{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2023:HDMCYXFQH5UT2APWUQZDJU3BHA","short_pith_number":"pith:HDMCYXFQ","schema_version":"1.0","canonical_sha256":"38d82c5cb03f693d01f6a43234d361381f78fc9fd3bc0fad9a6465ae81f429c1","source":{"kind":"arxiv","id":"2306.06103","version":2},"attestation_state":"computed","paper":{"title":"Beyond Diffusion: A Generalized Mean-Field Theory of Turbulent Dust Transport in Protoplanetary Disks","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.EP","authors_text":"Fabian Binkert","submitted_at":"2023-06-09T17:59:54Z","abstract_excerpt":"Turbulence in protoplanetary disks, when present, plays a critical role in transporting dust particles embedded in the gaseous disk component. When using a field description of dust dynamics, a diffusion approach is traditionally used to model this turbulent dust transport. However, it has been shown that classical turbulent diffusion models are not fully self-consistent. Several shortcomings exist, including the ambiguous nature of the diffused quantity and the nonconservation of angular momentum. Orbital effects are also neglected without an explicit prescription. In response to these incons"},"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":"2306.06103","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.EP","submitted_at":"2023-06-09T17:59:54Z","cross_cats_sorted":[],"title_canon_sha256":"1678afbf343430514d5437381c1a91357036d3a9ea00ced50dd0206243499221","abstract_canon_sha256":"b5ca1590ef3abdae972ea3a317f8730202c6b895e7a99ed7016527c403182b08"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T06:40:34.682613Z","signature_b64":"nHYVF2KqmoTfMafY8pifjkNXSgufW8ssmZu0oLFet/f9sGl3O3COdmlMcugS9Ud8/Q+DhZFD9V4ThLwzL5QmDQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"38d82c5cb03f693d01f6a43234d361381f78fc9fd3bc0fad9a6465ae81f429c1","last_reissued_at":"2026-07-05T06:40:34.682102Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T06:40:34.682102Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Beyond Diffusion: A Generalized Mean-Field Theory of Turbulent Dust Transport in Protoplanetary Disks","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.EP","authors_text":"Fabian Binkert","submitted_at":"2023-06-09T17:59:54Z","abstract_excerpt":"Turbulence in protoplanetary disks, when present, plays a critical role in transporting dust particles embedded in the gaseous disk component. When using a field description of dust dynamics, a diffusion approach is traditionally used to model this turbulent dust transport. However, it has been shown that classical turbulent diffusion models are not fully self-consistent. Several shortcomings exist, including the ambiguous nature of the diffused quantity and the nonconservation of angular momentum. Orbital effects are also neglected without an explicit prescription. In response to these incons"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2306.06103","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/2306.06103/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":"2306.06103","created_at":"2026-07-05T06:40:34.682161+00:00"},{"alias_kind":"arxiv_version","alias_value":"2306.06103v2","created_at":"2026-07-05T06:40:34.682161+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2306.06103","created_at":"2026-07-05T06:40:34.682161+00:00"},{"alias_kind":"pith_short_12","alias_value":"HDMCYXFQH5UT","created_at":"2026-07-05T06:40:34.682161+00:00"},{"alias_kind":"pith_short_16","alias_value":"HDMCYXFQH5UT2APW","created_at":"2026-07-05T06:40:34.682161+00:00"},{"alias_kind":"pith_short_8","alias_value":"HDMCYXFQ","created_at":"2026-07-05T06:40:34.682161+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2411.12462","citing_title":"Developing a Non-Newtonian Fluid Model for Dust, for Application to Astrophysical Flows","ref_index":11,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/HDMCYXFQH5UT2APWUQZDJU3BHA","json":"https://pith.science/pith/HDMCYXFQH5UT2APWUQZDJU3BHA.json","graph_json":"https://pith.science/api/pith-number/HDMCYXFQH5UT2APWUQZDJU3BHA/graph.json","events_json":"https://pith.science/api/pith-number/HDMCYXFQH5UT2APWUQZDJU3BHA/events.json","paper":"https://pith.science/paper/HDMCYXFQ"},"agent_actions":{"view_html":"https://pith.science/pith/HDMCYXFQH5UT2APWUQZDJU3BHA","download_json":"https://pith.science/pith/HDMCYXFQH5UT2APWUQZDJU3BHA.json","view_paper":"https://pith.science/paper/HDMCYXFQ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2306.06103&json=true","fetch_graph":"https://pith.science/api/pith-number/HDMCYXFQH5UT2APWUQZDJU3BHA/graph.json","fetch_events":"https://pith.science/api/pith-number/HDMCYXFQH5UT2APWUQZDJU3BHA/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/HDMCYXFQH5UT2APWUQZDJU3BHA/action/timestamp_anchor","attest_storage":"https://pith.science/pith/HDMCYXFQH5UT2APWUQZDJU3BHA/action/storage_attestation","attest_author":"https://pith.science/pith/HDMCYXFQH5UT2APWUQZDJU3BHA/action/author_attestation","sign_citation":"https://pith.science/pith/HDMCYXFQH5UT2APWUQZDJU3BHA/action/citation_signature","submit_replication":"https://pith.science/pith/HDMCYXFQH5UT2APWUQZDJU3BHA/action/replication_record"}},"created_at":"2026-07-05T06:40:34.682161+00:00","updated_at":"2026-07-05T06:40:34.682161+00:00"}