{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2023:3FQM2F3OM3ZSJG66QWXB25JGW5","short_pith_number":"pith:3FQM2F3O","schema_version":"1.0","canonical_sha256":"d960cd176e66f3249bde85ae1d7526b77f583d940b368df032d37a3df2aac82d","source":{"kind":"arxiv","id":"2305.06375","version":2},"attestation_state":"computed","paper":{"title":"A Leptonic Model for Neutrino Emission From Active Galactic Nuclei","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.CO","hep-ph"],"primary_cat":"astro-ph.HE","authors_text":"Dan Hooper, Kathryn Plant","submitted_at":"2023-05-10T18:00:02Z","abstract_excerpt":"It is often stated that the observation of high-energy neutrinos from an astrophysical source would constitute a smoking gun for the acceleration of hadronic cosmic rays. Here, we point out that there exists a purely leptonic mechanism to produce TeV-scale neutrinos in astrophysical environments. In particular, very high-energy synchrotron photons can scatter with X-rays, exceeding the threshold for muon-antimuon pair production. When these muons decay, they produce neutrinos without any cosmic-ray protons or nuclei being involved. In order for this mechanism to be efficient, the source in que"},"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":"2305.06375","kind":"arxiv","version":2},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.HE","submitted_at":"2023-05-10T18:00:02Z","cross_cats_sorted":["astro-ph.CO","hep-ph"],"title_canon_sha256":"d7ab04cf5b7eee3ddfc984cf9e869cc6f55c28e52844fcb00849a51923ab6ca1","abstract_canon_sha256":"9f94af05032ba853469739f40591ac016885e011c9ea914f5dbf2b90aaa62873"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T06:11:33.157234Z","signature_b64":"TvTt2WIEcac83vNpMcFzhFuHofLy3xRTkkZy9ujB+ouc+dj8ovSSaOWFegUtKgKgE5DJh95SIXdZHccwpRd7DA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"d960cd176e66f3249bde85ae1d7526b77f583d940b368df032d37a3df2aac82d","last_reissued_at":"2026-07-05T06:11:33.156779Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T06:11:33.156779Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"A Leptonic Model for Neutrino Emission From Active Galactic Nuclei","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.CO","hep-ph"],"primary_cat":"astro-ph.HE","authors_text":"Dan Hooper, Kathryn Plant","submitted_at":"2023-05-10T18:00:02Z","abstract_excerpt":"It is often stated that the observation of high-energy neutrinos from an astrophysical source would constitute a smoking gun for the acceleration of hadronic cosmic rays. Here, we point out that there exists a purely leptonic mechanism to produce TeV-scale neutrinos in astrophysical environments. In particular, very high-energy synchrotron photons can scatter with X-rays, exceeding the threshold for muon-antimuon pair production. When these muons decay, they produce neutrinos without any cosmic-ray protons or nuclei being involved. In order for this mechanism to be efficient, the source in que"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2305.06375","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/2305.06375/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":"2305.06375","created_at":"2026-07-05T06:11:33.156838+00:00"},{"alias_kind":"arxiv_version","alias_value":"2305.06375v2","created_at":"2026-07-05T06:11:33.156838+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2305.06375","created_at":"2026-07-05T06:11:33.156838+00:00"},{"alias_kind":"pith_short_12","alias_value":"3FQM2F3OM3ZS","created_at":"2026-07-05T06:11:33.156838+00:00"},{"alias_kind":"pith_short_16","alias_value":"3FQM2F3OM3ZSJG66","created_at":"2026-07-05T06:11:33.156838+00:00"},{"alias_kind":"pith_short_8","alias_value":"3FQM2F3O","created_at":"2026-07-05T06:11:33.156838+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2508.11891","citing_title":"High-Energy Neutrinos from Cosmic-Ray Scatterings with Supernova Neutrinos","ref_index":4,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/3FQM2F3OM3ZSJG66QWXB25JGW5","json":"https://pith.science/pith/3FQM2F3OM3ZSJG66QWXB25JGW5.json","graph_json":"https://pith.science/api/pith-number/3FQM2F3OM3ZSJG66QWXB25JGW5/graph.json","events_json":"https://pith.science/api/pith-number/3FQM2F3OM3ZSJG66QWXB25JGW5/events.json","paper":"https://pith.science/paper/3FQM2F3O"},"agent_actions":{"view_html":"https://pith.science/pith/3FQM2F3OM3ZSJG66QWXB25JGW5","download_json":"https://pith.science/pith/3FQM2F3OM3ZSJG66QWXB25JGW5.json","view_paper":"https://pith.science/paper/3FQM2F3O","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2305.06375&json=true","fetch_graph":"https://pith.science/api/pith-number/3FQM2F3OM3ZSJG66QWXB25JGW5/graph.json","fetch_events":"https://pith.science/api/pith-number/3FQM2F3OM3ZSJG66QWXB25JGW5/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/3FQM2F3OM3ZSJG66QWXB25JGW5/action/timestamp_anchor","attest_storage":"https://pith.science/pith/3FQM2F3OM3ZSJG66QWXB25JGW5/action/storage_attestation","attest_author":"https://pith.science/pith/3FQM2F3OM3ZSJG66QWXB25JGW5/action/author_attestation","sign_citation":"https://pith.science/pith/3FQM2F3OM3ZSJG66QWXB25JGW5/action/citation_signature","submit_replication":"https://pith.science/pith/3FQM2F3OM3ZSJG66QWXB25JGW5/action/replication_record"}},"created_at":"2026-07-05T06:11:33.156838+00:00","updated_at":"2026-07-05T06:11:33.156838+00:00"}