{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2014:56HNNR6NMQUYWKSSTTO43FQGMD","short_pith_number":"pith:56HNNR6N","schema_version":"1.0","canonical_sha256":"ef8ed6c7cd64298b2a529cddcd960660dfe0fb8c7599a6d4f980b336420a66e9","source":{"kind":"arxiv","id":"1401.3711","version":1},"attestation_state":"computed","paper":{"title":"A Be-type star with a black hole companion","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA"],"primary_cat":"astro-ph.SR","authors_text":"A. Herrero, I. Negueruela, I. Ribas, J. Casares, J. M. Paredes, M. Ribo, S. Simon-Diaz","submitted_at":"2014-01-15T19:22:20Z","abstract_excerpt":"Stellar-mass black holes have all been discovered through X-ray emission, which arises from the accretion of gas from their binary companions (this gas is either stripped from low-mass stars or supplied as winds from massive ones). Binary evolution models also predict the existence of black holes accreting from the equatorial envelope of rapidly spinning Be-type stars (stars of the Be type are hot blue irregular variables showing characteristic spectral emission lines of hydrogen). Of the ~80 Be X-ray binaries known in the Galaxy, however, only pulsating neutron stars have been found as compan"},"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":"1401.3711","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2014-01-15T19:22:20Z","cross_cats_sorted":["astro-ph.GA"],"title_canon_sha256":"2909c3053a4ced5770dcbbb6c1ce7c5867717639e9794dff58f174544c7d94be","abstract_canon_sha256":"884196bc549d83e4f4cc7060228ab1089006662553bab36f20a5df518c7ae4ee"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T03:02:07.882956Z","signature_b64":"gftRK0stXwcxJ62vqXLAarcPC0jsR0zMGRjG4OFH3kZ2tQrEdYcflLJyS4aZ4dsdj2LbWHEWq9hzpBxxMFSsAw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"ef8ed6c7cd64298b2a529cddcd960660dfe0fb8c7599a6d4f980b336420a66e9","last_reissued_at":"2026-05-18T03:02:07.882204Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T03:02:07.882204Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"A Be-type star with a black hole companion","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA"],"primary_cat":"astro-ph.SR","authors_text":"A. Herrero, I. Negueruela, I. Ribas, J. Casares, J. M. Paredes, M. Ribo, S. Simon-Diaz","submitted_at":"2014-01-15T19:22:20Z","abstract_excerpt":"Stellar-mass black holes have all been discovered through X-ray emission, which arises from the accretion of gas from their binary companions (this gas is either stripped from low-mass stars or supplied as winds from massive ones). Binary evolution models also predict the existence of black holes accreting from the equatorial envelope of rapidly spinning Be-type stars (stars of the Be type are hot blue irregular variables showing characteristic spectral emission lines of hydrogen). Of the ~80 Be X-ray binaries known in the Galaxy, however, only pulsating neutron stars have been found as compan"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1401.3711","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":""},"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":"1401.3711","created_at":"2026-05-18T03:02:07.882333+00:00"},{"alias_kind":"arxiv_version","alias_value":"1401.3711v1","created_at":"2026-05-18T03:02:07.882333+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1401.3711","created_at":"2026-05-18T03:02:07.882333+00:00"},{"alias_kind":"pith_short_12","alias_value":"56HNNR6NMQUY","created_at":"2026-05-18T12:28:14.216126+00:00"},{"alias_kind":"pith_short_16","alias_value":"56HNNR6NMQUYWKSS","created_at":"2026-05-18T12:28:14.216126+00:00"},{"alias_kind":"pith_short_8","alias_value":"56HNNR6N","created_at":"2026-05-18T12:28:14.216126+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2605.11703","citing_title":"GW240925 and GW250207: Astrophysical Calibration of Gravitational-wave Detectors","ref_index":87,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/56HNNR6NMQUYWKSSTTO43FQGMD","json":"https://pith.science/pith/56HNNR6NMQUYWKSSTTO43FQGMD.json","graph_json":"https://pith.science/api/pith-number/56HNNR6NMQUYWKSSTTO43FQGMD/graph.json","events_json":"https://pith.science/api/pith-number/56HNNR6NMQUYWKSSTTO43FQGMD/events.json","paper":"https://pith.science/paper/56HNNR6N"},"agent_actions":{"view_html":"https://pith.science/pith/56HNNR6NMQUYWKSSTTO43FQGMD","download_json":"https://pith.science/pith/56HNNR6NMQUYWKSSTTO43FQGMD.json","view_paper":"https://pith.science/paper/56HNNR6N","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1401.3711&json=true","fetch_graph":"https://pith.science/api/pith-number/56HNNR6NMQUYWKSSTTO43FQGMD/graph.json","fetch_events":"https://pith.science/api/pith-number/56HNNR6NMQUYWKSSTTO43FQGMD/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/56HNNR6NMQUYWKSSTTO43FQGMD/action/timestamp_anchor","attest_storage":"https://pith.science/pith/56HNNR6NMQUYWKSSTTO43FQGMD/action/storage_attestation","attest_author":"https://pith.science/pith/56HNNR6NMQUYWKSSTTO43FQGMD/action/author_attestation","sign_citation":"https://pith.science/pith/56HNNR6NMQUYWKSSTTO43FQGMD/action/citation_signature","submit_replication":"https://pith.science/pith/56HNNR6NMQUYWKSSTTO43FQGMD/action/replication_record"}},"created_at":"2026-05-18T03:02:07.882333+00:00","updated_at":"2026-05-18T03:02:07.882333+00:00"}