{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2021:FPRAYFSLBRXSVGDJJM4DMGC7BR","short_pith_number":"pith:FPRAYFSL","schema_version":"1.0","canonical_sha256":"2be20c164b0c6f2a98694b3836185f0c5817e338990352fb34a192b29d839bd6","source":{"kind":"arxiv","id":"2110.14723","version":1},"attestation_state":"computed","paper":{"title":"Time variation of the atmospheric neutrino flux at dark matter detectors","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"hep-ph","authors_text":"Louis E. Strigari, Rafael F. Lang, Yi Zhuang","submitted_at":"2021-10-27T19:20:54Z","abstract_excerpt":"The cosmic ray flux at the lowest energies, $\\lesssim 10$ GeV, is modulated by the solar cycle, inducing a time variation that is expected to carry over into the atmospheric neutrino flux at these energies. Here we estimate this time variation of the atmospheric neutrino flux at five prospective underground locations for multi-tonne scale dark matter detectors (CJPL, Kamioka, LNGS, SNOlab and SURF). We find that between solar minimum and solar maximum, the normalization of the flux changes by $\\sim 30\\%$ at a high-latitude location such as SURF, while it changes by a smaller amount, $\\lesssim "},"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":"2110.14723","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"hep-ph","submitted_at":"2021-10-27T19:20:54Z","cross_cats_sorted":["astro-ph.HE"],"title_canon_sha256":"601cd896aef94cf3a9e10a37390e3d5352ad56053b27f0cfe31f0af6af3a0c78","abstract_canon_sha256":"667cecf3c6fb6d22988a8d111538f7495846b027aebc13e578674e576299233e"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T03:57:14.609710Z","signature_b64":"ln6bu6UomXZ3NowFADtTnk8wP3mlQM1+yehOk6MVRfg7AcxO/Xc+fvGUY3SQAUc0hSPKQBCbDrsEaqnRbk5ACA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"2be20c164b0c6f2a98694b3836185f0c5817e338990352fb34a192b29d839bd6","last_reissued_at":"2026-07-05T03:57:14.609348Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T03:57:14.609348Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Time variation of the atmospheric neutrino flux at dark matter detectors","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"hep-ph","authors_text":"Louis E. Strigari, Rafael F. Lang, Yi Zhuang","submitted_at":"2021-10-27T19:20:54Z","abstract_excerpt":"The cosmic ray flux at the lowest energies, $\\lesssim 10$ GeV, is modulated by the solar cycle, inducing a time variation that is expected to carry over into the atmospheric neutrino flux at these energies. Here we estimate this time variation of the atmospheric neutrino flux at five prospective underground locations for multi-tonne scale dark matter detectors (CJPL, Kamioka, LNGS, SNOlab and SURF). We find that between solar minimum and solar maximum, the normalization of the flux changes by $\\sim 30\\%$ at a high-latitude location such as SURF, while it changes by a smaller amount, $\\lesssim "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2110.14723","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/2110.14723/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":"2110.14723","created_at":"2026-07-05T03:57:14.609406+00:00"},{"alias_kind":"arxiv_version","alias_value":"2110.14723v1","created_at":"2026-07-05T03:57:14.609406+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2110.14723","created_at":"2026-07-05T03:57:14.609406+00:00"},{"alias_kind":"pith_short_12","alias_value":"FPRAYFSLBRXS","created_at":"2026-07-05T03:57:14.609406+00:00"},{"alias_kind":"pith_short_16","alias_value":"FPRAYFSLBRXSVGDJ","created_at":"2026-07-05T03:57:14.609406+00:00"},{"alias_kind":"pith_short_8","alias_value":"FPRAYFSL","created_at":"2026-07-05T03:57:14.609406+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2505.09111","citing_title":"Measuring the Cosmic Ray Spectrum with Next Generation Neutrino Detectors","ref_index":51,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/FPRAYFSLBRXSVGDJJM4DMGC7BR","json":"https://pith.science/pith/FPRAYFSLBRXSVGDJJM4DMGC7BR.json","graph_json":"https://pith.science/api/pith-number/FPRAYFSLBRXSVGDJJM4DMGC7BR/graph.json","events_json":"https://pith.science/api/pith-number/FPRAYFSLBRXSVGDJJM4DMGC7BR/events.json","paper":"https://pith.science/paper/FPRAYFSL"},"agent_actions":{"view_html":"https://pith.science/pith/FPRAYFSLBRXSVGDJJM4DMGC7BR","download_json":"https://pith.science/pith/FPRAYFSLBRXSVGDJJM4DMGC7BR.json","view_paper":"https://pith.science/paper/FPRAYFSL","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2110.14723&json=true","fetch_graph":"https://pith.science/api/pith-number/FPRAYFSLBRXSVGDJJM4DMGC7BR/graph.json","fetch_events":"https://pith.science/api/pith-number/FPRAYFSLBRXSVGDJJM4DMGC7BR/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/FPRAYFSLBRXSVGDJJM4DMGC7BR/action/timestamp_anchor","attest_storage":"https://pith.science/pith/FPRAYFSLBRXSVGDJJM4DMGC7BR/action/storage_attestation","attest_author":"https://pith.science/pith/FPRAYFSLBRXSVGDJJM4DMGC7BR/action/author_attestation","sign_citation":"https://pith.science/pith/FPRAYFSLBRXSVGDJJM4DMGC7BR/action/citation_signature","submit_replication":"https://pith.science/pith/FPRAYFSLBRXSVGDJJM4DMGC7BR/action/replication_record"}},"created_at":"2026-07-05T03:57:14.609406+00:00","updated_at":"2026-07-05T03:57:14.609406+00:00"}