{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2010:OM57XMSTYOWVY64W5DJ3YN5YZN","short_pith_number":"pith:OM57XMST","schema_version":"1.0","canonical_sha256":"733bfbb253c3ad5c7b96e8d3bc37b8cb43bdd0b0ef630b225db42c8f75a8af2d","source":{"kind":"arxiv","id":"1011.3826","version":1},"attestation_state":"computed","paper":{"title":"Empirical Constraints on Turbulence in Protoplanetary Accretion Disks","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.EP"],"primary_cat":"astro-ph.SR","authors_text":"A. Meredith Hughes, Chunhua Qi, David J. Wilner, Michiel R. Hogerheijde, Sean M. Andrews","submitted_at":"2010-11-16T21:07:25Z","abstract_excerpt":"We present arcsecond-scale Submillimeter Array observations of the CO(3-2) line emission from the disks around the young stars HD 163296 and TW Hya at a spectral resolution of 44 m/s. These observations probe below the ~100 m/s turbulent linewidth inferred from lower-resolution observations, and allow us to place constraints on the turbulent linewidth in the disk atmospheres. We reproduce the observed CO(3-2) emission using two physical models of disk structure: (1) a power-law temperature distribution with a tapered density distribution following a simple functional form for an evolving accre"},"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":"1011.3826","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2010-11-16T21:07:25Z","cross_cats_sorted":["astro-ph.EP"],"title_canon_sha256":"aca9b8cd489afde7c143ab50630496842d49f1deac0155db9f548a07a59e17c8","abstract_canon_sha256":"ac05643cf1911f7efff493763f1ef487c0be83af5c73c031cc71bc40aafc4dc6"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:04:44.842820Z","signature_b64":"bEbPiVVvfzDKNUCtMINvKxRzdpoAZj6wWhkIivxmrRUF2aPi/Xvqz9/ZtMbzl8ay++SC5D6C/jmrHnMWBxZyDg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"733bfbb253c3ad5c7b96e8d3bc37b8cb43bdd0b0ef630b225db42c8f75a8af2d","last_reissued_at":"2026-05-18T02:04:44.842185Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:04:44.842185Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Empirical Constraints on Turbulence in Protoplanetary Accretion Disks","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.EP"],"primary_cat":"astro-ph.SR","authors_text":"A. Meredith Hughes, Chunhua Qi, David J. Wilner, Michiel R. Hogerheijde, Sean M. Andrews","submitted_at":"2010-11-16T21:07:25Z","abstract_excerpt":"We present arcsecond-scale Submillimeter Array observations of the CO(3-2) line emission from the disks around the young stars HD 163296 and TW Hya at a spectral resolution of 44 m/s. These observations probe below the ~100 m/s turbulent linewidth inferred from lower-resolution observations, and allow us to place constraints on the turbulent linewidth in the disk atmospheres. We reproduce the observed CO(3-2) emission using two physical models of disk structure: (1) a power-law temperature distribution with a tapered density distribution following a simple functional form for an evolving accre"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1011.3826","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":"1011.3826","created_at":"2026-05-18T02:04:44.842306+00:00"},{"alias_kind":"arxiv_version","alias_value":"1011.3826v1","created_at":"2026-05-18T02:04:44.842306+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1011.3826","created_at":"2026-05-18T02:04:44.842306+00:00"},{"alias_kind":"pith_short_12","alias_value":"OM57XMSTYOWV","created_at":"2026-05-18T12:26:12.377268+00:00"},{"alias_kind":"pith_short_16","alias_value":"OM57XMSTYOWVY64W","created_at":"2026-05-18T12:26:12.377268+00:00"},{"alias_kind":"pith_short_8","alias_value":"OM57XMST","created_at":"2026-05-18T12:26:12.377268+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":0,"internal_anchor_count":0,"sample":[]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/OM57XMSTYOWVY64W5DJ3YN5YZN","json":"https://pith.science/pith/OM57XMSTYOWVY64W5DJ3YN5YZN.json","graph_json":"https://pith.science/api/pith-number/OM57XMSTYOWVY64W5DJ3YN5YZN/graph.json","events_json":"https://pith.science/api/pith-number/OM57XMSTYOWVY64W5DJ3YN5YZN/events.json","paper":"https://pith.science/paper/OM57XMST"},"agent_actions":{"view_html":"https://pith.science/pith/OM57XMSTYOWVY64W5DJ3YN5YZN","download_json":"https://pith.science/pith/OM57XMSTYOWVY64W5DJ3YN5YZN.json","view_paper":"https://pith.science/paper/OM57XMST","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1011.3826&json=true","fetch_graph":"https://pith.science/api/pith-number/OM57XMSTYOWVY64W5DJ3YN5YZN/graph.json","fetch_events":"https://pith.science/api/pith-number/OM57XMSTYOWVY64W5DJ3YN5YZN/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/OM57XMSTYOWVY64W5DJ3YN5YZN/action/timestamp_anchor","attest_storage":"https://pith.science/pith/OM57XMSTYOWVY64W5DJ3YN5YZN/action/storage_attestation","attest_author":"https://pith.science/pith/OM57XMSTYOWVY64W5DJ3YN5YZN/action/author_attestation","sign_citation":"https://pith.science/pith/OM57XMSTYOWVY64W5DJ3YN5YZN/action/citation_signature","submit_replication":"https://pith.science/pith/OM57XMSTYOWVY64W5DJ3YN5YZN/action/replication_record"}},"created_at":"2026-05-18T02:04:44.842306+00:00","updated_at":"2026-05-18T02:04:44.842306+00:00"}