{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2025:5NWRPGA4EOPM4PT277DMNZ3AOC","short_pith_number":"pith:5NWRPGA4","schema_version":"1.0","canonical_sha256":"eb6d17981c239ece3e7affc6c6e76070a94f8c1f12b55e11383f240fe5d4f22b","source":{"kind":"arxiv","id":"2507.21048","version":1},"attestation_state":"computed","paper":{"title":"Galactic Super-Accreting X-ray Binaries as Super-PeVatron Accelerators","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.GA","astro-ph.SR"],"primary_cat":"astro-ph.HE","authors_text":"Brian Reville, Felix Aharonian, Jieshuang Wang","submitted_at":"2025-07-28T17:59:15Z","abstract_excerpt":"The extension of the cosmic-ray (CR) spectrum well beyond 1~PeV necessitates the existence of a population of accelerators in the Milky Way, which we refer to as Super PeVatrons. Identifying the nature of these sources remains a challenge to the paradigm of galactic CRs. Galactic super-accreting X-ray binaries, where the compact object accretes at a rate near or above the Eddington limit, can meet the energy requirement to supply the high-energy population of galactic CRs. We demonstrate that the trans-relativistic jets and/or winds of these powerful objects with kinetic energy luminosity exce"},"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":"2507.21048","kind":"arxiv","version":1},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.HE","submitted_at":"2025-07-28T17:59:15Z","cross_cats_sorted":["astro-ph.GA","astro-ph.SR"],"title_canon_sha256":"68af3405cbb78afa3dd12995941309519483b11e6a11f5ff0b426231165d2d0c","abstract_canon_sha256":"e6ce21fdd34fe97fd4bb9122f9b8968e0c2c8b31bbaff77c40bc3148e75724d3"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T11:44:30.248291Z","signature_b64":"XIqDr/xdUtyHvtlO3QV18N8cP2Ya/eL3/rJwCvMWtALcmWtWPkC/RuRFtNtqrinUfIoliBHUXnTeLBZqH478Dg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"eb6d17981c239ece3e7affc6c6e76070a94f8c1f12b55e11383f240fe5d4f22b","last_reissued_at":"2026-07-05T11:44:30.247881Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T11:44:30.247881Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Galactic Super-Accreting X-ray Binaries as Super-PeVatron Accelerators","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.GA","astro-ph.SR"],"primary_cat":"astro-ph.HE","authors_text":"Brian Reville, Felix Aharonian, Jieshuang Wang","submitted_at":"2025-07-28T17:59:15Z","abstract_excerpt":"The extension of the cosmic-ray (CR) spectrum well beyond 1~PeV necessitates the existence of a population of accelerators in the Milky Way, which we refer to as Super PeVatrons. Identifying the nature of these sources remains a challenge to the paradigm of galactic CRs. Galactic super-accreting X-ray binaries, where the compact object accretes at a rate near or above the Eddington limit, can meet the energy requirement to supply the high-energy population of galactic CRs. We demonstrate that the trans-relativistic jets and/or winds of these powerful objects with kinetic energy luminosity exce"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2507.21048","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/2507.21048/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":"2507.21048","created_at":"2026-07-05T11:44:30.247937+00:00"},{"alias_kind":"arxiv_version","alias_value":"2507.21048v1","created_at":"2026-07-05T11:44:30.247937+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2507.21048","created_at":"2026-07-05T11:44:30.247937+00:00"},{"alias_kind":"pith_short_12","alias_value":"5NWRPGA4EOPM","created_at":"2026-07-05T11:44:30.247937+00:00"},{"alias_kind":"pith_short_16","alias_value":"5NWRPGA4EOPM4PT2","created_at":"2026-07-05T11:44:30.247937+00:00"},{"alias_kind":"pith_short_8","alias_value":"5NWRPGA4","created_at":"2026-07-05T11:44:30.247937+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2512.16638","citing_title":"Cygnus X-3: A variable petaelectronvolt gamma-ray source","ref_index":48,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/5NWRPGA4EOPM4PT277DMNZ3AOC","json":"https://pith.science/pith/5NWRPGA4EOPM4PT277DMNZ3AOC.json","graph_json":"https://pith.science/api/pith-number/5NWRPGA4EOPM4PT277DMNZ3AOC/graph.json","events_json":"https://pith.science/api/pith-number/5NWRPGA4EOPM4PT277DMNZ3AOC/events.json","paper":"https://pith.science/paper/5NWRPGA4"},"agent_actions":{"view_html":"https://pith.science/pith/5NWRPGA4EOPM4PT277DMNZ3AOC","download_json":"https://pith.science/pith/5NWRPGA4EOPM4PT277DMNZ3AOC.json","view_paper":"https://pith.science/paper/5NWRPGA4","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2507.21048&json=true","fetch_graph":"https://pith.science/api/pith-number/5NWRPGA4EOPM4PT277DMNZ3AOC/graph.json","fetch_events":"https://pith.science/api/pith-number/5NWRPGA4EOPM4PT277DMNZ3AOC/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/5NWRPGA4EOPM4PT277DMNZ3AOC/action/timestamp_anchor","attest_storage":"https://pith.science/pith/5NWRPGA4EOPM4PT277DMNZ3AOC/action/storage_attestation","attest_author":"https://pith.science/pith/5NWRPGA4EOPM4PT277DMNZ3AOC/action/author_attestation","sign_citation":"https://pith.science/pith/5NWRPGA4EOPM4PT277DMNZ3AOC/action/citation_signature","submit_replication":"https://pith.science/pith/5NWRPGA4EOPM4PT277DMNZ3AOC/action/replication_record"}},"created_at":"2026-07-05T11:44:30.247937+00:00","updated_at":"2026-07-05T11:44:30.247937+00:00"}