{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2020:LQYXR2LMTEKGAKFFZLLIAPTTK6","short_pith_number":"pith:LQYXR2LM","schema_version":"1.0","canonical_sha256":"5c3178e96c99146028a5cad6803e7357b7466dfea66d6872dd8c20f0d5a95973","source":{"kind":"arxiv","id":"2003.07997","version":1},"attestation_state":"computed","paper":{"title":"On the saturation mechanism of the fluctuation dynamo at ${\\text{Pr}_\\mathrm{M}} \\ge 1$","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["physics.flu-dyn","physics.plasm-ph"],"primary_cat":"astro-ph.GA","authors_text":"Amit Seta, Anvar Shukurov, Paul J. Bushby, Toby S. Wood","submitted_at":"2020-03-18T00:46:53Z","abstract_excerpt":"The presence of magnetic fields in many astrophysical objects is due to dynamo action, whereby a part of the kinetic energy is converted into magnetic energy. A turbulent dynamo that produces magnetic field structures on the same scale as the turbulent flow is known as the fluctuation dynamo. We use numerical simulations to explore the nonlinear, statistically steady state of the fluctuation dynamo in driven turbulence. We demonstrate that as the magnetic field growth saturates, its amplification and diffusion are both affected by the back-reaction of the Lorentz force upon the flow. The ampli"},"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":"2003.07997","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2020-03-18T00:46:53Z","cross_cats_sorted":["physics.flu-dyn","physics.plasm-ph"],"title_canon_sha256":"147d92021a99d6fa3e8405393b968c23dd51989eb20664ec38d02c2dbec28132","abstract_canon_sha256":"75d49bc512e6242483f683960532637ea23eb40f1a4b771967efa5506efb6fb4"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T00:49:03.266905Z","signature_b64":"TVFUXNntxgavKeNNiMNhhCv2D37LoO0Qn5ldTpenXog7EWHNu+WbMngwBlO/5skynGt1OGFx7Pg+R/IESgXSAg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"5c3178e96c99146028a5cad6803e7357b7466dfea66d6872dd8c20f0d5a95973","last_reissued_at":"2026-07-05T00:49:03.266451Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T00:49:03.266451Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"On the saturation mechanism of the fluctuation dynamo at ${\\text{Pr}_\\mathrm{M}} \\ge 1$","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["physics.flu-dyn","physics.plasm-ph"],"primary_cat":"astro-ph.GA","authors_text":"Amit Seta, Anvar Shukurov, Paul J. Bushby, Toby S. Wood","submitted_at":"2020-03-18T00:46:53Z","abstract_excerpt":"The presence of magnetic fields in many astrophysical objects is due to dynamo action, whereby a part of the kinetic energy is converted into magnetic energy. A turbulent dynamo that produces magnetic field structures on the same scale as the turbulent flow is known as the fluctuation dynamo. We use numerical simulations to explore the nonlinear, statistically steady state of the fluctuation dynamo in driven turbulence. We demonstrate that as the magnetic field growth saturates, its amplification and diffusion are both affected by the back-reaction of the Lorentz force upon the flow. The ampli"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2003.07997","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/2003.07997/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":"2003.07997","created_at":"2026-07-05T00:49:03.266514+00:00"},{"alias_kind":"arxiv_version","alias_value":"2003.07997v1","created_at":"2026-07-05T00:49:03.266514+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2003.07997","created_at":"2026-07-05T00:49:03.266514+00:00"},{"alias_kind":"pith_short_12","alias_value":"LQYXR2LMTEKG","created_at":"2026-07-05T00:49:03.266514+00:00"},{"alias_kind":"pith_short_16","alias_value":"LQYXR2LMTEKGAKFF","created_at":"2026-07-05T00:49:03.266514+00:00"},{"alias_kind":"pith_short_8","alias_value":"LQYXR2LM","created_at":"2026-07-05T00:49:03.266514+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":4,"internal_anchor_count":2,"sample":[{"citing_arxiv_id":"2607.07004","citing_title":"The dynamical origin of the magnetic field distributions in compressible turbulence","ref_index":44,"is_internal_anchor":true},{"citing_arxiv_id":"2607.06346","citing_title":"Unravelling Turbulence and Magnetic Fields in Galaxy Clusters with SKA and XRISM","ref_index":76,"is_internal_anchor":true},{"citing_arxiv_id":"2606.22596","citing_title":"Understanding the non-Gaussian nature of Galactic foreground emissions towards small scales","ref_index":49,"is_internal_anchor":false},{"citing_arxiv_id":"2509.09949","citing_title":"The universal growth of magnetic energy during the nonlinear phase of subsonic and supersonic small-scale dynamos","ref_index":44,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/LQYXR2LMTEKGAKFFZLLIAPTTK6","json":"https://pith.science/pith/LQYXR2LMTEKGAKFFZLLIAPTTK6.json","graph_json":"https://pith.science/api/pith-number/LQYXR2LMTEKGAKFFZLLIAPTTK6/graph.json","events_json":"https://pith.science/api/pith-number/LQYXR2LMTEKGAKFFZLLIAPTTK6/events.json","paper":"https://pith.science/paper/LQYXR2LM"},"agent_actions":{"view_html":"https://pith.science/pith/LQYXR2LMTEKGAKFFZLLIAPTTK6","download_json":"https://pith.science/pith/LQYXR2LMTEKGAKFFZLLIAPTTK6.json","view_paper":"https://pith.science/paper/LQYXR2LM","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2003.07997&json=true","fetch_graph":"https://pith.science/api/pith-number/LQYXR2LMTEKGAKFFZLLIAPTTK6/graph.json","fetch_events":"https://pith.science/api/pith-number/LQYXR2LMTEKGAKFFZLLIAPTTK6/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/LQYXR2LMTEKGAKFFZLLIAPTTK6/action/timestamp_anchor","attest_storage":"https://pith.science/pith/LQYXR2LMTEKGAKFFZLLIAPTTK6/action/storage_attestation","attest_author":"https://pith.science/pith/LQYXR2LMTEKGAKFFZLLIAPTTK6/action/author_attestation","sign_citation":"https://pith.science/pith/LQYXR2LMTEKGAKFFZLLIAPTTK6/action/citation_signature","submit_replication":"https://pith.science/pith/LQYXR2LMTEKGAKFFZLLIAPTTK6/action/replication_record"}},"created_at":"2026-07-05T00:49:03.266514+00:00","updated_at":"2026-07-05T00:49:03.266514+00:00"}