{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2023:Y6SIDFFHL2YSRMFMDBSRVBNTEO","short_pith_number":"pith:Y6SIDFFH","schema_version":"1.0","canonical_sha256":"c7a48194a75eb128b0ac18651a85b323814fb5b32b9dcf93c1d2e4867a6edecc","source":{"kind":"arxiv","id":"2309.02161","version":1},"attestation_state":"computed","paper":{"title":"Supernova-like explosion of massive rotating stars from disks surrounding a black hole","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["gr-qc"],"primary_cat":"astro-ph.HE","authors_text":"Alan Tsz-Lok Lam, Masaru Shibata, Sho Fujibayashi, Yuichiro Sekiguchi","submitted_at":"2023-09-05T11:58:26Z","abstract_excerpt":"We perform a new general-relativistic viscous-radiation hydrodynamics simulation for supernova-like explosion associated with stellar core collapse of rotating massive stars to a system of a black hole and a massive torus paying particular attention to large-mass progenitor stars with the zero-age main-sequence mass of $M_\\mathrm{ZAMS}=$20, 35, and 45$M_\\odot$ of Ref.~\\cite{Aguilera-Dena2020oct}. Assuming that a black hole is formed in a short timescale after the onset of the stellar collapse, the new simulations are started from initial data of a spinning black hole and infalling matter 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":"2309.02161","kind":"arxiv","version":1},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.HE","submitted_at":"2023-09-05T11:58:26Z","cross_cats_sorted":["gr-qc"],"title_canon_sha256":"835c196187211031f256cd7d8011b88bb8641fcd599cd0bb1c4f2edd44fc5a5b","abstract_canon_sha256":"16a0123f5886f5ca3c82b3c79d1f0b58f3afd346cb6381495e3453fa09be58c1"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T06:47:49.407039Z","signature_b64":"wXjqlXsJ2a9FGJw6jHQ/ICPxqKYBhggzbJ7486II9X5ToYeOcNdhlB9G4X7fanbiPzPcESL5bHo7CbDlSh8gCg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"c7a48194a75eb128b0ac18651a85b323814fb5b32b9dcf93c1d2e4867a6edecc","last_reissued_at":"2026-07-05T06:47:49.406514Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T06:47:49.406514Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Supernova-like explosion of massive rotating stars from disks surrounding a black hole","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["gr-qc"],"primary_cat":"astro-ph.HE","authors_text":"Alan Tsz-Lok Lam, Masaru Shibata, Sho Fujibayashi, Yuichiro Sekiguchi","submitted_at":"2023-09-05T11:58:26Z","abstract_excerpt":"We perform a new general-relativistic viscous-radiation hydrodynamics simulation for supernova-like explosion associated with stellar core collapse of rotating massive stars to a system of a black hole and a massive torus paying particular attention to large-mass progenitor stars with the zero-age main-sequence mass of $M_\\mathrm{ZAMS}=$20, 35, and 45$M_\\odot$ of Ref.~\\cite{Aguilera-Dena2020oct}. Assuming that a black hole is formed in a short timescale after the onset of the stellar collapse, the new simulations are started from initial data of a spinning black hole and infalling matter that "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2309.02161","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/2309.02161/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":"2309.02161","created_at":"2026-07-05T06:47:49.406586+00:00"},{"alias_kind":"arxiv_version","alias_value":"2309.02161v1","created_at":"2026-07-05T06:47:49.406586+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2309.02161","created_at":"2026-07-05T06:47:49.406586+00:00"},{"alias_kind":"pith_short_12","alias_value":"Y6SIDFFHL2YS","created_at":"2026-07-05T06:47:49.406586+00:00"},{"alias_kind":"pith_short_16","alias_value":"Y6SIDFFHL2YSRMFM","created_at":"2026-07-05T06:47:49.406586+00:00"},{"alias_kind":"pith_short_8","alias_value":"Y6SIDFFH","created_at":"2026-07-05T06:47:49.406586+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":0,"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":31,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/Y6SIDFFHL2YSRMFMDBSRVBNTEO","json":"https://pith.science/pith/Y6SIDFFHL2YSRMFMDBSRVBNTEO.json","graph_json":"https://pith.science/api/pith-number/Y6SIDFFHL2YSRMFMDBSRVBNTEO/graph.json","events_json":"https://pith.science/api/pith-number/Y6SIDFFHL2YSRMFMDBSRVBNTEO/events.json","paper":"https://pith.science/paper/Y6SIDFFH"},"agent_actions":{"view_html":"https://pith.science/pith/Y6SIDFFHL2YSRMFMDBSRVBNTEO","download_json":"https://pith.science/pith/Y6SIDFFHL2YSRMFMDBSRVBNTEO.json","view_paper":"https://pith.science/paper/Y6SIDFFH","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2309.02161&json=true","fetch_graph":"https://pith.science/api/pith-number/Y6SIDFFHL2YSRMFMDBSRVBNTEO/graph.json","fetch_events":"https://pith.science/api/pith-number/Y6SIDFFHL2YSRMFMDBSRVBNTEO/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/Y6SIDFFHL2YSRMFMDBSRVBNTEO/action/timestamp_anchor","attest_storage":"https://pith.science/pith/Y6SIDFFHL2YSRMFMDBSRVBNTEO/action/storage_attestation","attest_author":"https://pith.science/pith/Y6SIDFFHL2YSRMFMDBSRVBNTEO/action/author_attestation","sign_citation":"https://pith.science/pith/Y6SIDFFHL2YSRMFMDBSRVBNTEO/action/citation_signature","submit_replication":"https://pith.science/pith/Y6SIDFFHL2YSRMFMDBSRVBNTEO/action/replication_record"}},"created_at":"2026-07-05T06:47:49.406586+00:00","updated_at":"2026-07-05T06:47:49.406586+00:00"}