{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2000:GY5ZIJFDXILWM5DGBBNLB7V34B","short_pith_number":"pith:GY5ZIJFD","schema_version":"1.0","canonical_sha256":"363b9424a3ba17667466085ab0febbe06620fb05d5cac8a7ed3effd5207c344b","source":{"kind":"arxiv","id":"astro-ph/0008432","version":2},"attestation_state":"computed","paper":{"title":"Conditions for Shock Revival by Neutrino Heating in Core-Collapse Supernovae","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Garching, Germany), H.-Th. Janka (MPA","submitted_at":"2000-08-28T19:20:21Z","abstract_excerpt":"Energy deposition by neutrinos can rejuvenate the stalled bounce shock and can provide the energy for the supernova explosion of a massive star. This neutrino-heating mechanism, however, is not finally accepted or proven as the trigger of the explosion. Part of the problem is that the complexity of the hydrodynamic models often hampers a clear and simple interpretation of the results. This demands a deeper theoretical understanding of the requirements of a successful shock revival. A toy model is presented here for discussing the neutrino heating phase analytically by a time-dependent treatmen"},"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/0008432","kind":"arxiv","version":2},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2000-08-28T19:20:21Z","cross_cats_sorted":[],"title_canon_sha256":"9521dc265291426d23e50e90297c67494f50c885afef441aaaf40827c0be3db7","abstract_canon_sha256":"449b5991fd01c264bfedc3c048daed1f0376a3ca6cf1662b1fa5094fb6b5fbca"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T16:17:05.126202Z","signature_b64":"pSRTYdzGRpAUUSthRw9/dvpZDw4k8j+OcvNdCKqMk+i9GU+ZD9QG3qsycia6DQKaAbTW5wos+rN2ZI6jlGi+AA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"363b9424a3ba17667466085ab0febbe06620fb05d5cac8a7ed3effd5207c344b","last_reissued_at":"2026-07-04T16:17:05.125798Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T16:17:05.125798Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Conditions for Shock Revival by Neutrino Heating in Core-Collapse Supernovae","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Garching, Germany), H.-Th. Janka (MPA","submitted_at":"2000-08-28T19:20:21Z","abstract_excerpt":"Energy deposition by neutrinos can rejuvenate the stalled bounce shock and can provide the energy for the supernova explosion of a massive star. This neutrino-heating mechanism, however, is not finally accepted or proven as the trigger of the explosion. Part of the problem is that the complexity of the hydrodynamic models often hampers a clear and simple interpretation of the results. This demands a deeper theoretical understanding of the requirements of a successful shock revival. A toy model is presented here for discussing the neutrino heating phase analytically by a time-dependent treatmen"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0008432","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/0008432/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/0008432","created_at":"2026-07-04T16:17:05.125855+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/0008432v2","created_at":"2026-07-04T16:17:05.125855+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/0008432","created_at":"2026-07-04T16:17:05.125855+00:00"},{"alias_kind":"pith_short_12","alias_value":"GY5ZIJFDXILW","created_at":"2026-07-04T16:17:05.125855+00:00"},{"alias_kind":"pith_short_16","alias_value":"GY5ZIJFDXILWM5DG","created_at":"2026-07-04T16:17:05.125855+00:00"},{"alias_kind":"pith_short_8","alias_value":"GY5ZIJFD","created_at":"2026-07-04T16:17:05.125855+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2302.12089","citing_title":"Time integration for neutrino radiation transport using minimally implicit Runge-Kutta methods","ref_index":21,"is_internal_anchor":true},{"citing_arxiv_id":"2605.04896","citing_title":"Parameter Estimation Horizon of Core-Collapse Supernovae with Current and Next-Generation Gravitational-Wave Detectors","ref_index":11,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/GY5ZIJFDXILWM5DGBBNLB7V34B","json":"https://pith.science/pith/GY5ZIJFDXILWM5DGBBNLB7V34B.json","graph_json":"https://pith.science/api/pith-number/GY5ZIJFDXILWM5DGBBNLB7V34B/graph.json","events_json":"https://pith.science/api/pith-number/GY5ZIJFDXILWM5DGBBNLB7V34B/events.json","paper":"https://pith.science/paper/GY5ZIJFD"},"agent_actions":{"view_html":"https://pith.science/pith/GY5ZIJFDXILWM5DGBBNLB7V34B","download_json":"https://pith.science/pith/GY5ZIJFDXILWM5DGBBNLB7V34B.json","view_paper":"https://pith.science/paper/GY5ZIJFD","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/0008432&json=true","fetch_graph":"https://pith.science/api/pith-number/GY5ZIJFDXILWM5DGBBNLB7V34B/graph.json","fetch_events":"https://pith.science/api/pith-number/GY5ZIJFDXILWM5DGBBNLB7V34B/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/GY5ZIJFDXILWM5DGBBNLB7V34B/action/timestamp_anchor","attest_storage":"https://pith.science/pith/GY5ZIJFDXILWM5DGBBNLB7V34B/action/storage_attestation","attest_author":"https://pith.science/pith/GY5ZIJFDXILWM5DGBBNLB7V34B/action/author_attestation","sign_citation":"https://pith.science/pith/GY5ZIJFDXILWM5DGBBNLB7V34B/action/citation_signature","submit_replication":"https://pith.science/pith/GY5ZIJFDXILWM5DGBBNLB7V34B/action/replication_record"}},"created_at":"2026-07-04T16:17:05.125855+00:00","updated_at":"2026-07-04T16:17:05.125855+00:00"}