{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:1999:2NG744ZYQTXRUX2GAWPUMP6D3K","short_pith_number":"pith:2NG744ZY","schema_version":"1.0","canonical_sha256":"d34dfe733884ef1a5f46059f463fc3da95b910058b81bde31d299c289a82b207","source":{"kind":"arxiv","id":"astro-ph/9904256","version":2},"attestation_state":"computed","paper":{"title":"Implications of massive close binaries for black hole formation and supernovae","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"N. Langer (Institut fuer Physik, S. Wellstein, Universitaet Potsdam)","submitted_at":"1999-04-20T08:09:34Z","abstract_excerpt":"The progenitor evolution of the massive X-ray binary Wray 977 is investigated using new models of massive close binary evolution. These models yield constraints on the mass limit for neutron star/black hole formation in single stars, M_BH. We argue for quasi-conservative evolution in this system, and we find M_BH > 13...21 M_sun from the existence of a neutron star in Wray 977, with the uncertainty being due to uncertainties in the treatment of convection. Our results revise earlier published much larger values of M_BH derived from the parameters of Wray 977. Then, on the basis of a grid of 37"},"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":"astro-ph/9904256","kind":"arxiv","version":2},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"1999-04-20T08:09:34Z","cross_cats_sorted":[],"title_canon_sha256":"23c9afcd5707f43f7080d46697d2e81f091ef78b58e1f208ad12ca88694c93ee","abstract_canon_sha256":"6e27f0ba473a33f4504052f0ef58cea3a90177f245d19fa0c5bd9cf082abbd84"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T14:16:40.242504Z","signature_b64":"oks4jCx3XSNl6o8iWldLiG2nM3X8bxoyMurfd66dMrf0+XSXTFa1XAiQ/DzdBQsq025CHDUdEaHttQvWrnnABw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"d34dfe733884ef1a5f46059f463fc3da95b910058b81bde31d299c289a82b207","last_reissued_at":"2026-07-04T14:16:40.242086Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T14:16:40.242086Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Implications of massive close binaries for black hole formation and supernovae","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"N. Langer (Institut fuer Physik, S. Wellstein, Universitaet Potsdam)","submitted_at":"1999-04-20T08:09:34Z","abstract_excerpt":"The progenitor evolution of the massive X-ray binary Wray 977 is investigated using new models of massive close binary evolution. These models yield constraints on the mass limit for neutron star/black hole formation in single stars, M_BH. We argue for quasi-conservative evolution in this system, and we find M_BH > 13...21 M_sun from the existence of a neutron star in Wray 977, with the uncertainty being due to uncertainties in the treatment of convection. Our results revise earlier published much larger values of M_BH derived from the parameters of Wray 977. Then, on the basis of a grid of 37"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/9904256","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/astro-ph/9904256/integrity.json","findings":[],"available":true,"detectors_run":[],"snapshot_sha256":"c28c3603d3b5d939e8dc4c7e95fa8dfce3d595e45f758748cecf8e644a296938"},"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":"astro-ph/9904256","created_at":"2026-07-04T14:16:40.242156+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/9904256v2","created_at":"2026-07-04T14:16:40.242156+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/9904256","created_at":"2026-07-04T14:16:40.242156+00:00"},{"alias_kind":"pith_short_12","alias_value":"2NG744ZYQTXR","created_at":"2026-07-04T14:16:40.242156+00:00"},{"alias_kind":"pith_short_16","alias_value":"2NG744ZYQTXRUX2G","created_at":"2026-07-04T14:16:40.242156+00:00"},{"alias_kind":"pith_short_8","alias_value":"2NG744ZY","created_at":"2026-07-04T14:16:40.242156+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":5,"internal_anchor_count":5,"sample":[{"citing_arxiv_id":"2604.21759","citing_title":"Magnetar Engines in Broad-lined Type Ic Supernovae and a Unified Picture for Magnetar-powered Stripped-envelope Supernovae","ref_index":187,"is_internal_anchor":true},{"citing_arxiv_id":"2606.30979","citing_title":"SN 2023rve: A Type II Supernova with No Nebular Oxygen","ref_index":107,"is_internal_anchor":true},{"citing_arxiv_id":"2605.21062","citing_title":"Neutron star-companion interaction in core collapse supernovae. Population synthesis based on detailed binary evolution models","ref_index":77,"is_internal_anchor":true},{"citing_arxiv_id":"2604.21759","citing_title":"Magnetar Engines in Broad-lined Type Ic Supernovae and a Unified Picture for Magnetar-powered Stripped-envelope Supernovae","ref_index":187,"is_internal_anchor":true},{"citing_arxiv_id":"2605.01200","citing_title":"Type Ib supernovae are bluer than Type Ic supernovae","ref_index":239,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/2NG744ZYQTXRUX2GAWPUMP6D3K","json":"https://pith.science/pith/2NG744ZYQTXRUX2GAWPUMP6D3K.json","graph_json":"https://pith.science/api/pith-number/2NG744ZYQTXRUX2GAWPUMP6D3K/graph.json","events_json":"https://pith.science/api/pith-number/2NG744ZYQTXRUX2GAWPUMP6D3K/events.json","paper":"https://pith.science/paper/2NG744ZY"},"agent_actions":{"view_html":"https://pith.science/pith/2NG744ZYQTXRUX2GAWPUMP6D3K","download_json":"https://pith.science/pith/2NG744ZYQTXRUX2GAWPUMP6D3K.json","view_paper":"https://pith.science/paper/2NG744ZY","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/9904256&json=true","fetch_graph":"https://pith.science/api/pith-number/2NG744ZYQTXRUX2GAWPUMP6D3K/graph.json","fetch_events":"https://pith.science/api/pith-number/2NG744ZYQTXRUX2GAWPUMP6D3K/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/2NG744ZYQTXRUX2GAWPUMP6D3K/action/timestamp_anchor","attest_storage":"https://pith.science/pith/2NG744ZYQTXRUX2GAWPUMP6D3K/action/storage_attestation","attest_author":"https://pith.science/pith/2NG744ZYQTXRUX2GAWPUMP6D3K/action/author_attestation","sign_citation":"https://pith.science/pith/2NG744ZYQTXRUX2GAWPUMP6D3K/action/citation_signature","submit_replication":"https://pith.science/pith/2NG744ZYQTXRUX2GAWPUMP6D3K/action/replication_record"}},"created_at":"2026-07-04T14:16:40.242156+00:00","updated_at":"2026-07-04T14:16:40.242156+00:00"}