{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2004:NPFTI7EP6GP3CNUQCPUCR2GQQK","short_pith_number":"pith:NPFTI7EP","schema_version":"1.0","canonical_sha256":"6bcb347c8ff19fb1369013e828e8d082874b1bfc5636cda28372b06d53929680","source":{"kind":"arxiv","id":"astro-ph/0404457","version":4},"attestation_state":"computed","paper":{"title":"A New calculation of the atmospheric neutrino flux in a 3-dimensional scheme","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"K.kasahara, M.Honda, S.Midorikawa, T.Kajita","submitted_at":"2004-04-23T04:03:00Z","abstract_excerpt":"We have revised the calculation of the flux of atmospheric neutrinos based on a 3-dimensional scheme with the realistic IGRF geomagnetic model. The primary flux model has been revised, based on the AMS and BESS observations, and the interaction model updated to DPMJET-III. With a fast simulation code and computer system, the statistical errors in the Monte Carlo study are negligible. We estimate the total uncertainty of the atmospheric neutrino flux prediction is reduced to $\\lesssim$ 10 % below 10 GeV. The `3-dimensional effects' are found to be almost the same as the study with the dipole ma"},"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/0404457","kind":"arxiv","version":4},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2004-04-23T04:03:00Z","cross_cats_sorted":[],"title_canon_sha256":"c86b0473a380a62a76459bdeca8f56d03989511607d4dca8dc8ce982cb32aa16","abstract_canon_sha256":"7991f6964cc4ecf1db324be1c7010b04d17ef5eea5bdb90754458d3908f38c49"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T16:43:38.043150Z","signature_b64":"SelIssPdj87YUQsLGVYB1eWRcqh/97x/xqoa2ZdewIeVkkP1cssAtjdkLCtCuo+vYSUnXMQiX4KNpSdP8jiFCA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"6bcb347c8ff19fb1369013e828e8d082874b1bfc5636cda28372b06d53929680","last_reissued_at":"2026-07-04T16:43:38.042710Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T16:43:38.042710Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"A New calculation of the atmospheric neutrino flux in a 3-dimensional scheme","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"K.kasahara, M.Honda, S.Midorikawa, T.Kajita","submitted_at":"2004-04-23T04:03:00Z","abstract_excerpt":"We have revised the calculation of the flux of atmospheric neutrinos based on a 3-dimensional scheme with the realistic IGRF geomagnetic model. The primary flux model has been revised, based on the AMS and BESS observations, and the interaction model updated to DPMJET-III. With a fast simulation code and computer system, the statistical errors in the Monte Carlo study are negligible. We estimate the total uncertainty of the atmospheric neutrino flux prediction is reduced to $\\lesssim$ 10 % below 10 GeV. The `3-dimensional effects' are found to be almost the same as the study with the dipole ma"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0404457","kind":"arxiv","version":4},"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/0404457/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/0404457","created_at":"2026-07-04T16:43:38.042804+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/0404457v4","created_at":"2026-07-04T16:43:38.042804+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/0404457","created_at":"2026-07-04T16:43:38.042804+00:00"},{"alias_kind":"pith_short_12","alias_value":"NPFTI7EP6GP3","created_at":"2026-07-04T16:43:38.042804+00:00"},{"alias_kind":"pith_short_16","alias_value":"NPFTI7EP6GP3CNUQ","created_at":"2026-07-04T16:43:38.042804+00:00"},{"alias_kind":"pith_short_8","alias_value":"NPFTI7EP","created_at":"2026-07-04T16:43:38.042804+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":2,"sample":[{"citing_arxiv_id":"2605.16721","citing_title":"Towards Measuring the CP-Violating Phase with Atmospheric Neutrinos","ref_index":86,"is_internal_anchor":true},{"citing_arxiv_id":"2605.16721","citing_title":"Towards Measuring the CP-Violating Phase with Atmospheric Neutrinos","ref_index":86,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/NPFTI7EP6GP3CNUQCPUCR2GQQK","json":"https://pith.science/pith/NPFTI7EP6GP3CNUQCPUCR2GQQK.json","graph_json":"https://pith.science/api/pith-number/NPFTI7EP6GP3CNUQCPUCR2GQQK/graph.json","events_json":"https://pith.science/api/pith-number/NPFTI7EP6GP3CNUQCPUCR2GQQK/events.json","paper":"https://pith.science/paper/NPFTI7EP"},"agent_actions":{"view_html":"https://pith.science/pith/NPFTI7EP6GP3CNUQCPUCR2GQQK","download_json":"https://pith.science/pith/NPFTI7EP6GP3CNUQCPUCR2GQQK.json","view_paper":"https://pith.science/paper/NPFTI7EP","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/0404457&json=true","fetch_graph":"https://pith.science/api/pith-number/NPFTI7EP6GP3CNUQCPUCR2GQQK/graph.json","fetch_events":"https://pith.science/api/pith-number/NPFTI7EP6GP3CNUQCPUCR2GQQK/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/NPFTI7EP6GP3CNUQCPUCR2GQQK/action/timestamp_anchor","attest_storage":"https://pith.science/pith/NPFTI7EP6GP3CNUQCPUCR2GQQK/action/storage_attestation","attest_author":"https://pith.science/pith/NPFTI7EP6GP3CNUQCPUCR2GQQK/action/author_attestation","sign_citation":"https://pith.science/pith/NPFTI7EP6GP3CNUQCPUCR2GQQK/action/citation_signature","submit_replication":"https://pith.science/pith/NPFTI7EP6GP3CNUQCPUCR2GQQK/action/replication_record"}},"created_at":"2026-07-04T16:43:38.042804+00:00","updated_at":"2026-07-04T16:43:38.042804+00:00"}