{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2023:RKP7IGBHO7PDEAXNNEYDMMDDMW","short_pith_number":"pith:RKP7IGBH","schema_version":"1.0","canonical_sha256":"8a9ff4182777de3202ed69303630636596e5bdbfff585de149ae8039067efdbd","source":{"kind":"arxiv","id":"2301.08635","version":1},"attestation_state":"computed","paper":{"title":"Supercritical colliding wind binaries","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"G.E. Romero, L. Abaroa, P. Sotomayor","submitted_at":"2023-01-20T15:35:22Z","abstract_excerpt":"Context. Particle-accelerating colliding-wind binaries (PACWBs) are systems that are formed by two massive and hot stars and produce nonthermal (NT) radiation. The key elements of these systems are fast winds and the shocks that they create when they collide. Binaries with nonaccreting young pulsars have also been detected as NT emitters, again as a consequence of the wind-wind interaction. Black holes (BHs) might produce NT radiation by this mechanism if they accrete at super-Eddington rates. In such cases, the disk is expected to launch a radiation-driven wind, and if this wind has an equato"},"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":"2301.08635","kind":"arxiv","version":1},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.HE","submitted_at":"2023-01-20T15:35:22Z","cross_cats_sorted":[],"title_canon_sha256":"6baede7eb9e496ca232ddabfd5b3d5905c1ae7b92b3039b0f3f155b4848f72e6","abstract_canon_sha256":"3325d005fdebfe604b7c4eda559c7c193e2fd3e4778149ebd6cc3f1fb14717c7"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T05:46:36.338731Z","signature_b64":"WtlC3Xu+UVYckiqzwUXhElVOtP3jVoILGmnHebIVWyTWHpO6N/mOyfgHHQmjzVOytNuO+IyZrN9COMme8+8IAA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"8a9ff4182777de3202ed69303630636596e5bdbfff585de149ae8039067efdbd","last_reissued_at":"2026-07-05T05:46:36.338360Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T05:46:36.338360Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Supercritical colliding wind binaries","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"G.E. Romero, L. Abaroa, P. Sotomayor","submitted_at":"2023-01-20T15:35:22Z","abstract_excerpt":"Context. Particle-accelerating colliding-wind binaries (PACWBs) are systems that are formed by two massive and hot stars and produce nonthermal (NT) radiation. The key elements of these systems are fast winds and the shocks that they create when they collide. Binaries with nonaccreting young pulsars have also been detected as NT emitters, again as a consequence of the wind-wind interaction. Black holes (BHs) might produce NT radiation by this mechanism if they accrete at super-Eddington rates. In such cases, the disk is expected to launch a radiation-driven wind, and if this wind has an equato"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2301.08635","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/2301.08635/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":"2301.08635","created_at":"2026-07-05T05:46:36.338427+00:00"},{"alias_kind":"arxiv_version","alias_value":"2301.08635v1","created_at":"2026-07-05T05:46:36.338427+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2301.08635","created_at":"2026-07-05T05:46:36.338427+00:00"},{"alias_kind":"pith_short_12","alias_value":"RKP7IGBHO7PD","created_at":"2026-07-05T05:46:36.338427+00:00"},{"alias_kind":"pith_short_16","alias_value":"RKP7IGBHO7PDEAXN","created_at":"2026-07-05T05:46:36.338427+00:00"},{"alias_kind":"pith_short_8","alias_value":"RKP7IGBH","created_at":"2026-07-05T05:46:36.338427+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2509.03735","citing_title":"Effects of Bethe-Heitler pair production in ultraluminous X-ray sources","ref_index":2023,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/RKP7IGBHO7PDEAXNNEYDMMDDMW","json":"https://pith.science/pith/RKP7IGBHO7PDEAXNNEYDMMDDMW.json","graph_json":"https://pith.science/api/pith-number/RKP7IGBHO7PDEAXNNEYDMMDDMW/graph.json","events_json":"https://pith.science/api/pith-number/RKP7IGBHO7PDEAXNNEYDMMDDMW/events.json","paper":"https://pith.science/paper/RKP7IGBH"},"agent_actions":{"view_html":"https://pith.science/pith/RKP7IGBHO7PDEAXNNEYDMMDDMW","download_json":"https://pith.science/pith/RKP7IGBHO7PDEAXNNEYDMMDDMW.json","view_paper":"https://pith.science/paper/RKP7IGBH","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2301.08635&json=true","fetch_graph":"https://pith.science/api/pith-number/RKP7IGBHO7PDEAXNNEYDMMDDMW/graph.json","fetch_events":"https://pith.science/api/pith-number/RKP7IGBHO7PDEAXNNEYDMMDDMW/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/RKP7IGBHO7PDEAXNNEYDMMDDMW/action/timestamp_anchor","attest_storage":"https://pith.science/pith/RKP7IGBHO7PDEAXNNEYDMMDDMW/action/storage_attestation","attest_author":"https://pith.science/pith/RKP7IGBHO7PDEAXNNEYDMMDDMW/action/author_attestation","sign_citation":"https://pith.science/pith/RKP7IGBHO7PDEAXNNEYDMMDDMW/action/citation_signature","submit_replication":"https://pith.science/pith/RKP7IGBHO7PDEAXNNEYDMMDDMW/action/replication_record"}},"created_at":"2026-07-05T05:46:36.338427+00:00","updated_at":"2026-07-05T05:46:36.338427+00:00"}