{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2010:E6YP3LNK45UHSM2YT7IJ7OW7G4","short_pith_number":"pith:E6YP3LNK","schema_version":"1.0","canonical_sha256":"27b0fdadaae7687933589fd09fbadf3719a6edac73f96fb8d81d43d36de4e868","source":{"kind":"arxiv","id":"1011.4168","version":1},"attestation_state":"computed","paper":{"title":"On the volatile enrichments and heavy element content in HD 189733b","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.IM"],"primary_cat":"astro-ph.EP","authors_text":"C. Griffith, D. Cordier, J.B.A. Mitchell, J.I. Lunine, J.-M. Petit, K. Zahnle, L. Biennier, M. Devel, M.S. Marley, N. Iro, O. Mousis, R. Georges, S. Picaud, T.V. Johnson, U. Marboeuf, V. Boudon","submitted_at":"2010-11-18T10:56:14Z","abstract_excerpt":"Favored theories of giant planet formation center around two main paradigms, namely the core accretion model and the gravitational instability model. These two formation scenarios support the hypothesis that the giant planet metallicities should be higher or equal to that of the parent star. Meanwhile, spectra of the transiting hot Jupiter HD189733b suggest that carbon and oxygen abundances range from depleted to enriched with respect to the star. Here, using a model describing the formation sequence and composition of planetesimals in the protoplanetary disk, we determine the range of volatil"},"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":"1011.4168","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.EP","submitted_at":"2010-11-18T10:56:14Z","cross_cats_sorted":["astro-ph.IM"],"title_canon_sha256":"bda1528be107ff7db2fd7703dfcdafbc6bf444100e07db427edb2224b5d280a4","abstract_canon_sha256":"06c7c34502b8d9b8f02752087cb81a1020451a242402006de0f59b33b5051ff1"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:04:44.047081Z","signature_b64":"OM9S0An5rkUiTWbBK66pgSiicl4g6iYvHuPPTmZxqEK4DrRgZ+P5DRU5KZMO1tORlPTKiha9KLFaIOsdgdroCw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"27b0fdadaae7687933589fd09fbadf3719a6edac73f96fb8d81d43d36de4e868","last_reissued_at":"2026-05-18T02:04:44.046227Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:04:44.046227Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"On the volatile enrichments and heavy element content in HD 189733b","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.IM"],"primary_cat":"astro-ph.EP","authors_text":"C. Griffith, D. Cordier, J.B.A. Mitchell, J.I. Lunine, J.-M. Petit, K. Zahnle, L. Biennier, M. Devel, M.S. Marley, N. Iro, O. Mousis, R. Georges, S. Picaud, T.V. Johnson, U. Marboeuf, V. Boudon","submitted_at":"2010-11-18T10:56:14Z","abstract_excerpt":"Favored theories of giant planet formation center around two main paradigms, namely the core accretion model and the gravitational instability model. These two formation scenarios support the hypothesis that the giant planet metallicities should be higher or equal to that of the parent star. Meanwhile, spectra of the transiting hot Jupiter HD189733b suggest that carbon and oxygen abundances range from depleted to enriched with respect to the star. Here, using a model describing the formation sequence and composition of planetesimals in the protoplanetary disk, we determine the range of volatil"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1011.4168","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":"1011.4168","created_at":"2026-05-18T02:04:44.046376+00:00"},{"alias_kind":"arxiv_version","alias_value":"1011.4168v1","created_at":"2026-05-18T02:04:44.046376+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1011.4168","created_at":"2026-05-18T02:04:44.046376+00:00"},{"alias_kind":"pith_short_12","alias_value":"E6YP3LNK45UH","created_at":"2026-05-18T12:26:06.534383+00:00"},{"alias_kind":"pith_short_16","alias_value":"E6YP3LNK45UHSM2Y","created_at":"2026-05-18T12:26:06.534383+00:00"},{"alias_kind":"pith_short_8","alias_value":"E6YP3LNK","created_at":"2026-05-18T12:26:06.534383+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/E6YP3LNK45UHSM2YT7IJ7OW7G4","json":"https://pith.science/pith/E6YP3LNK45UHSM2YT7IJ7OW7G4.json","graph_json":"https://pith.science/api/pith-number/E6YP3LNK45UHSM2YT7IJ7OW7G4/graph.json","events_json":"https://pith.science/api/pith-number/E6YP3LNK45UHSM2YT7IJ7OW7G4/events.json","paper":"https://pith.science/paper/E6YP3LNK"},"agent_actions":{"view_html":"https://pith.science/pith/E6YP3LNK45UHSM2YT7IJ7OW7G4","download_json":"https://pith.science/pith/E6YP3LNK45UHSM2YT7IJ7OW7G4.json","view_paper":"https://pith.science/paper/E6YP3LNK","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1011.4168&json=true","fetch_graph":"https://pith.science/api/pith-number/E6YP3LNK45UHSM2YT7IJ7OW7G4/graph.json","fetch_events":"https://pith.science/api/pith-number/E6YP3LNK45UHSM2YT7IJ7OW7G4/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/E6YP3LNK45UHSM2YT7IJ7OW7G4/action/timestamp_anchor","attest_storage":"https://pith.science/pith/E6YP3LNK45UHSM2YT7IJ7OW7G4/action/storage_attestation","attest_author":"https://pith.science/pith/E6YP3LNK45UHSM2YT7IJ7OW7G4/action/author_attestation","sign_citation":"https://pith.science/pith/E6YP3LNK45UHSM2YT7IJ7OW7G4/action/citation_signature","submit_replication":"https://pith.science/pith/E6YP3LNK45UHSM2YT7IJ7OW7G4/action/replication_record"}},"created_at":"2026-05-18T02:04:44.046376+00:00","updated_at":"2026-05-18T02:04:44.046376+00:00"}