{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2008:WJUBGFF7UDMPC3YAZGNYPN2ZVF","short_pith_number":"pith:WJUBGFF7","schema_version":"1.0","canonical_sha256":"b2681314bfa0d8f16f00c99b87b759a94d5640139e2303d80376599a4d6993b1","source":{"kind":"arxiv","id":"0803.4315","version":1},"attestation_state":"computed","paper":{"title":"Dust in Brown Dwarfs and Extra-solar Planets I. Chemical composition and spectral appearance of quasi-static cloud layers","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Ch. Helling, P. Woitke, W.-F. Thi","submitted_at":"2008-03-30T12:05:48Z","abstract_excerpt":"We aim at understanding the formation of cloud layers in quasi-static substellar atmospheres. The time-dependent description presented in (Helling & Woitke 2006) is a kinetic model describing nucleation, growth and evaporation. It is extended to treat gravitational settling and is applied to the static-stationary case of substellar model atmospheres. From the solution for the dust moments, we determine the grain size distribution function which, together with the calculated material volume fractions, provides the basis to calculate the opacities of the composite dust grains. The cloud particle"},"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":"0803.4315","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph","submitted_at":"2008-03-30T12:05:48Z","cross_cats_sorted":[],"title_canon_sha256":"1081a4f5608330b58e63e5b64ba9aecbfced365807a6f4bb9c64ae926b782da5","abstract_canon_sha256":"fd8ecb7269f7282907b9b9a30a719ba9259aa5e82158c3441e696389f58342e0"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T17:10:01.465335Z","signature_b64":"5xV3MpK8t/PQisWW70uwhGPw9OIrDL94JYaOs4QearIIb2Eo+RvXKU7iA/rWLg8Qe2kygf77rlO8qcPJ5oRrAg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"b2681314bfa0d8f16f00c99b87b759a94d5640139e2303d80376599a4d6993b1","last_reissued_at":"2026-07-04T17:10:01.464941Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T17:10:01.464941Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Dust in Brown Dwarfs and Extra-solar Planets I. Chemical composition and spectral appearance of quasi-static cloud layers","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Ch. Helling, P. Woitke, W.-F. Thi","submitted_at":"2008-03-30T12:05:48Z","abstract_excerpt":"We aim at understanding the formation of cloud layers in quasi-static substellar atmospheres. The time-dependent description presented in (Helling & Woitke 2006) is a kinetic model describing nucleation, growth and evaporation. It is extended to treat gravitational settling and is applied to the static-stationary case of substellar model atmospheres. From the solution for the dust moments, we determine the grain size distribution function which, together with the calculated material volume fractions, provides the basis to calculate the opacities of the composite dust grains. The cloud particle"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"0803.4315","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/0803.4315/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":"0803.4315","created_at":"2026-07-04T17:10:01.465004+00:00"},{"alias_kind":"arxiv_version","alias_value":"0803.4315v1","created_at":"2026-07-04T17:10:01.465004+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.0803.4315","created_at":"2026-07-04T17:10:01.465004+00:00"},{"alias_kind":"pith_short_12","alias_value":"WJUBGFF7UDMP","created_at":"2026-07-04T17:10:01.465004+00:00"},{"alias_kind":"pith_short_16","alias_value":"WJUBGFF7UDMPC3YA","created_at":"2026-07-04T17:10:01.465004+00:00"},{"alias_kind":"pith_short_8","alias_value":"WJUBGFF7","created_at":"2026-07-04T17:10:01.465004+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2607.09851","citing_title":"Benchmark Brown Dwarf Systems I: Chemical Abundance Analysis of FGK Stars with Wide-Separation Brown Dwarf Companions Using PEPSI","ref_index":243,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/WJUBGFF7UDMPC3YAZGNYPN2ZVF","json":"https://pith.science/pith/WJUBGFF7UDMPC3YAZGNYPN2ZVF.json","graph_json":"https://pith.science/api/pith-number/WJUBGFF7UDMPC3YAZGNYPN2ZVF/graph.json","events_json":"https://pith.science/api/pith-number/WJUBGFF7UDMPC3YAZGNYPN2ZVF/events.json","paper":"https://pith.science/paper/WJUBGFF7"},"agent_actions":{"view_html":"https://pith.science/pith/WJUBGFF7UDMPC3YAZGNYPN2ZVF","download_json":"https://pith.science/pith/WJUBGFF7UDMPC3YAZGNYPN2ZVF.json","view_paper":"https://pith.science/paper/WJUBGFF7","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=0803.4315&json=true","fetch_graph":"https://pith.science/api/pith-number/WJUBGFF7UDMPC3YAZGNYPN2ZVF/graph.json","fetch_events":"https://pith.science/api/pith-number/WJUBGFF7UDMPC3YAZGNYPN2ZVF/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/WJUBGFF7UDMPC3YAZGNYPN2ZVF/action/timestamp_anchor","attest_storage":"https://pith.science/pith/WJUBGFF7UDMPC3YAZGNYPN2ZVF/action/storage_attestation","attest_author":"https://pith.science/pith/WJUBGFF7UDMPC3YAZGNYPN2ZVF/action/author_attestation","sign_citation":"https://pith.science/pith/WJUBGFF7UDMPC3YAZGNYPN2ZVF/action/citation_signature","submit_replication":"https://pith.science/pith/WJUBGFF7UDMPC3YAZGNYPN2ZVF/action/replication_record"}},"created_at":"2026-07-04T17:10:01.465004+00:00","updated_at":"2026-07-04T17:10:01.465004+00:00"}