{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2018:LU5B23DNK3WZ73XSDCQFJ5AWMK","short_pith_number":"pith:LU5B23DN","schema_version":"1.0","canonical_sha256":"5d3a1d6c6d56ed9feef218a054f4166289a58ff8f3e759507cd36dd0029e9bcf","source":{"kind":"arxiv","id":"1803.00549","version":2},"attestation_state":"computed","paper":{"title":"New constraints on radii and tidal deformabilities of neutron stars from GW170817","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE","nucl-th"],"primary_cat":"gr-qc","authors_text":"Elias R. Most, J\\\"urgen Schaffner-Bielich, Luciano Rezzolla, Lukas R. Weih","submitted_at":"2018-03-01T18:36:24Z","abstract_excerpt":"We explore in a parameterized manner a very large range of physically plausible equations of state (EOSs) for compact stars for matter that is either purely hadronic or that exhibits a phase transition. In particular, we produce two classes of EOSs with and without phase transitions, each containing one million EOSs. We then impose constraints on the maximum mass, ($M < 2.16 M_{\\odot}$), and on the dimensionless tidal deformability ($\\tilde{\\Lambda} <800$) deduced from GW170817, together with recent suggestions of lower limits on $\\tilde{\\Lambda}$. Exploiting more than $10^9$ equilibrium model"},"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":"1803.00549","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"gr-qc","submitted_at":"2018-03-01T18:36:24Z","cross_cats_sorted":["astro-ph.HE","nucl-th"],"title_canon_sha256":"567672ec9e3423a3d17bdd8ede3a7160bcc14236584e96553231fc48196550d0","abstract_canon_sha256":"94bd36e4452b11324d7df68b863365d50387de23b497db68abd5368471dc18ed"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:11:37.730694Z","signature_b64":"mzBe3TzF4/hn9GwQIHu2aFCd+TRxpw7FmByrcGNZcgVvdAjS3DnU7bGcq3UJvXDXAWfduwUhnRcRXlDHQQgDAQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"5d3a1d6c6d56ed9feef218a054f4166289a58ff8f3e759507cd36dd0029e9bcf","last_reissued_at":"2026-05-18T00:11:37.730015Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:11:37.730015Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"New constraints on radii and tidal deformabilities of neutron stars from GW170817","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE","nucl-th"],"primary_cat":"gr-qc","authors_text":"Elias R. Most, J\\\"urgen Schaffner-Bielich, Luciano Rezzolla, Lukas R. Weih","submitted_at":"2018-03-01T18:36:24Z","abstract_excerpt":"We explore in a parameterized manner a very large range of physically plausible equations of state (EOSs) for compact stars for matter that is either purely hadronic or that exhibits a phase transition. In particular, we produce two classes of EOSs with and without phase transitions, each containing one million EOSs. We then impose constraints on the maximum mass, ($M < 2.16 M_{\\odot}$), and on the dimensionless tidal deformability ($\\tilde{\\Lambda} <800$) deduced from GW170817, together with recent suggestions of lower limits on $\\tilde{\\Lambda}$. Exploiting more than $10^9$ equilibrium model"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1803.00549","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":"1803.00549","created_at":"2026-05-18T00:11:37.730121+00:00"},{"alias_kind":"arxiv_version","alias_value":"1803.00549v2","created_at":"2026-05-18T00:11:37.730121+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1803.00549","created_at":"2026-05-18T00:11:37.730121+00:00"},{"alias_kind":"pith_short_12","alias_value":"LU5B23DNK3WZ","created_at":"2026-05-18T12:32:37.024351+00:00"},{"alias_kind":"pith_short_16","alias_value":"LU5B23DNK3WZ73XS","created_at":"2026-05-18T12:32:37.024351+00:00"},{"alias_kind":"pith_short_8","alias_value":"LU5B23DN","created_at":"2026-05-18T12:32:37.024351+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":4,"internal_anchor_count":4,"sample":[{"citing_arxiv_id":"1907.06597","citing_title":"Hot quark matter and (proto-) neutron stars","ref_index":86,"is_internal_anchor":true},{"citing_arxiv_id":"2510.08707","citing_title":"Neutrino diagnostics of hadron-quark phase transition in Neutron Stars","ref_index":21,"is_internal_anchor":true},{"citing_arxiv_id":"2512.19907","citing_title":"Astrophysical constraints on the cold equation of state of the strongly interacting matter","ref_index":51,"is_internal_anchor":true},{"citing_arxiv_id":"2601.07931","citing_title":"General gravitational properties of neutron stars: curvature invariants, binding energy, and trace anomaly","ref_index":2,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/LU5B23DNK3WZ73XSDCQFJ5AWMK","json":"https://pith.science/pith/LU5B23DNK3WZ73XSDCQFJ5AWMK.json","graph_json":"https://pith.science/api/pith-number/LU5B23DNK3WZ73XSDCQFJ5AWMK/graph.json","events_json":"https://pith.science/api/pith-number/LU5B23DNK3WZ73XSDCQFJ5AWMK/events.json","paper":"https://pith.science/paper/LU5B23DN"},"agent_actions":{"view_html":"https://pith.science/pith/LU5B23DNK3WZ73XSDCQFJ5AWMK","download_json":"https://pith.science/pith/LU5B23DNK3WZ73XSDCQFJ5AWMK.json","view_paper":"https://pith.science/paper/LU5B23DN","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1803.00549&json=true","fetch_graph":"https://pith.science/api/pith-number/LU5B23DNK3WZ73XSDCQFJ5AWMK/graph.json","fetch_events":"https://pith.science/api/pith-number/LU5B23DNK3WZ73XSDCQFJ5AWMK/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/LU5B23DNK3WZ73XSDCQFJ5AWMK/action/timestamp_anchor","attest_storage":"https://pith.science/pith/LU5B23DNK3WZ73XSDCQFJ5AWMK/action/storage_attestation","attest_author":"https://pith.science/pith/LU5B23DNK3WZ73XSDCQFJ5AWMK/action/author_attestation","sign_citation":"https://pith.science/pith/LU5B23DNK3WZ73XSDCQFJ5AWMK/action/citation_signature","submit_replication":"https://pith.science/pith/LU5B23DNK3WZ73XSDCQFJ5AWMK/action/replication_record"}},"created_at":"2026-05-18T00:11:37.730121+00:00","updated_at":"2026-05-18T00:11:37.730121+00:00"}