{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2022:4AXMOKWG7DVKNRTFRBN5WF2UZQ","short_pith_number":"pith:4AXMOKWG","schema_version":"1.0","canonical_sha256":"e02ec72ac6f8eaa6c665885bdb1754cc2964768a8791e931c6c8903bea892bad","source":{"kind":"arxiv","id":"2204.06646","version":1},"attestation_state":"computed","paper":{"title":"The Many-Faceted Light Curves of Young Disk-bearing Stars in Taurus as Seen by K2","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.GA"],"primary_cat":"astro-ph.SR","authors_text":"Ann Marie Cody, Luisa M. Rebull, Lynne A. Hillenbrand","submitted_at":"2022-04-13T21:48:04Z","abstract_excerpt":"We present a comprehensive study of the variability properties of young disk-bearing stars in the Taurus star-forming region, paralleling our previous investigation in rho Oph and Upper Sco. A sample of 99 confirmed Taurus association members is placed in the diagnostic Q-M plane of flux asymmetry (M) and quasi-periodicity (Q), which guides our assignment of variability classes. We find a similar proportion of flux-symmetric variables in Taurus, but more bursters and fewer dippers relative to Upper Sco. The regions also differ in that the amplitudes for periodic and quasi-periodic sources are "},"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":"2204.06646","kind":"arxiv","version":1},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.SR","submitted_at":"2022-04-13T21:48:04Z","cross_cats_sorted":["astro-ph.GA"],"title_canon_sha256":"1a56824653b902e1be066f86aa04b074a5b43d634d71d1f5d628c6a0e6ea378f","abstract_canon_sha256":"d279ed327eaca29eb66b6d8da2b18f78fb2d8d662a5f3027c1c96618b089d376"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T04:14:44.235828Z","signature_b64":"JauakNvSLC6mqOx6TAeNpNplVJ2tR9tYEZg79mKQQ/0A5pZcxpXQeMRNI3xfkl6vRLq8uQx8n6mvwD+CdFArCA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"e02ec72ac6f8eaa6c665885bdb1754cc2964768a8791e931c6c8903bea892bad","last_reissued_at":"2026-07-05T04:14:44.235474Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T04:14:44.235474Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The Many-Faceted Light Curves of Young Disk-bearing Stars in Taurus as Seen by K2","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.GA"],"primary_cat":"astro-ph.SR","authors_text":"Ann Marie Cody, Luisa M. Rebull, Lynne A. Hillenbrand","submitted_at":"2022-04-13T21:48:04Z","abstract_excerpt":"We present a comprehensive study of the variability properties of young disk-bearing stars in the Taurus star-forming region, paralleling our previous investigation in rho Oph and Upper Sco. A sample of 99 confirmed Taurus association members is placed in the diagnostic Q-M plane of flux asymmetry (M) and quasi-periodicity (Q), which guides our assignment of variability classes. We find a similar proportion of flux-symmetric variables in Taurus, but more bursters and fewer dippers relative to Upper Sco. The regions also differ in that the amplitudes for periodic and quasi-periodic sources are "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2204.06646","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/2204.06646/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":"2204.06646","created_at":"2026-07-05T04:14:44.235525+00:00"},{"alias_kind":"arxiv_version","alias_value":"2204.06646v1","created_at":"2026-07-05T04:14:44.235525+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2204.06646","created_at":"2026-07-05T04:14:44.235525+00:00"},{"alias_kind":"pith_short_12","alias_value":"4AXMOKWG7DVK","created_at":"2026-07-05T04:14:44.235525+00:00"},{"alias_kind":"pith_short_16","alias_value":"4AXMOKWG7DVKNRTF","created_at":"2026-07-05T04:14:44.235525+00:00"},{"alias_kind":"pith_short_8","alias_value":"4AXMOKWG","created_at":"2026-07-05T04:14:44.235525+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2607.11674","citing_title":"Unstable magnetospheric accretion on the T Tauri star TW Hya","ref_index":20,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/4AXMOKWG7DVKNRTFRBN5WF2UZQ","json":"https://pith.science/pith/4AXMOKWG7DVKNRTFRBN5WF2UZQ.json","graph_json":"https://pith.science/api/pith-number/4AXMOKWG7DVKNRTFRBN5WF2UZQ/graph.json","events_json":"https://pith.science/api/pith-number/4AXMOKWG7DVKNRTFRBN5WF2UZQ/events.json","paper":"https://pith.science/paper/4AXMOKWG"},"agent_actions":{"view_html":"https://pith.science/pith/4AXMOKWG7DVKNRTFRBN5WF2UZQ","download_json":"https://pith.science/pith/4AXMOKWG7DVKNRTFRBN5WF2UZQ.json","view_paper":"https://pith.science/paper/4AXMOKWG","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2204.06646&json=true","fetch_graph":"https://pith.science/api/pith-number/4AXMOKWG7DVKNRTFRBN5WF2UZQ/graph.json","fetch_events":"https://pith.science/api/pith-number/4AXMOKWG7DVKNRTFRBN5WF2UZQ/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/4AXMOKWG7DVKNRTFRBN5WF2UZQ/action/timestamp_anchor","attest_storage":"https://pith.science/pith/4AXMOKWG7DVKNRTFRBN5WF2UZQ/action/storage_attestation","attest_author":"https://pith.science/pith/4AXMOKWG7DVKNRTFRBN5WF2UZQ/action/author_attestation","sign_citation":"https://pith.science/pith/4AXMOKWG7DVKNRTFRBN5WF2UZQ/action/citation_signature","submit_replication":"https://pith.science/pith/4AXMOKWG7DVKNRTFRBN5WF2UZQ/action/replication_record"}},"created_at":"2026-07-05T04:14:44.235525+00:00","updated_at":"2026-07-05T04:14:44.235525+00:00"}