{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2025:BSWKIEEILDM2GPSAL7RICHHW6R","short_pith_number":"pith:BSWKIEEI","schema_version":"1.0","canonical_sha256":"0caca4108858d9a33e405fe2811cf6f45cb4c03092a00c0ad16349a67ece0851","source":{"kind":"arxiv","id":"2503.03839","version":2},"attestation_state":"computed","paper":{"title":"Too fast to be single: Tidal evolution and photometric identification of stellar and planetary companions","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.EP"],"primary_cat":"astro-ph.SR","authors_text":"Hagai B. Perets, Ilay Kamai","submitted_at":"2025-03-05T19:04:28Z","abstract_excerpt":"Many stars, including those in binary or multiple systems, exhibit modified rotational evolution due to tidal interactions. While magnetic braking slows rotation in single stars, close binaries experience synchronization from tidal forces, resulting in high spin rates. Thus, fast rotators often signify synchronized binaries or planetary systems. We analyze stellar rotation in the Kepler field to photometrically identify non-single systems. Establishing an initial rotation-temperature relationship for individual stars via young clusters, we confirm our findings through magnitude excess and prio"},"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":"2503.03839","kind":"arxiv","version":2},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.SR","submitted_at":"2025-03-05T19:04:28Z","cross_cats_sorted":["astro-ph.EP"],"title_canon_sha256":"ea69c6312ded2cdc559c146de5ceeda4265ec64af0da615ad5328f845248dbec","abstract_canon_sha256":"b333725d3935f9a23209df0651013595a5bf888c058a5aae5e37aae5462e264f"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T11:03:57.513706Z","signature_b64":"ba1L9Tayixh4MplZdYckwKRloSYTRydKbxR+O9LbnkJscgXGYH4ye8+1aOY6TWHx2UbsoIkFtcjDIA2Y1eSfCQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"0caca4108858d9a33e405fe2811cf6f45cb4c03092a00c0ad16349a67ece0851","last_reissued_at":"2026-07-05T11:03:57.513268Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T11:03:57.513268Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Too fast to be single: Tidal evolution and photometric identification of stellar and planetary companions","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.EP"],"primary_cat":"astro-ph.SR","authors_text":"Hagai B. Perets, Ilay Kamai","submitted_at":"2025-03-05T19:04:28Z","abstract_excerpt":"Many stars, including those in binary or multiple systems, exhibit modified rotational evolution due to tidal interactions. While magnetic braking slows rotation in single stars, close binaries experience synchronization from tidal forces, resulting in high spin rates. Thus, fast rotators often signify synchronized binaries or planetary systems. We analyze stellar rotation in the Kepler field to photometrically identify non-single systems. Establishing an initial rotation-temperature relationship for individual stars via young clusters, we confirm our findings through magnitude excess and prio"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2503.03839","kind":"arxiv","version":2},"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/2503.03839/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":"2503.03839","created_at":"2026-07-05T11:03:57.513322+00:00"},{"alias_kind":"arxiv_version","alias_value":"2503.03839v2","created_at":"2026-07-05T11:03:57.513322+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2503.03839","created_at":"2026-07-05T11:03:57.513322+00:00"},{"alias_kind":"pith_short_12","alias_value":"BSWKIEEILDM2","created_at":"2026-07-05T11:03:57.513322+00:00"},{"alias_kind":"pith_short_16","alias_value":"BSWKIEEILDM2GPSA","created_at":"2026-07-05T11:03:57.513322+00:00"},{"alias_kind":"pith_short_8","alias_value":"BSWKIEEI","created_at":"2026-07-05T11:03:57.513322+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2608.06604","citing_title":"The Maunder Model and Catalog: Stellar Rotation, Bimodal Activity, and Magnetic Braking in Kepler Main-Sequence Stars","ref_index":76,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/BSWKIEEILDM2GPSAL7RICHHW6R","json":"https://pith.science/pith/BSWKIEEILDM2GPSAL7RICHHW6R.json","graph_json":"https://pith.science/api/pith-number/BSWKIEEILDM2GPSAL7RICHHW6R/graph.json","events_json":"https://pith.science/api/pith-number/BSWKIEEILDM2GPSAL7RICHHW6R/events.json","paper":"https://pith.science/paper/BSWKIEEI"},"agent_actions":{"view_html":"https://pith.science/pith/BSWKIEEILDM2GPSAL7RICHHW6R","download_json":"https://pith.science/pith/BSWKIEEILDM2GPSAL7RICHHW6R.json","view_paper":"https://pith.science/paper/BSWKIEEI","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2503.03839&json=true","fetch_graph":"https://pith.science/api/pith-number/BSWKIEEILDM2GPSAL7RICHHW6R/graph.json","fetch_events":"https://pith.science/api/pith-number/BSWKIEEILDM2GPSAL7RICHHW6R/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/BSWKIEEILDM2GPSAL7RICHHW6R/action/timestamp_anchor","attest_storage":"https://pith.science/pith/BSWKIEEILDM2GPSAL7RICHHW6R/action/storage_attestation","attest_author":"https://pith.science/pith/BSWKIEEILDM2GPSAL7RICHHW6R/action/author_attestation","sign_citation":"https://pith.science/pith/BSWKIEEILDM2GPSAL7RICHHW6R/action/citation_signature","submit_replication":"https://pith.science/pith/BSWKIEEILDM2GPSAL7RICHHW6R/action/replication_record"}},"created_at":"2026-07-05T11:03:57.513322+00:00","updated_at":"2026-07-05T11:03:57.513322+00:00"}