{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2024:NOW6VSC2UHHAUJFTGU7A64TAL6","short_pith_number":"pith:NOW6VSC2","schema_version":"1.0","canonical_sha256":"6badeac85aa1ce0a24b3353e0f72605fb93677bc3aadce12c6d999f9c4d35471","source":{"kind":"arxiv","id":"2409.02058","version":1},"attestation_state":"computed","paper":{"title":"It's written in the massive stars: The role of stellar physics in the formation of black holes","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE","gr-qc"],"primary_cat":"astro-ph.SR","authors_text":"E. Laplace, F. R. N. Schneider, Ph. Podsiadlowski","submitted_at":"2024-09-03T17:07:23Z","abstract_excerpt":"In the age of gravitational-wave (GW) sources and newly discovered local black holes (BH) and neutron stars (NS), understanding the fate of stars is a key question. Not every massive star is expected to successfully explode as a supernova and leave behind a NS; some stars form BHs. The remnant depends on explosion physics but also on the final core structure, often summarized by the compactness parameter or iron core mass, where high values have been linked to BH formation. Several groups have reported similar patterns in these parameters as a function of mass, characterized by a prominent com"},"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":"2409.02058","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2024-09-03T17:07:23Z","cross_cats_sorted":["astro-ph.HE","gr-qc"],"title_canon_sha256":"1c294b58813875c27c7828fb988b256eed350f3bb5c2f23d4dd3bb2f6b9bf909","abstract_canon_sha256":"0acc47a52a4dc5d82781dd96e75e5eeafce7ba47be5816e04a58aa4bdff51ed7"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T10:28:21.138712Z","signature_b64":"XH20zsayMKpczqMn9Qh8gVA/bZKMb5rAf2ZNuaJu5AHCoMhmYxUKpRXS/78dhe/9BNjjQqip2Ri8hKpYI8koAg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"6badeac85aa1ce0a24b3353e0f72605fb93677bc3aadce12c6d999f9c4d35471","last_reissued_at":"2026-07-05T10:28:21.138168Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T10:28:21.138168Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"It's written in the massive stars: The role of stellar physics in the formation of black holes","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE","gr-qc"],"primary_cat":"astro-ph.SR","authors_text":"E. Laplace, F. R. N. Schneider, Ph. Podsiadlowski","submitted_at":"2024-09-03T17:07:23Z","abstract_excerpt":"In the age of gravitational-wave (GW) sources and newly discovered local black holes (BH) and neutron stars (NS), understanding the fate of stars is a key question. Not every massive star is expected to successfully explode as a supernova and leave behind a NS; some stars form BHs. The remnant depends on explosion physics but also on the final core structure, often summarized by the compactness parameter or iron core mass, where high values have been linked to BH formation. Several groups have reported similar patterns in these parameters as a function of mass, characterized by a prominent com"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2409.02058","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/2409.02058/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":"2409.02058","created_at":"2026-07-05T10:28:21.138230+00:00"},{"alias_kind":"arxiv_version","alias_value":"2409.02058v1","created_at":"2026-07-05T10:28:21.138230+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2409.02058","created_at":"2026-07-05T10:28:21.138230+00:00"},{"alias_kind":"pith_short_12","alias_value":"NOW6VSC2UHHA","created_at":"2026-07-05T10:28:21.138230+00:00"},{"alias_kind":"pith_short_16","alias_value":"NOW6VSC2UHHAUJFT","created_at":"2026-07-05T10:28:21.138230+00:00"},{"alias_kind":"pith_short_8","alias_value":"NOW6VSC2","created_at":"2026-07-05T10:28:21.138230+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":4,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2606.11927","citing_title":"Building three-dimensional giant stellar models for common envelope simulations","ref_index":149,"is_internal_anchor":false},{"citing_arxiv_id":"2606.27193","citing_title":"Stellar black hole binaries from two common envelope evolution phases in triple stellar systems","ref_index":157,"is_internal_anchor":false},{"citing_arxiv_id":"2605.12356","citing_title":"Reproducing morphological features in the supernova remnant G11.2-0.3 by simulating jittering jets","ref_index":154,"is_internal_anchor":false},{"citing_arxiv_id":"2604.22605","citing_title":"The Effect of Mass Loss and Convective Overshooting on the Pre-Collapse Structure, Composition, and Neutrino Emission of Red Supergiants","ref_index":71,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/NOW6VSC2UHHAUJFTGU7A64TAL6","json":"https://pith.science/pith/NOW6VSC2UHHAUJFTGU7A64TAL6.json","graph_json":"https://pith.science/api/pith-number/NOW6VSC2UHHAUJFTGU7A64TAL6/graph.json","events_json":"https://pith.science/api/pith-number/NOW6VSC2UHHAUJFTGU7A64TAL6/events.json","paper":"https://pith.science/paper/NOW6VSC2"},"agent_actions":{"view_html":"https://pith.science/pith/NOW6VSC2UHHAUJFTGU7A64TAL6","download_json":"https://pith.science/pith/NOW6VSC2UHHAUJFTGU7A64TAL6.json","view_paper":"https://pith.science/paper/NOW6VSC2","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2409.02058&json=true","fetch_graph":"https://pith.science/api/pith-number/NOW6VSC2UHHAUJFTGU7A64TAL6/graph.json","fetch_events":"https://pith.science/api/pith-number/NOW6VSC2UHHAUJFTGU7A64TAL6/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/NOW6VSC2UHHAUJFTGU7A64TAL6/action/timestamp_anchor","attest_storage":"https://pith.science/pith/NOW6VSC2UHHAUJFTGU7A64TAL6/action/storage_attestation","attest_author":"https://pith.science/pith/NOW6VSC2UHHAUJFTGU7A64TAL6/action/author_attestation","sign_citation":"https://pith.science/pith/NOW6VSC2UHHAUJFTGU7A64TAL6/action/citation_signature","submit_replication":"https://pith.science/pith/NOW6VSC2UHHAUJFTGU7A64TAL6/action/replication_record"}},"created_at":"2026-07-05T10:28:21.138230+00:00","updated_at":"2026-07-05T10:28:21.138230+00:00"}