{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2023:FLQL44SS7U47KWA7RMEZ5UNPHV","short_pith_number":"pith:FLQL44SS","schema_version":"1.0","canonical_sha256":"2ae0be7252fd39f5581f8b099ed1af3d654156ab212ec81f676071b5f64afa62","source":{"kind":"arxiv","id":"2303.16902","version":2},"attestation_state":"computed","paper":{"title":"GRB-SN Association within the Binary-Driven Hypernova Model","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"C. Cherubini, C.L. Bianco, F. Rastegarnia, J. A. Rueda, Liang Li, L. M. Becerra, M. Della Valle, N. Sahakyan, R. Moradi, R. Ruffini, S. Filippi, S. R. Zhang, Y. Aimuratov, Y. Wang","submitted_at":"2023-03-14T10:20:39Z","abstract_excerpt":"The observations of supernovae (SNe) Ic occurring after the prompt emission of long gamma-ray bursts (GRBs) are addressed within the binary-driven hypernova (BdHN) model where GRBs originate from a binary composed of a $\\sim10M_\\odot$ carbon-oxygen (CO) star and a neutron star (NS). The CO core collapse gives the trigger, leading to a hypernova with a fast-spinning newborn NS ($\\nu$NS) at its center. The evolution depends strongly on the binary period, $P_{\\rm bin}$. For $P_{\\rm bin}\\sim5$min, BdHNe I occur with energies $10^{52}$--$10^{54}$erg. The accretion of SN ejecta onto the NS leads to "},"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":"2303.16902","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2023-03-14T10:20:39Z","cross_cats_sorted":[],"title_canon_sha256":"b39382f1be6ad3b0370dd4b09a364e37c5a2eb1e6a01a7c272390254597b5bf3","abstract_canon_sha256":"5c82608b83552c04015c87054d0d07b7ea05b6dc2dd0d42fc40afd6f2480fa87"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T06:53:06.588432Z","signature_b64":"8yLZHohcrUYF5TPmk3MViAQlR95phnpC1M7vA3HGfwQMmMFTFoHnZAr6v3bJIuFyO8jeITzV9J9NrTkUlFD1Bg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"2ae0be7252fd39f5581f8b099ed1af3d654156ab212ec81f676071b5f64afa62","last_reissued_at":"2026-07-05T06:53:06.587940Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T06:53:06.587940Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"GRB-SN Association within the Binary-Driven Hypernova Model","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"C. Cherubini, C.L. Bianco, F. Rastegarnia, J. A. Rueda, Liang Li, L. M. Becerra, M. Della Valle, N. Sahakyan, R. Moradi, R. Ruffini, S. Filippi, S. R. Zhang, Y. Aimuratov, Y. Wang","submitted_at":"2023-03-14T10:20:39Z","abstract_excerpt":"The observations of supernovae (SNe) Ic occurring after the prompt emission of long gamma-ray bursts (GRBs) are addressed within the binary-driven hypernova (BdHN) model where GRBs originate from a binary composed of a $\\sim10M_\\odot$ carbon-oxygen (CO) star and a neutron star (NS). The CO core collapse gives the trigger, leading to a hypernova with a fast-spinning newborn NS ($\\nu$NS) at its center. The evolution depends strongly on the binary period, $P_{\\rm bin}$. For $P_{\\rm bin}\\sim5$min, BdHNe I occur with energies $10^{52}$--$10^{54}$erg. The accretion of SN ejecta onto the NS leads to "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2303.16902","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/2303.16902/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":"2303.16902","created_at":"2026-07-05T06:53:06.587998+00:00"},{"alias_kind":"arxiv_version","alias_value":"2303.16902v2","created_at":"2026-07-05T06:53:06.587998+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2303.16902","created_at":"2026-07-05T06:53:06.587998+00:00"},{"alias_kind":"pith_short_12","alias_value":"FLQL44SS7U47","created_at":"2026-07-05T06:53:06.587998+00:00"},{"alias_kind":"pith_short_16","alias_value":"FLQL44SS7U47KWA7","created_at":"2026-07-05T06:53:06.587998+00:00"},{"alias_kind":"pith_short_8","alias_value":"FLQL44SS","created_at":"2026-07-05T06:53:06.587998+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2509.08172","citing_title":"Short GRB 090510: a magnetized neutron star binary merger leading to a black hole","ref_index":3,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/FLQL44SS7U47KWA7RMEZ5UNPHV","json":"https://pith.science/pith/FLQL44SS7U47KWA7RMEZ5UNPHV.json","graph_json":"https://pith.science/api/pith-number/FLQL44SS7U47KWA7RMEZ5UNPHV/graph.json","events_json":"https://pith.science/api/pith-number/FLQL44SS7U47KWA7RMEZ5UNPHV/events.json","paper":"https://pith.science/paper/FLQL44SS"},"agent_actions":{"view_html":"https://pith.science/pith/FLQL44SS7U47KWA7RMEZ5UNPHV","download_json":"https://pith.science/pith/FLQL44SS7U47KWA7RMEZ5UNPHV.json","view_paper":"https://pith.science/paper/FLQL44SS","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2303.16902&json=true","fetch_graph":"https://pith.science/api/pith-number/FLQL44SS7U47KWA7RMEZ5UNPHV/graph.json","fetch_events":"https://pith.science/api/pith-number/FLQL44SS7U47KWA7RMEZ5UNPHV/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/FLQL44SS7U47KWA7RMEZ5UNPHV/action/timestamp_anchor","attest_storage":"https://pith.science/pith/FLQL44SS7U47KWA7RMEZ5UNPHV/action/storage_attestation","attest_author":"https://pith.science/pith/FLQL44SS7U47KWA7RMEZ5UNPHV/action/author_attestation","sign_citation":"https://pith.science/pith/FLQL44SS7U47KWA7RMEZ5UNPHV/action/citation_signature","submit_replication":"https://pith.science/pith/FLQL44SS7U47KWA7RMEZ5UNPHV/action/replication_record"}},"created_at":"2026-07-05T06:53:06.587998+00:00","updated_at":"2026-07-05T06:53:06.587998+00:00"}