{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2005:P3LEWPPOK6ZAMXVGPNWDIGMO53","short_pith_number":"pith:P3LEWPPO","schema_version":"1.0","canonical_sha256":"7ed64b3dee57b2065ea67b6c34198eeec18b7506df1a732213419086fc82ca93","source":{"kind":"arxiv","id":"astro-ph/0502470","version":2},"attestation_state":"computed","paper":{"title":"Neutrino-Dominated Accretion and Supernovae","license":"","headline":"","cross_cats":["hep-ph"],"primary_cat":"astro-ph","authors_text":"Kazunori Kohri, Ramesh Narayan, Tsvi Piran","submitted_at":"2005-02-22T23:31:24Z","abstract_excerpt":"We suggest that part of the infalling material during the core-collapse of a massive star goes into orbit around the compact core to form a hot, dense, centrifugally-supported accretion disk whose evolution is strongly influenced by neutrino interactions. Under a wide range of conditions, this neutrino-dominated accretion flow will be advection-dominated and will develop a substantial outflowing wind. We estimate the energy carried out in the wind and find that it exceeds $10^{50}$ erg for a wide range of parameters and even exceeds 10^{51} erg for reasonable parameter choices. We propose that"},"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/0502470","kind":"arxiv","version":2},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2005-02-22T23:31:24Z","cross_cats_sorted":["hep-ph"],"title_canon_sha256":"8272d935e10f1cfc1856638d8c71c7e4c0aa1a5cb37abda0e44999add5be4d76","abstract_canon_sha256":"361c75bc3444a2aa76699ab8a49749b22edf8cbad950d0ff836c5f87de19e232"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T16:50:52.593136Z","signature_b64":"sjT+Ro7LxlMYiDvhSkJnSKniKaZHU9WceT1Saf1OzHLvSlLFIeGs7c7GMRGAi1d+KKdMLE7+gqjzEG0rO8O+CA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"7ed64b3dee57b2065ea67b6c34198eeec18b7506df1a732213419086fc82ca93","last_reissued_at":"2026-07-04T16:50:52.592793Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T16:50:52.592793Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Neutrino-Dominated Accretion and Supernovae","license":"","headline":"","cross_cats":["hep-ph"],"primary_cat":"astro-ph","authors_text":"Kazunori Kohri, Ramesh Narayan, Tsvi Piran","submitted_at":"2005-02-22T23:31:24Z","abstract_excerpt":"We suggest that part of the infalling material during the core-collapse of a massive star goes into orbit around the compact core to form a hot, dense, centrifugally-supported accretion disk whose evolution is strongly influenced by neutrino interactions. Under a wide range of conditions, this neutrino-dominated accretion flow will be advection-dominated and will develop a substantial outflowing wind. We estimate the energy carried out in the wind and find that it exceeds $10^{50}$ erg for a wide range of parameters and even exceeds 10^{51} erg for reasonable parameter choices. We propose that"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0502470","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/0502470/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/0502470","created_at":"2026-07-04T16:50:52.592848+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/0502470v2","created_at":"2026-07-04T16:50:52.592848+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/0502470","created_at":"2026-07-04T16:50:52.592848+00:00"},{"alias_kind":"pith_short_12","alias_value":"P3LEWPPOK6ZA","created_at":"2026-07-04T16:50:52.592848+00:00"},{"alias_kind":"pith_short_16","alias_value":"P3LEWPPOK6ZAMXVG","created_at":"2026-07-04T16:50:52.592848+00:00"},{"alias_kind":"pith_short_8","alias_value":"P3LEWPPO","created_at":"2026-07-04T16:50:52.592848+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2502.02077","citing_title":"Self-consistent scenario for jet and stellar explosion in collapsar: General relativistic magnetohydrodynamics simulation with dynamo","ref_index":10,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/P3LEWPPOK6ZAMXVGPNWDIGMO53","json":"https://pith.science/pith/P3LEWPPOK6ZAMXVGPNWDIGMO53.json","graph_json":"https://pith.science/api/pith-number/P3LEWPPOK6ZAMXVGPNWDIGMO53/graph.json","events_json":"https://pith.science/api/pith-number/P3LEWPPOK6ZAMXVGPNWDIGMO53/events.json","paper":"https://pith.science/paper/P3LEWPPO"},"agent_actions":{"view_html":"https://pith.science/pith/P3LEWPPOK6ZAMXVGPNWDIGMO53","download_json":"https://pith.science/pith/P3LEWPPOK6ZAMXVGPNWDIGMO53.json","view_paper":"https://pith.science/paper/P3LEWPPO","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/0502470&json=true","fetch_graph":"https://pith.science/api/pith-number/P3LEWPPOK6ZAMXVGPNWDIGMO53/graph.json","fetch_events":"https://pith.science/api/pith-number/P3LEWPPOK6ZAMXVGPNWDIGMO53/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/P3LEWPPOK6ZAMXVGPNWDIGMO53/action/timestamp_anchor","attest_storage":"https://pith.science/pith/P3LEWPPOK6ZAMXVGPNWDIGMO53/action/storage_attestation","attest_author":"https://pith.science/pith/P3LEWPPOK6ZAMXVGPNWDIGMO53/action/author_attestation","sign_citation":"https://pith.science/pith/P3LEWPPOK6ZAMXVGPNWDIGMO53/action/citation_signature","submit_replication":"https://pith.science/pith/P3LEWPPOK6ZAMXVGPNWDIGMO53/action/replication_record"}},"created_at":"2026-07-04T16:50:52.592848+00:00","updated_at":"2026-07-04T16:50:52.592848+00:00"}