{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2013:SWKITUBJO2JZQEXWPUS4U6VSJ7","short_pith_number":"pith:SWKITUBJ","schema_version":"1.0","canonical_sha256":"959489d02976939812f67d25ca7ab24fe70a111683e06efff6059da45bc99346","source":{"kind":"arxiv","id":"1311.2044","version":3},"attestation_state":"computed","paper":{"title":"Testing the Newborn Pulsar Origin of Ultrahigh Energy Cosmic Rays with EeV Neutrinos","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"Angela V. Olinto, Ke Fang, Kohta Murase, Kumiko Kotera","submitted_at":"2013-11-08T19:33:02Z","abstract_excerpt":"Fast-spinning newborn pulsars are intriguing candidate sources of ultrahigh energy cosmic rays (UHECRs). The acceleration of particles with a given composition in a fraction of the extragalactic pulsar population can give a consistent explanation for the measurements of the Auger Observatory. We calculate the associated diffuse neutrino flux produced while particles cross the supernova ejecta surrounding the stars. We show that in the minimal pulsar scenario that are compatible with the UHECR data, the effective optical depth to hadronuclear interactions is larger than unity at ultrahigh energ"},"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":"1311.2044","kind":"arxiv","version":3},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2013-11-08T19:33:02Z","cross_cats_sorted":[],"title_canon_sha256":"1b8403c7fb44ff473c6e3e535b6d6501addafebf3dba63ed091e005fa46f55d6","abstract_canon_sha256":"716d270f748d7bd94b2e2975dc96f48f9c103c9586618571ed269f73617ba1b8"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:21:13.998499Z","signature_b64":"PBSpsQi+Z5uMy+4Bd+EGi+kH0BjpWdEPAd/iLlELPHQ+WF5++kurSeoDKPjUYEC8Xu9sSxTZ5cvr+uswEnfdBg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"959489d02976939812f67d25ca7ab24fe70a111683e06efff6059da45bc99346","last_reissued_at":"2026-05-18T01:21:13.997775Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:21:13.997775Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Testing the Newborn Pulsar Origin of Ultrahigh Energy Cosmic Rays with EeV Neutrinos","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"Angela V. Olinto, Ke Fang, Kohta Murase, Kumiko Kotera","submitted_at":"2013-11-08T19:33:02Z","abstract_excerpt":"Fast-spinning newborn pulsars are intriguing candidate sources of ultrahigh energy cosmic rays (UHECRs). The acceleration of particles with a given composition in a fraction of the extragalactic pulsar population can give a consistent explanation for the measurements of the Auger Observatory. We calculate the associated diffuse neutrino flux produced while particles cross the supernova ejecta surrounding the stars. We show that in the minimal pulsar scenario that are compatible with the UHECR data, the effective optical depth to hadronuclear interactions is larger than unity at ultrahigh energ"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1311.2044","kind":"arxiv","version":3},"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":"1311.2044","created_at":"2026-05-18T01:21:13.997887+00:00"},{"alias_kind":"arxiv_version","alias_value":"1311.2044v3","created_at":"2026-05-18T01:21:13.997887+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1311.2044","created_at":"2026-05-18T01:21:13.997887+00:00"},{"alias_kind":"pith_short_12","alias_value":"SWKITUBJO2JZ","created_at":"2026-05-18T12:27:59.945178+00:00"},{"alias_kind":"pith_short_16","alias_value":"SWKITUBJO2JZQEXW","created_at":"2026-05-18T12:27:59.945178+00:00"},{"alias_kind":"pith_short_8","alias_value":"SWKITUBJ","created_at":"2026-05-18T12:27:59.945178+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":3,"internal_anchor_count":2,"sample":[{"citing_arxiv_id":"2512.00660","citing_title":"Particle Astrophysics with High and Ultrahigh Energy Neutrinos","ref_index":90,"is_internal_anchor":true},{"citing_arxiv_id":"2512.20594","citing_title":"The Sensitivity of PUEO to Cosmogenic Neutrinos and Exotic Physics Scenarios","ref_index":90,"is_internal_anchor":true},{"citing_arxiv_id":"2605.04268","citing_title":"Sensitivity of the As-Built Askaryan Radio Array to Ultra-High Energy Neutrinos","ref_index":38,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/SWKITUBJO2JZQEXWPUS4U6VSJ7","json":"https://pith.science/pith/SWKITUBJO2JZQEXWPUS4U6VSJ7.json","graph_json":"https://pith.science/api/pith-number/SWKITUBJO2JZQEXWPUS4U6VSJ7/graph.json","events_json":"https://pith.science/api/pith-number/SWKITUBJO2JZQEXWPUS4U6VSJ7/events.json","paper":"https://pith.science/paper/SWKITUBJ"},"agent_actions":{"view_html":"https://pith.science/pith/SWKITUBJO2JZQEXWPUS4U6VSJ7","download_json":"https://pith.science/pith/SWKITUBJO2JZQEXWPUS4U6VSJ7.json","view_paper":"https://pith.science/paper/SWKITUBJ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1311.2044&json=true","fetch_graph":"https://pith.science/api/pith-number/SWKITUBJO2JZQEXWPUS4U6VSJ7/graph.json","fetch_events":"https://pith.science/api/pith-number/SWKITUBJO2JZQEXWPUS4U6VSJ7/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/SWKITUBJO2JZQEXWPUS4U6VSJ7/action/timestamp_anchor","attest_storage":"https://pith.science/pith/SWKITUBJO2JZQEXWPUS4U6VSJ7/action/storage_attestation","attest_author":"https://pith.science/pith/SWKITUBJO2JZQEXWPUS4U6VSJ7/action/author_attestation","sign_citation":"https://pith.science/pith/SWKITUBJO2JZQEXWPUS4U6VSJ7/action/citation_signature","submit_replication":"https://pith.science/pith/SWKITUBJO2JZQEXWPUS4U6VSJ7/action/replication_record"}},"created_at":"2026-05-18T01:21:13.997887+00:00","updated_at":"2026-05-18T01:21:13.997887+00:00"}