{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2000:L23KGMI56ZC3M6U65DQQRKNHLA","short_pith_number":"pith:L23KGMI5","schema_version":"1.0","canonical_sha256":"5eb6a3311df645b67a9ee8e108a9a7581bdf5d2446c66fa5ec12a5ef0b1f7b86","source":{"kind":"arxiv","id":"astro-ph/0003462","version":2},"attestation_state":"computed","paper":{"title":"A Central Engine for Cosmic Gamma-Ray Burst Sources","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"L. Tao (Columbia Astronomy), M.A. Ruderman (Columbia Physics), Warsaw), W. Kluzniak (Copernicus Astronomical Center","submitted_at":"2000-03-30T22:45:04Z","abstract_excerpt":"One of a family previously proposed ``central engines'' for cosmic gamma-ray burst sources (Klu\\'zniak & Ruderman 1998) is considered in some detail. A steadily accreting $10^6$ Gauss magnetic white dwarf should ultimately collapse to a strongly differentially rotating, millisecond-rotation-period neutron star for a wide range of steady accretion rates and initial masses if the accreting white dwarf has an evolved O-Ne-Mg composition. A similar neutron star could also result from an initial C-O white dwarf but only for more constrained accretion rates. Because the collapsing white dwarf begins"},"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/0003462","kind":"arxiv","version":2},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2000-03-30T22:45:04Z","cross_cats_sorted":[],"title_canon_sha256":"bacb520d9b68003ed052d6f77fafb9c2a9ed3e8216b25f5468a0f6f70f08f234","abstract_canon_sha256":"ecc2b90ed33061c2ed9fa0a93439a6fb0ebce2ebbe532b7212ed9fe356577211"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T16:16:14.642836Z","signature_b64":"JnTMpKE/VQuKLtAwW8TWcaGzX5DRpIyFahty3zrwEJo2h/i+X6KLQAEyOKK7Dn6ItqvY+w+B1dCoCcDbW5BbDQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"5eb6a3311df645b67a9ee8e108a9a7581bdf5d2446c66fa5ec12a5ef0b1f7b86","last_reissued_at":"2026-07-04T16:16:14.642433Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T16:16:14.642433Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"A Central Engine for Cosmic Gamma-Ray Burst Sources","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"L. Tao (Columbia Astronomy), M.A. Ruderman (Columbia Physics), Warsaw), W. Kluzniak (Copernicus Astronomical Center","submitted_at":"2000-03-30T22:45:04Z","abstract_excerpt":"One of a family previously proposed ``central engines'' for cosmic gamma-ray burst sources (Klu\\'zniak & Ruderman 1998) is considered in some detail. A steadily accreting $10^6$ Gauss magnetic white dwarf should ultimately collapse to a strongly differentially rotating, millisecond-rotation-period neutron star for a wide range of steady accretion rates and initial masses if the accreting white dwarf has an evolved O-Ne-Mg composition. A similar neutron star could also result from an initial C-O white dwarf but only for more constrained accretion rates. Because the collapsing white dwarf begins"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0003462","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/0003462/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/0003462","created_at":"2026-07-04T16:16:14.642492+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/0003462v2","created_at":"2026-07-04T16:16:14.642492+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/0003462","created_at":"2026-07-04T16:16:14.642492+00:00"},{"alias_kind":"pith_short_12","alias_value":"L23KGMI56ZC3","created_at":"2026-07-04T16:16:14.642492+00:00"},{"alias_kind":"pith_short_16","alias_value":"L23KGMI56ZC3M6U6","created_at":"2026-07-04T16:16:14.642492+00:00"},{"alias_kind":"pith_short_8","alias_value":"L23KGMI5","created_at":"2026-07-04T16:16:14.642492+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2501.00239","citing_title":"On the Duration of Gamma-Ray Bursts","ref_index":63,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/L23KGMI56ZC3M6U65DQQRKNHLA","json":"https://pith.science/pith/L23KGMI56ZC3M6U65DQQRKNHLA.json","graph_json":"https://pith.science/api/pith-number/L23KGMI56ZC3M6U65DQQRKNHLA/graph.json","events_json":"https://pith.science/api/pith-number/L23KGMI56ZC3M6U65DQQRKNHLA/events.json","paper":"https://pith.science/paper/L23KGMI5"},"agent_actions":{"view_html":"https://pith.science/pith/L23KGMI56ZC3M6U65DQQRKNHLA","download_json":"https://pith.science/pith/L23KGMI56ZC3M6U65DQQRKNHLA.json","view_paper":"https://pith.science/paper/L23KGMI5","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/0003462&json=true","fetch_graph":"https://pith.science/api/pith-number/L23KGMI56ZC3M6U65DQQRKNHLA/graph.json","fetch_events":"https://pith.science/api/pith-number/L23KGMI56ZC3M6U65DQQRKNHLA/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/L23KGMI56ZC3M6U65DQQRKNHLA/action/timestamp_anchor","attest_storage":"https://pith.science/pith/L23KGMI56ZC3M6U65DQQRKNHLA/action/storage_attestation","attest_author":"https://pith.science/pith/L23KGMI56ZC3M6U65DQQRKNHLA/action/author_attestation","sign_citation":"https://pith.science/pith/L23KGMI56ZC3M6U65DQQRKNHLA/action/citation_signature","submit_replication":"https://pith.science/pith/L23KGMI56ZC3M6U65DQQRKNHLA/action/replication_record"}},"created_at":"2026-07-04T16:16:14.642492+00:00","updated_at":"2026-07-04T16:16:14.642492+00:00"}