{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2025:7GQRQH5M7YN4LQTPXOBDGJZWHW","short_pith_number":"pith:7GQRQH5M","schema_version":"1.0","canonical_sha256":"f9a1181facfe1bc5c26fbb823327363d9ba8587a355a48de1d326f246430516e","source":{"kind":"arxiv","id":"2501.13807","version":3},"attestation_state":"computed","paper":{"title":"Theory of the kinetic helicity effect on turbulent diffusion of magnetic and scalar fields","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.SR","physics.plasm-ph"],"primary_cat":"physics.flu-dyn","authors_text":"Axel Brandenburg, Igor Rogachevskii, Nathan Kleeorin","submitted_at":"2025-01-23T16:28:15Z","abstract_excerpt":"Kinetic helicity is a fundamental characteristics of astrophysical turbulent flows. It is not only responsible for the generation of large-scale magnetic fields in the Sun, stars, and spiral galaxies, but it also affects turbulent diffusion resulting in the dissipation of large-scale magnetic fields. Using the path integral approach for random helical velocity fields with a finite correlation time and large Reynolds numbers, we show that turbulent magnetic diffusion is reduced by the kinetic helicity, while the turbulent diffusivity of a passive scalar is enhanced by the helicity. The latter c"},"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":"2501.13807","kind":"arxiv","version":3},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"physics.flu-dyn","submitted_at":"2025-01-23T16:28:15Z","cross_cats_sorted":["astro-ph.SR","physics.plasm-ph"],"title_canon_sha256":"159fc01581e99bdcc2ff20819199839a4a2b3d895bb792cfb7c47a75d76ef2ee","abstract_canon_sha256":"9399458131a67bc01c5741cd520fb0a1f4b53a30000224a94e6626abdba8cd65"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T11:02:41.206257Z","signature_b64":"DIPU1skXAoYSgdzqQQdrLi7cDlG43tXyra//fmIDTiBUGS5HJDoOM3s/qblGyIQaapMKt1b4h+qciIuuBVhvAA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"f9a1181facfe1bc5c26fbb823327363d9ba8587a355a48de1d326f246430516e","last_reissued_at":"2026-07-05T11:02:41.205702Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T11:02:41.205702Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Theory of the kinetic helicity effect on turbulent diffusion of magnetic and scalar fields","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.SR","physics.plasm-ph"],"primary_cat":"physics.flu-dyn","authors_text":"Axel Brandenburg, Igor Rogachevskii, Nathan Kleeorin","submitted_at":"2025-01-23T16:28:15Z","abstract_excerpt":"Kinetic helicity is a fundamental characteristics of astrophysical turbulent flows. It is not only responsible for the generation of large-scale magnetic fields in the Sun, stars, and spiral galaxies, but it also affects turbulent diffusion resulting in the dissipation of large-scale magnetic fields. Using the path integral approach for random helical velocity fields with a finite correlation time and large Reynolds numbers, we show that turbulent magnetic diffusion is reduced by the kinetic helicity, while the turbulent diffusivity of a passive scalar is enhanced by the helicity. The latter c"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2501.13807","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/2501.13807/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":"2501.13807","created_at":"2026-07-05T11:02:41.205760+00:00"},{"alias_kind":"arxiv_version","alias_value":"2501.13807v3","created_at":"2026-07-05T11:02:41.205760+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2501.13807","created_at":"2026-07-05T11:02:41.205760+00:00"},{"alias_kind":"pith_short_12","alias_value":"7GQRQH5M7YN4","created_at":"2026-07-05T11:02:41.205760+00:00"},{"alias_kind":"pith_short_16","alias_value":"7GQRQH5M7YN4LQTP","created_at":"2026-07-05T11:02:41.205760+00:00"},{"alias_kind":"pith_short_8","alias_value":"7GQRQH5M","created_at":"2026-07-05T11:02:41.205760+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2501.08879","citing_title":"Helicity effect on turbulent passive and active scalar diffusivities","ref_index":24,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/7GQRQH5M7YN4LQTPXOBDGJZWHW","json":"https://pith.science/pith/7GQRQH5M7YN4LQTPXOBDGJZWHW.json","graph_json":"https://pith.science/api/pith-number/7GQRQH5M7YN4LQTPXOBDGJZWHW/graph.json","events_json":"https://pith.science/api/pith-number/7GQRQH5M7YN4LQTPXOBDGJZWHW/events.json","paper":"https://pith.science/paper/7GQRQH5M"},"agent_actions":{"view_html":"https://pith.science/pith/7GQRQH5M7YN4LQTPXOBDGJZWHW","download_json":"https://pith.science/pith/7GQRQH5M7YN4LQTPXOBDGJZWHW.json","view_paper":"https://pith.science/paper/7GQRQH5M","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2501.13807&json=true","fetch_graph":"https://pith.science/api/pith-number/7GQRQH5M7YN4LQTPXOBDGJZWHW/graph.json","fetch_events":"https://pith.science/api/pith-number/7GQRQH5M7YN4LQTPXOBDGJZWHW/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/7GQRQH5M7YN4LQTPXOBDGJZWHW/action/timestamp_anchor","attest_storage":"https://pith.science/pith/7GQRQH5M7YN4LQTPXOBDGJZWHW/action/storage_attestation","attest_author":"https://pith.science/pith/7GQRQH5M7YN4LQTPXOBDGJZWHW/action/author_attestation","sign_citation":"https://pith.science/pith/7GQRQH5M7YN4LQTPXOBDGJZWHW/action/citation_signature","submit_replication":"https://pith.science/pith/7GQRQH5M7YN4LQTPXOBDGJZWHW/action/replication_record"}},"created_at":"2026-07-05T11:02:41.205760+00:00","updated_at":"2026-07-05T11:02:41.205760+00:00"}