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While rotation rates from spots can be difficult to determine for older, less active stars, rotational splitting of asteroseismic oscillation frequencies can provide rotation rates for both active and quiescent stars, and so can confirm whether this effect really takes place on the main sequence.\n  We obtained asteroseismic rotation rates of 91 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":"2104.10919","kind":"arxiv","version":2},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.SR","submitted_at":"2021-04-22T08:19:34Z","cross_cats_sorted":["astro-ph.EP"],"title_canon_sha256":"2811441bb9af0b2c950f8ebe87d6597f8edef2ca801ea8469f35ac3cb056d5f8","abstract_canon_sha256":"31ae8903f62c19715be5f4eb8686e8132cd61e8d61e99ac6b06956cbd396ea7f"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T02:34:49.742045Z","signature_b64":"Pm+egfNS/qIqT6hWxsfbJsCNN0gbTECIya30CfWby+3caXQSZSAD29E551bX+UhZwoK9gv3ZVkZMSyTv4JJOCA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"7e69bb55dd15597ffed49d1c9f234deaf62a1bbf82842b1a727f816a72e56aa6","last_reissued_at":"2026-07-05T02:34:49.741590Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T02:34:49.741590Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Weakened magnetic braking supported by asteroseismic rotation rates of Kepler dwarfs","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.EP"],"primary_cat":"astro-ph.SR","authors_text":"Angela A. 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