{"paper":{"title":"The rotation-magnetism relationship in solar-type stars. Constraining magnetic flux emergence rates","license":"http://creativecommons.org/licenses/by-nc-sa/4.0/","headline":"Magnetic flux emergence rates in solar-type stars must scale with the 1.9 power of rotation rate to match observed field strengths.","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"Alexander I. Shapiro, Emre Isik, Natalie A. Krivova, Sami K. Solanki","submitted_at":"2025-12-19T22:07:37Z","abstract_excerpt":"The rotation-activity relationship of G-type stars results from surface magnetic fields emerging from the interior. How the magnetic flux and its emergence rate scale with rotation rate are not well understood, both observationally and theoretically. We aim at constraining the emerging magnetic flux as a function of the rotation rate in solar-type stars by numerical simulations compared to empirical constraints set by direct measurements of stellar magnetic fields. We use our Flux Emergence And Transport (FEAT) model for stars with a range of power-law slopes for the dependence of emerging flu"},"claims":{"count":4,"items":[{"kind":"strongest_claim","text":"magnetic flux emergence rates must scale steeply with rotation (power-law exponent of about 1.9) to reproduce observed field strengths, significantly exceeding the estimates in the literature","source":"verdict.strongest_claim","status":"machine_extracted","claim_id":"C1","attestation":"unclaimed"},{"kind":"weakest_assumption","text":"The heuristic decomposition of total surface flux into active-region and small-scale-dynamo components plus the assumption that the FEAT transport physics remains valid across the full range of rotation rates and metallicities tested","source":"verdict.weakest_assumption","status":"machine_extracted","claim_id":"C2","attestation":"unclaimed"},{"kind":"one_line_summary","text":"Magnetic flux emergence rates in G-type stars must scale as rotation to the power ~1.9 to match observed surface field strengths, after correcting for metallicity and effective temperature effects.","source":"verdict.one_line_summary","status":"machine_extracted","claim_id":"C3","attestation":"unclaimed"},{"kind":"headline","text":"Magnetic flux emergence rates in solar-type stars must scale with the 1.9 power of rotation rate to match observed field strengths.","source":"verdict.pith_extraction.headline","status":"machine_extracted","claim_id":"C4","attestation":"unclaimed"}],"snapshot_sha256":"f43652579566b63de13bac24faab5656334b1eae3f69d161b756f319d1d2717a"},"source":{"id":"2512.18095","kind":"arxiv","version":3},"verdict":{"id":"28da07cf-ee41-43cb-91d4-5eb8fd9c83bd","model_set":{"reader":"grok-4.3"},"created_at":"2026-05-16T20:16:48.022254Z","strongest_claim":"magnetic flux emergence rates must scale steeply with rotation (power-law exponent of about 1.9) to reproduce observed field strengths, significantly exceeding the estimates in the literature","one_line_summary":"Magnetic flux emergence rates in G-type stars must scale as rotation to the power ~1.9 to match observed surface field strengths, after correcting for metallicity and effective temperature effects.","pipeline_version":"pith-pipeline@v0.9.0","weakest_assumption":"The heuristic decomposition of total surface flux into active-region and small-scale-dynamo components plus the assumption that the FEAT transport physics remains valid across the full range of rotation rates and metallicities tested","pith_extraction_headline":"Magnetic flux emergence rates in solar-type stars must scale with the 1.9 power of rotation rate to match observed field strengths."},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/2512.18095/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":2,"snapshot_sha256":"289c2f0980ff0fd0e638ee1538ad95edccf638216ec58a6b921a92de892c9c2e"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"}