{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2016:6XLYYA7447OL32H5XPZHXAP7H3","short_pith_number":"pith:6XLYYA74","schema_version":"1.0","canonical_sha256":"f5d78c03fce7dcbde8fdbbf27b81ff3ee98e8cebc88ac1504427c5fbd64fc2cf","source":{"kind":"arxiv","id":"1603.04022","version":4},"attestation_state":"computed","paper":{"title":"The mineral clouds on HD 209458b and HD189733b","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.SR","physics.ao-ph","physics.flu-dyn"],"primary_cat":"astro-ph.EP","authors_text":"1), 2 - NYU Abu Dhabi, 3 - University of Exeter, 4 - Brooklyn College New York, 5 - UK Met Office), A.A. Unger (1), Ch. Helling (1), C. Smith (5) (1 - University of St Andrews, D. Acreman (5), D. S. Amundsen (3), G. Lee (1), I. Dobbs-Dixon (2), J. Khaimova (4, J. Manners (3), N. Mayne (3)","submitted_at":"2016-03-13T12:35:41Z","abstract_excerpt":"3D atmosphere model results are used to comparatively study the kinetic, non-equilibrium cloud formation in the atmospheres of two example planets guided by the giant gas planets HD209458b and HD189733b. Rather independently of hydrodynamic model differences, our cloud modelling suggests that both planets are covered in mineral clouds throughout the entire modelling domain. Both planets harbour chemically complex clouds that are made of mineral particles that have a height-dependent material composition and size. The remaining gas-phase element abundances strongly effects the molecular abundan"},"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":"1603.04022","kind":"arxiv","version":4},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.EP","submitted_at":"2016-03-13T12:35:41Z","cross_cats_sorted":["astro-ph.SR","physics.ao-ph","physics.flu-dyn"],"title_canon_sha256":"d13f9d9f9aab39a50d9c20f68f9dcea4b2aae0b314cf2318145b35d2f56a602d","abstract_canon_sha256":"daae845efc32c95a47c95815a2247aef5b0f815122dd995c8863e44efa09fadb"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:12:48.754629Z","signature_b64":"UGC1JLa8qsvOLVOIPRkzn2J/d3nWVpJlDUgLXe/5OQYhne6MIplVcApdDRPLmVdGe2j/pMoq1VWDe4T2r3bjAw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"f5d78c03fce7dcbde8fdbbf27b81ff3ee98e8cebc88ac1504427c5fbd64fc2cf","last_reissued_at":"2026-05-18T01:12:48.754243Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:12:48.754243Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The mineral clouds on HD 209458b and HD189733b","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.SR","physics.ao-ph","physics.flu-dyn"],"primary_cat":"astro-ph.EP","authors_text":"1), 2 - NYU Abu Dhabi, 3 - University of Exeter, 4 - Brooklyn College New York, 5 - UK Met Office), A.A. Unger (1), Ch. Helling (1), C. Smith (5) (1 - University of St Andrews, D. Acreman (5), D. S. Amundsen (3), G. Lee (1), I. Dobbs-Dixon (2), J. Khaimova (4, J. Manners (3), N. Mayne (3)","submitted_at":"2016-03-13T12:35:41Z","abstract_excerpt":"3D atmosphere model results are used to comparatively study the kinetic, non-equilibrium cloud formation in the atmospheres of two example planets guided by the giant gas planets HD209458b and HD189733b. Rather independently of hydrodynamic model differences, our cloud modelling suggests that both planets are covered in mineral clouds throughout the entire modelling domain. Both planets harbour chemically complex clouds that are made of mineral particles that have a height-dependent material composition and size. The remaining gas-phase element abundances strongly effects the molecular abundan"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1603.04022","kind":"arxiv","version":4},"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":"1603.04022","created_at":"2026-05-18T01:12:48.754308+00:00"},{"alias_kind":"arxiv_version","alias_value":"1603.04022v4","created_at":"2026-05-18T01:12:48.754308+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1603.04022","created_at":"2026-05-18T01:12:48.754308+00:00"},{"alias_kind":"pith_short_12","alias_value":"6XLYYA7447OL","created_at":"2026-05-18T12:30:04.600751+00:00"},{"alias_kind":"pith_short_16","alias_value":"6XLYYA7447OL32H5","created_at":"2026-05-18T12:30:04.600751+00:00"},{"alias_kind":"pith_short_8","alias_value":"6XLYYA74","created_at":"2026-05-18T12:30:04.600751+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/6XLYYA7447OL32H5XPZHXAP7H3","json":"https://pith.science/pith/6XLYYA7447OL32H5XPZHXAP7H3.json","graph_json":"https://pith.science/api/pith-number/6XLYYA7447OL32H5XPZHXAP7H3/graph.json","events_json":"https://pith.science/api/pith-number/6XLYYA7447OL32H5XPZHXAP7H3/events.json","paper":"https://pith.science/paper/6XLYYA74"},"agent_actions":{"view_html":"https://pith.science/pith/6XLYYA7447OL32H5XPZHXAP7H3","download_json":"https://pith.science/pith/6XLYYA7447OL32H5XPZHXAP7H3.json","view_paper":"https://pith.science/paper/6XLYYA74","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1603.04022&json=true","fetch_graph":"https://pith.science/api/pith-number/6XLYYA7447OL32H5XPZHXAP7H3/graph.json","fetch_events":"https://pith.science/api/pith-number/6XLYYA7447OL32H5XPZHXAP7H3/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/6XLYYA7447OL32H5XPZHXAP7H3/action/timestamp_anchor","attest_storage":"https://pith.science/pith/6XLYYA7447OL32H5XPZHXAP7H3/action/storage_attestation","attest_author":"https://pith.science/pith/6XLYYA7447OL32H5XPZHXAP7H3/action/author_attestation","sign_citation":"https://pith.science/pith/6XLYYA7447OL32H5XPZHXAP7H3/action/citation_signature","submit_replication":"https://pith.science/pith/6XLYYA7447OL32H5XPZHXAP7H3/action/replication_record"}},"created_at":"2026-05-18T01:12:48.754308+00:00","updated_at":"2026-05-18T01:12:48.754308+00:00"}