{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2023:UL7RM2IGS3W3I2EFLYRRYM5YBX","short_pith_number":"pith:UL7RM2IG","schema_version":"1.0","canonical_sha256":"a2ff16690696edb468855e231c33b80dc6c7b883dfa3f1b88cf53298561ba920","source":{"kind":"arxiv","id":"2306.09119","version":1},"attestation_state":"computed","paper":{"title":"An abrupt change in the stellar spin-down law at the fully convective boundary","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"Louis Amard, Ruth Angus, Sean P. Matt, Victor See, Yuxi Lu","submitted_at":"2023-06-15T13:27:15Z","abstract_excerpt":"The importance of the existence of a radiative core in generating a solar-like magnetic dynamo is still unclear. Analytic models and magnetohydrodynamic simulations of stars suggest the thin layer between a star's radiative core and its convective zone can produce shearing that reproduces key characteristics of a solar-like dynamo. However, recent studies suggest fully and partially convective stars exhibit very similar period-activity relations, hinting that dynamos generated by stars with and without radiative cores hold similar properties. Here, using kinematic ages, we discover an abrupt 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":"2306.09119","kind":"arxiv","version":1},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.SR","submitted_at":"2023-06-15T13:27:15Z","cross_cats_sorted":[],"title_canon_sha256":"7d8da2ee5590f72019cc27060804d8a529d6791818103c89e16809bd36410707","abstract_canon_sha256":"603c27a859ce54fda77de4c6bf9f08e3b1237b1b666fe5312eb3ec90ee29c122"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T06:21:09.021000Z","signature_b64":"QSsBXtAxLp7LXm8R09w3RPi2WaVyvtVAIESFC7TbXT3XizS4WQIFDCQeHdYPMdl3hb5ugh4mpofgRZQTSbKtAQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"a2ff16690696edb468855e231c33b80dc6c7b883dfa3f1b88cf53298561ba920","last_reissued_at":"2026-07-05T06:21:09.020514Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T06:21:09.020514Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"An abrupt change in the stellar spin-down law at the fully convective boundary","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"Louis Amard, Ruth Angus, Sean P. Matt, Victor See, Yuxi Lu","submitted_at":"2023-06-15T13:27:15Z","abstract_excerpt":"The importance of the existence of a radiative core in generating a solar-like magnetic dynamo is still unclear. Analytic models and magnetohydrodynamic simulations of stars suggest the thin layer between a star's radiative core and its convective zone can produce shearing that reproduces key characteristics of a solar-like dynamo. However, recent studies suggest fully and partially convective stars exhibit very similar period-activity relations, hinting that dynamos generated by stars with and without radiative cores hold similar properties. Here, using kinematic ages, we discover an abrupt c"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2306.09119","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/2306.09119/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":"2306.09119","created_at":"2026-07-05T06:21:09.020574+00:00"},{"alias_kind":"arxiv_version","alias_value":"2306.09119v1","created_at":"2026-07-05T06:21:09.020574+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2306.09119","created_at":"2026-07-05T06:21:09.020574+00:00"},{"alias_kind":"pith_short_12","alias_value":"UL7RM2IGS3W3","created_at":"2026-07-05T06:21:09.020574+00:00"},{"alias_kind":"pith_short_16","alias_value":"UL7RM2IGS3W3I2EF","created_at":"2026-07-05T06:21:09.020574+00:00"},{"alias_kind":"pith_short_8","alias_value":"UL7RM2IG","created_at":"2026-07-05T06:21:09.020574+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2607.08050","citing_title":"RedDots: Magnetic field of the nearby active M dwarf GJ 729, and a search for companions","ref_index":137,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/UL7RM2IGS3W3I2EFLYRRYM5YBX","json":"https://pith.science/pith/UL7RM2IGS3W3I2EFLYRRYM5YBX.json","graph_json":"https://pith.science/api/pith-number/UL7RM2IGS3W3I2EFLYRRYM5YBX/graph.json","events_json":"https://pith.science/api/pith-number/UL7RM2IGS3W3I2EFLYRRYM5YBX/events.json","paper":"https://pith.science/paper/UL7RM2IG"},"agent_actions":{"view_html":"https://pith.science/pith/UL7RM2IGS3W3I2EFLYRRYM5YBX","download_json":"https://pith.science/pith/UL7RM2IGS3W3I2EFLYRRYM5YBX.json","view_paper":"https://pith.science/paper/UL7RM2IG","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2306.09119&json=true","fetch_graph":"https://pith.science/api/pith-number/UL7RM2IGS3W3I2EFLYRRYM5YBX/graph.json","fetch_events":"https://pith.science/api/pith-number/UL7RM2IGS3W3I2EFLYRRYM5YBX/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/UL7RM2IGS3W3I2EFLYRRYM5YBX/action/timestamp_anchor","attest_storage":"https://pith.science/pith/UL7RM2IGS3W3I2EFLYRRYM5YBX/action/storage_attestation","attest_author":"https://pith.science/pith/UL7RM2IGS3W3I2EFLYRRYM5YBX/action/author_attestation","sign_citation":"https://pith.science/pith/UL7RM2IGS3W3I2EFLYRRYM5YBX/action/citation_signature","submit_replication":"https://pith.science/pith/UL7RM2IGS3W3I2EFLYRRYM5YBX/action/replication_record"}},"created_at":"2026-07-05T06:21:09.020574+00:00","updated_at":"2026-07-05T06:21:09.020574+00:00"}