{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:1993:27G6AXEHYWVEXQIBFIXGRBYRX5","short_pith_number":"pith:27G6AXEH","schema_version":"1.0","canonical_sha256":"d7cde05c87c5aa4bc1012a2e688711bf7001847869f2d1fc70d081217d670f6c","source":{"kind":"arxiv","id":"astro-ph/9302006","version":2},"attestation_state":"computed","paper":{"title":"The Proton Blazar","license":"","headline":"","cross_cats":["hep-ph"],"primary_cat":"astro-ph","authors_text":"Karl Mannheim","submitted_at":"1993-02-04T16:20:57Z","abstract_excerpt":"Considering shock-accelerated protons in addition to electrons in a synchrotron radio jet naturally produces the observed X- through gamma ray continuum emission of flat-spectrum radio-loud AGN, whereas the corresponding shock-accelerated electrons produce the infrared through optical continuum. All of these emission components are rapidly variable on short time scales which can be accounted for by a common origin of the blazar emission in a relativistic sub-parsec scale jet. Moreover, neutrino fluxes are estimated which may be observable with the HiRes experiment and the impact on the ISM of "},"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/9302006","kind":"arxiv","version":2},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"1993-02-04T16:20:57Z","cross_cats_sorted":["hep-ph"],"title_canon_sha256":"32ccea87085540fe024ac7461b22634210acc8c86996db3c7bc87b910493cf1a","abstract_canon_sha256":"9312d90bc0d0b27c8b46d6769e1f70f14a8c7c3059aba0e747859844a6f4ba0e"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T15:07:15.439696Z","signature_b64":"1ge7wFq3YpD0Ig9uFQGcgpN8nZE3Ps8N56G1YfgymWVpm026CtMn+7z9EHCYG+qpT2G6PSNXcXdwY9umgITrAw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"d7cde05c87c5aa4bc1012a2e688711bf7001847869f2d1fc70d081217d670f6c","last_reissued_at":"2026-07-04T15:07:15.439286Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T15:07:15.439286Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The Proton Blazar","license":"","headline":"","cross_cats":["hep-ph"],"primary_cat":"astro-ph","authors_text":"Karl Mannheim","submitted_at":"1993-02-04T16:20:57Z","abstract_excerpt":"Considering shock-accelerated protons in addition to electrons in a synchrotron radio jet naturally produces the observed X- through gamma ray continuum emission of flat-spectrum radio-loud AGN, whereas the corresponding shock-accelerated electrons produce the infrared through optical continuum. All of these emission components are rapidly variable on short time scales which can be accounted for by a common origin of the blazar emission in a relativistic sub-parsec scale jet. Moreover, neutrino fluxes are estimated which may be observable with the HiRes experiment and the impact on the ISM of "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/9302006","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/9302006/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/9302006","created_at":"2026-07-04T15:07:15.439359+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/9302006v2","created_at":"2026-07-04T15:07:15.439359+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/9302006","created_at":"2026-07-04T15:07:15.439359+00:00"},{"alias_kind":"pith_short_12","alias_value":"27G6AXEHYWVE","created_at":"2026-07-04T15:07:15.439359+00:00"},{"alias_kind":"pith_short_16","alias_value":"27G6AXEHYWVEXQIB","created_at":"2026-07-04T15:07:15.439359+00:00"},{"alias_kind":"pith_short_8","alias_value":"27G6AXEH","created_at":"2026-07-04T15:07:15.439359+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":8,"internal_anchor_count":3,"sample":[{"citing_arxiv_id":"2606.00816","citing_title":"High-Synchrotron-Peaked BL Lacs as Multi-Messenger Sources: Connecting Ultra-High-Energy Cosmic Rays and Neutrinos","ref_index":51,"is_internal_anchor":true},{"citing_arxiv_id":"2605.01139","citing_title":"Detectability of Polarized Gamma-ray Emission from Blazar Flares with COSI","ref_index":25,"is_internal_anchor":true},{"citing_arxiv_id":"2512.00660","citing_title":"Particle Astrophysics with High and Ultrahigh Energy Neutrinos","ref_index":53,"is_internal_anchor":true},{"citing_arxiv_id":"2605.08775","citing_title":"Chasing the neutrino blazar candidates II: SED modeling with hadronic model","ref_index":35,"is_internal_anchor":false},{"citing_arxiv_id":"2605.07680","citing_title":"Advance warning of $\\gamma$-ray blazar flares from \\textit{Fermi}-LAT light curves: a strictly causal machine-learning backtest","ref_index":31,"is_internal_anchor":false},{"citing_arxiv_id":"2605.01601","citing_title":"Zooming in on the GeV $\\gamma$-ray flare of the blazar PKS 1725+123 with a multimessenger lens","ref_index":47,"is_internal_anchor":false},{"citing_arxiv_id":"2605.01139","citing_title":"Detectability of Polarized Gamma-ray Emission from Blazar Flares with COSI","ref_index":25,"is_internal_anchor":false},{"citing_arxiv_id":"2605.04619","citing_title":"Spectro-Polarimetric Observations of TeV Sources (SPOTS): First results","ref_index":18,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/27G6AXEHYWVEXQIBFIXGRBYRX5","json":"https://pith.science/pith/27G6AXEHYWVEXQIBFIXGRBYRX5.json","graph_json":"https://pith.science/api/pith-number/27G6AXEHYWVEXQIBFIXGRBYRX5/graph.json","events_json":"https://pith.science/api/pith-number/27G6AXEHYWVEXQIBFIXGRBYRX5/events.json","paper":"https://pith.science/paper/27G6AXEH"},"agent_actions":{"view_html":"https://pith.science/pith/27G6AXEHYWVEXQIBFIXGRBYRX5","download_json":"https://pith.science/pith/27G6AXEHYWVEXQIBFIXGRBYRX5.json","view_paper":"https://pith.science/paper/27G6AXEH","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/9302006&json=true","fetch_graph":"https://pith.science/api/pith-number/27G6AXEHYWVEXQIBFIXGRBYRX5/graph.json","fetch_events":"https://pith.science/api/pith-number/27G6AXEHYWVEXQIBFIXGRBYRX5/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/27G6AXEHYWVEXQIBFIXGRBYRX5/action/timestamp_anchor","attest_storage":"https://pith.science/pith/27G6AXEHYWVEXQIBFIXGRBYRX5/action/storage_attestation","attest_author":"https://pith.science/pith/27G6AXEHYWVEXQIBFIXGRBYRX5/action/author_attestation","sign_citation":"https://pith.science/pith/27G6AXEHYWVEXQIBFIXGRBYRX5/action/citation_signature","submit_replication":"https://pith.science/pith/27G6AXEHYWVEXQIBFIXGRBYRX5/action/replication_record"}},"created_at":"2026-07-04T15:07:15.439359+00:00","updated_at":"2026-07-04T15:07:15.439359+00:00"}