{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2010:RHOJRUVLCHR4MCNJOAA2BUKP7M","short_pith_number":"pith:RHOJRUVL","schema_version":"1.0","canonical_sha256":"89dc98d2ab11e3c609a97001a0d14ffb1391d77428a909bd39cd699a6d9eb762","source":{"kind":"arxiv","id":"1009.5303","version":2},"attestation_state":"computed","paper":{"title":"Formation of black hole and accretion disk in a massive high-entropy stellar core collapse","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["gr-qc"],"primary_cat":"astro-ph.HE","authors_text":"Masaru Shibata, Yuichiro Sekiguchi","submitted_at":"2010-09-27T15:56:41Z","abstract_excerpt":"We present the first numerical result of fully general relativistic axisymmetric simulations for the collapse of a rotating high-entropy stellar core to a black hole and an accretion disk. The simulations are performed taking into account the relevant microphysics. We adopt as initial condition a spherical core with constant electron fraction ($Y_e = 0.5$) and entropy per baryon $s$ = 8 $k_B$, and angular velocity is superimposed. In the early phase, the core collapses in a homologous manner. Then, it experiences a weak bounce due to the gas pressure of free nucleons. Because the bounce is wea"},"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":"1009.5303","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2010-09-27T15:56:41Z","cross_cats_sorted":["gr-qc"],"title_canon_sha256":"29a4839bc2a722bfaa76dc5d921fab9e6143af83ade4cb6fe757b44fd136079d","abstract_canon_sha256":"5a77472cde543b06aaace48a428adab12e86b51a642dffe39f7dcef3df949942"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:05:16.786561Z","signature_b64":"d3p60NBvqhsykwch90SzZQbNo005eOC/BtB3xLP0zojgrSrR4Ywv7ZliguhWclMdh0NwIC4yoqCQEDLFgVYUCw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"89dc98d2ab11e3c609a97001a0d14ffb1391d77428a909bd39cd699a6d9eb762","last_reissued_at":"2026-05-18T02:05:16.785843Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:05:16.785843Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Formation of black hole and accretion disk in a massive high-entropy stellar core collapse","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["gr-qc"],"primary_cat":"astro-ph.HE","authors_text":"Masaru Shibata, Yuichiro Sekiguchi","submitted_at":"2010-09-27T15:56:41Z","abstract_excerpt":"We present the first numerical result of fully general relativistic axisymmetric simulations for the collapse of a rotating high-entropy stellar core to a black hole and an accretion disk. The simulations are performed taking into account the relevant microphysics. We adopt as initial condition a spherical core with constant electron fraction ($Y_e = 0.5$) and entropy per baryon $s$ = 8 $k_B$, and angular velocity is superimposed. In the early phase, the core collapses in a homologous manner. Then, it experiences a weak bounce due to the gas pressure of free nucleons. Because the bounce is wea"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1009.5303","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":"1009.5303","created_at":"2026-05-18T02:05:16.785955+00:00"},{"alias_kind":"arxiv_version","alias_value":"1009.5303v2","created_at":"2026-05-18T02:05:16.785955+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1009.5303","created_at":"2026-05-18T02:05:16.785955+00:00"},{"alias_kind":"pith_short_12","alias_value":"RHOJRUVLCHR4","created_at":"2026-05-18T12:26:13.927090+00:00"},{"alias_kind":"pith_short_16","alias_value":"RHOJRUVLCHR4MCNJ","created_at":"2026-05-18T12:26:13.927090+00:00"},{"alias_kind":"pith_short_8","alias_value":"RHOJRUVL","created_at":"2026-05-18T12:26:13.927090+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2606.12542","citing_title":"Implementation of multi-grid Poisson solver in numerical relativity and its application to gravitational collapse of massive star","ref_index":48,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/RHOJRUVLCHR4MCNJOAA2BUKP7M","json":"https://pith.science/pith/RHOJRUVLCHR4MCNJOAA2BUKP7M.json","graph_json":"https://pith.science/api/pith-number/RHOJRUVLCHR4MCNJOAA2BUKP7M/graph.json","events_json":"https://pith.science/api/pith-number/RHOJRUVLCHR4MCNJOAA2BUKP7M/events.json","paper":"https://pith.science/paper/RHOJRUVL"},"agent_actions":{"view_html":"https://pith.science/pith/RHOJRUVLCHR4MCNJOAA2BUKP7M","download_json":"https://pith.science/pith/RHOJRUVLCHR4MCNJOAA2BUKP7M.json","view_paper":"https://pith.science/paper/RHOJRUVL","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1009.5303&json=true","fetch_graph":"https://pith.science/api/pith-number/RHOJRUVLCHR4MCNJOAA2BUKP7M/graph.json","fetch_events":"https://pith.science/api/pith-number/RHOJRUVLCHR4MCNJOAA2BUKP7M/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/RHOJRUVLCHR4MCNJOAA2BUKP7M/action/timestamp_anchor","attest_storage":"https://pith.science/pith/RHOJRUVLCHR4MCNJOAA2BUKP7M/action/storage_attestation","attest_author":"https://pith.science/pith/RHOJRUVLCHR4MCNJOAA2BUKP7M/action/author_attestation","sign_citation":"https://pith.science/pith/RHOJRUVLCHR4MCNJOAA2BUKP7M/action/citation_signature","submit_replication":"https://pith.science/pith/RHOJRUVLCHR4MCNJOAA2BUKP7M/action/replication_record"}},"created_at":"2026-05-18T02:05:16.785955+00:00","updated_at":"2026-05-18T02:05:16.785955+00:00"}