{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2012:6EI75B6GZH3GRPRYCEZ4ZAYCV7","short_pith_number":"pith:6EI75B6G","schema_version":"1.0","canonical_sha256":"f111fe87c6c9f668be381133cc8302afe5174c92a4d9e7e22f88926cf1be266e","source":{"kind":"arxiv","id":"1206.5238","version":1},"attestation_state":"computed","paper":{"title":"Can we predict the global magnetic topology of a pre-main sequence star from its position in the Hertzsprung-Russell diagram?","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"(2) Toulouse, (3) G\\\"ottingen, 4), (4) DIAS, (5) ESO, (6) Exeter, (7) St Andrews), G. A. J. Hussain (5), J.-F. Donati (2), J. Morin (3, L. A. Hillenbrand (1), M. Jardine (7) ((1) Caltech, N. J. Mayne (6), S. G. Gregory (1)","submitted_at":"2012-06-22T19:53:59Z","abstract_excerpt":"ZDI studies have shown that the magnetic fields of T Tauri stars can be significantly more complex than a simple dipole and can vary markedly between sources. We collect and summarize the magnetic field topology information obtained to date and present Hertzsprung-Russell (HR) diagrams for the stars in the sample. Intriguingly, the large scale field topology of a given pre-main sequence (PMS) star is strongly dependent upon the stellar internal structure, with the strength of the dipole component of its multipolar magnetic field decaying rapidly with the development of a radiative core. Using "},"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":"1206.5238","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2012-06-22T19:53:59Z","cross_cats_sorted":[],"title_canon_sha256":"008172c94348fc6ce5d75701a2dbedc5d66ee1842f7a0387a3a387d4a267c85c","abstract_canon_sha256":"bb82f4eb976ccaabb88537ff447db6afd544c098c21b8c67d1bc7744860c5701"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:56:43.049206Z","signature_b64":"xOPYUnxsajoatZsZ2ySIs+L2q5m7E8AnetL+pFA9NtgOU9Sd7sawiURlM2Z4hRR7tOs+wEs72opQi2MJEvQLBQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"f111fe87c6c9f668be381133cc8302afe5174c92a4d9e7e22f88926cf1be266e","last_reissued_at":"2026-05-18T01:56:43.048696Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:56:43.048696Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Can we predict the global magnetic topology of a pre-main sequence star from its position in the Hertzsprung-Russell diagram?","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"(2) Toulouse, (3) G\\\"ottingen, 4), (4) DIAS, (5) ESO, (6) Exeter, (7) St Andrews), G. A. J. Hussain (5), J.-F. Donati (2), J. Morin (3, L. A. Hillenbrand (1), M. Jardine (7) ((1) Caltech, N. J. Mayne (6), S. G. Gregory (1)","submitted_at":"2012-06-22T19:53:59Z","abstract_excerpt":"ZDI studies have shown that the magnetic fields of T Tauri stars can be significantly more complex than a simple dipole and can vary markedly between sources. We collect and summarize the magnetic field topology information obtained to date and present Hertzsprung-Russell (HR) diagrams for the stars in the sample. Intriguingly, the large scale field topology of a given pre-main sequence (PMS) star is strongly dependent upon the stellar internal structure, with the strength of the dipole component of its multipolar magnetic field decaying rapidly with the development of a radiative core. Using "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1206.5238","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":""},"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":"1206.5238","created_at":"2026-05-18T01:56:43.048771+00:00"},{"alias_kind":"arxiv_version","alias_value":"1206.5238v1","created_at":"2026-05-18T01:56:43.048771+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1206.5238","created_at":"2026-05-18T01:56:43.048771+00:00"},{"alias_kind":"pith_short_12","alias_value":"6EI75B6GZH3G","created_at":"2026-05-18T12:26:56.085431+00:00"},{"alias_kind":"pith_short_16","alias_value":"6EI75B6GZH3GRPRY","created_at":"2026-05-18T12:26:56.085431+00:00"},{"alias_kind":"pith_short_8","alias_value":"6EI75B6G","created_at":"2026-05-18T12:26:56.085431+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2605.13189","citing_title":"The Accretion Process on Protostars","ref_index":72,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/6EI75B6GZH3GRPRYCEZ4ZAYCV7","json":"https://pith.science/pith/6EI75B6GZH3GRPRYCEZ4ZAYCV7.json","graph_json":"https://pith.science/api/pith-number/6EI75B6GZH3GRPRYCEZ4ZAYCV7/graph.json","events_json":"https://pith.science/api/pith-number/6EI75B6GZH3GRPRYCEZ4ZAYCV7/events.json","paper":"https://pith.science/paper/6EI75B6G"},"agent_actions":{"view_html":"https://pith.science/pith/6EI75B6GZH3GRPRYCEZ4ZAYCV7","download_json":"https://pith.science/pith/6EI75B6GZH3GRPRYCEZ4ZAYCV7.json","view_paper":"https://pith.science/paper/6EI75B6G","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1206.5238&json=true","fetch_graph":"https://pith.science/api/pith-number/6EI75B6GZH3GRPRYCEZ4ZAYCV7/graph.json","fetch_events":"https://pith.science/api/pith-number/6EI75B6GZH3GRPRYCEZ4ZAYCV7/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/6EI75B6GZH3GRPRYCEZ4ZAYCV7/action/timestamp_anchor","attest_storage":"https://pith.science/pith/6EI75B6GZH3GRPRYCEZ4ZAYCV7/action/storage_attestation","attest_author":"https://pith.science/pith/6EI75B6GZH3GRPRYCEZ4ZAYCV7/action/author_attestation","sign_citation":"https://pith.science/pith/6EI75B6GZH3GRPRYCEZ4ZAYCV7/action/citation_signature","submit_replication":"https://pith.science/pith/6EI75B6GZH3GRPRYCEZ4ZAYCV7/action/replication_record"}},"created_at":"2026-05-18T01:56:43.048771+00:00","updated_at":"2026-05-18T01:56:43.048771+00:00"}