.248279+00:00"}