{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2008:353YKAIOKT6SRE7RV736WJGVKU","short_pith_number":"pith:353YKAIO","schema_version":"1.0","canonical_sha256":"df7785010e54fd2893f1aff7eb24d55533ab621fa303e6a553acdec661241ebc","source":{"kind":"arxiv","id":"0803.4312","version":1},"attestation_state":"computed","paper":{"title":"Solar neutrino measurements in Super-Kamiokande-II","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"hep-ex","authors_text":"the Super-Kamiokande collaboration","submitted_at":"2008-03-30T10:03:53Z","abstract_excerpt":"The results of the second phase of the Super-Kamiokande solar neutrino measurement are presented and compared to the first phase. The solar neutrino flux spectrum and time-variation as well as oscillation results are statistically consistent with the first phase and do not show spectral distortion. The time-dependent flux measurement of the combined first and second phases coincides with the full period of solar cycle 23 and shows no correlation with solar activity. The measured boron 8 total flux is 2.38 +/-0.05(stat.) +0.16-0.15(sys.) X 10^6 cm^-2 sec^-1 and the day-night difference is found"},"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":"0803.4312","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"hep-ex","submitted_at":"2008-03-30T10:03:53Z","cross_cats_sorted":[],"title_canon_sha256":"c427fecea64b0c02458114c72dd935137f23dd52bedc8c164fe3689e14ca0c86","abstract_canon_sha256":"d2cdc0517f7aec66e4e121100f2479480f2b0553a764f6cf0a210d63afdc6b3d"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T15:29:57.527910Z","signature_b64":"4lGU9l30llhMR5yyX74V2QMYUB6t+Xf2ECXOZg04e+4RmHotr+Wmv2SD/B6eRQYPpt5HhLw4GjN+VgOxH1P7CA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"df7785010e54fd2893f1aff7eb24d55533ab621fa303e6a553acdec661241ebc","last_reissued_at":"2026-07-04T15:29:57.527413Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T15:29:57.527413Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Solar neutrino measurements in Super-Kamiokande-II","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"hep-ex","authors_text":"the Super-Kamiokande collaboration","submitted_at":"2008-03-30T10:03:53Z","abstract_excerpt":"The results of the second phase of the Super-Kamiokande solar neutrino measurement are presented and compared to the first phase. The solar neutrino flux spectrum and time-variation as well as oscillation results are statistically consistent with the first phase and do not show spectral distortion. The time-dependent flux measurement of the combined first and second phases coincides with the full period of solar cycle 23 and shows no correlation with solar activity. The measured boron 8 total flux is 2.38 +/-0.05(stat.) +0.16-0.15(sys.) X 10^6 cm^-2 sec^-1 and the day-night difference is found"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"0803.4312","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/0803.4312/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":"0803.4312","created_at":"2026-07-04T15:29:57.527476+00:00"},{"alias_kind":"arxiv_version","alias_value":"0803.4312v1","created_at":"2026-07-04T15:29:57.527476+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.0803.4312","created_at":"2026-07-04T15:29:57.527476+00:00"},{"alias_kind":"pith_short_12","alias_value":"353YKAIOKT6S","created_at":"2026-07-04T15:29:57.527476+00:00"},{"alias_kind":"pith_short_16","alias_value":"353YKAIOKT6SRE7R","created_at":"2026-07-04T15:29:57.527476+00:00"},{"alias_kind":"pith_short_8","alias_value":"353YKAIO","created_at":"2026-07-04T15:29:57.527476+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":5,"internal_anchor_count":5,"sample":[{"citing_arxiv_id":"2606.12915","citing_title":"Mass Varying Neutrino Oscillation in Teleparallel Gravity","ref_index":58,"is_internal_anchor":true},{"citing_arxiv_id":"2606.12155","citing_title":"Improving the Angular Resolution of IBD Events Using Neutron Capture Information in Super-Kamiokande","ref_index":56,"is_internal_anchor":true},{"citing_arxiv_id":"2606.09998","citing_title":"Constraints and Projections for Millicharged Dark Matter in the Sun with Water Cherenkov Neutrino Detectors","ref_index":117,"is_internal_anchor":true},{"citing_arxiv_id":"2006.11237","citing_title":"2020 Global reassessment of the neutrino oscillation picture","ref_index":40,"is_internal_anchor":true},{"citing_arxiv_id":"2605.13955","citing_title":"Exploring neutrino loss with diffuse astrophysical neutrino fluxes","ref_index":23,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/353YKAIOKT6SRE7RV736WJGVKU","json":"https://pith.science/pith/353YKAIOKT6SRE7RV736WJGVKU.json","graph_json":"https://pith.science/api/pith-number/353YKAIOKT6SRE7RV736WJGVKU/graph.json","events_json":"https://pith.science/api/pith-number/353YKAIOKT6SRE7RV736WJGVKU/events.json","paper":"https://pith.science/paper/353YKAIO"},"agent_actions":{"view_html":"https://pith.science/pith/353YKAIOKT6SRE7RV736WJGVKU","download_json":"https://pith.science/pith/353YKAIOKT6SRE7RV736WJGVKU.json","view_paper":"https://pith.science/paper/353YKAIO","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=0803.4312&json=true","fetch_graph":"https://pith.science/api/pith-number/353YKAIOKT6SRE7RV736WJGVKU/graph.json","fetch_events":"https://pith.science/api/pith-number/353YKAIOKT6SRE7RV736WJGVKU/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/353YKAIOKT6SRE7RV736WJGVKU/action/timestamp_anchor","attest_storage":"https://pith.science/pith/353YKAIOKT6SRE7RV736WJGVKU/action/storage_attestation","attest_author":"https://pith.science/pith/353YKAIOKT6SRE7RV736WJGVKU/action/author_attestation","sign_citation":"https://pith.science/pith/353YKAIOKT6SRE7RV736WJGVKU/action/citation_signature","submit_replication":"https://pith.science/pith/353YKAIOKT6SRE7RV736WJGVKU/action/replication_record"}},"created_at":"2026-07-04T15:29:57.527476+00:00","updated_at":"2026-07-04T15:29:57.527476+00:00"}