{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2009:PVGL2TPHUSJ3RJBKW5SKNRT2SN","short_pith_number":"pith:PVGL2TPH","schema_version":"1.0","canonical_sha256":"7d4cbd4de7a493b8a42ab764a6c67a937b53d0ff4f094fa3c1fc18edfec1ec58","source":{"kind":"arxiv","id":"0909.0975","version":1},"attestation_state":"computed","paper":{"title":"Radiative transfer models of mid-infrared H2O lines in the Planet-forming Region of Circumstellar Disks","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.EP","authors_text":"C.P. Dullemond, D.R. Poelman, G.A. Blake, K.M. Pontoppidan, R. Meijerink","submitted_at":"2009-09-04T22:46:50Z","abstract_excerpt":"The study of warm molecular gas in the inner regions of protoplanetary disks is of key importance for the study of planet formation and especially for the transport of H2O and organic molecules to the surfaces of rocky planets/satellites. Recent Spitzer observations have shown that the mid-infrared spectra of protoplanetary disks are covered in emission lines due to water and other molecules. Here, we present a non-LTE 2D radiative transfer model of water lines in the 10-36 mum range that can be used to constrain the abundance structure of water vapor, given an observed spectrum, and show that"},"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":"0909.0975","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.EP","submitted_at":"2009-09-04T22:46:50Z","cross_cats_sorted":[],"title_canon_sha256":"f13669687250f9f929e0663bcf4637329b6d4d73bff32887c924037c050da94a","abstract_canon_sha256":"01a09032d9bec1c6cead55ef8345cc63f4b57958b00819a9ed0b18eb5c4c2ecd"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:34:30.997089Z","signature_b64":"MRlpz5JWmr4d8O8+OdGYNsYUz+R+DQb0B2Ulvmih6Rq2uZ7zUC1OMb5756jOEkcD5+WRccdKec9oVawXfoo9Cg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"7d4cbd4de7a493b8a42ab764a6c67a937b53d0ff4f094fa3c1fc18edfec1ec58","last_reissued_at":"2026-05-18T02:34:30.996710Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:34:30.996710Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Radiative transfer models of mid-infrared H2O lines in the Planet-forming Region of Circumstellar Disks","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.EP","authors_text":"C.P. Dullemond, D.R. Poelman, G.A. Blake, K.M. Pontoppidan, R. Meijerink","submitted_at":"2009-09-04T22:46:50Z","abstract_excerpt":"The study of warm molecular gas in the inner regions of protoplanetary disks is of key importance for the study of planet formation and especially for the transport of H2O and organic molecules to the surfaces of rocky planets/satellites. Recent Spitzer observations have shown that the mid-infrared spectra of protoplanetary disks are covered in emission lines due to water and other molecules. Here, we present a non-LTE 2D radiative transfer model of water lines in the 10-36 mum range that can be used to constrain the abundance structure of water vapor, given an observed spectrum, and show that"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"0909.0975","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":"0909.0975","created_at":"2026-05-18T02:34:30.996767+00:00"},{"alias_kind":"arxiv_version","alias_value":"0909.0975v1","created_at":"2026-05-18T02:34:30.996767+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.0909.0975","created_at":"2026-05-18T02:34:30.996767+00:00"},{"alias_kind":"pith_short_12","alias_value":"PVGL2TPHUSJ3","created_at":"2026-05-18T12:26:01.383474+00:00"},{"alias_kind":"pith_short_16","alias_value":"PVGL2TPHUSJ3RJBK","created_at":"2026-05-18T12:26:01.383474+00:00"},{"alias_kind":"pith_short_8","alias_value":"PVGL2TPH","created_at":"2026-05-18T12:26:01.383474+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":2,"sample":[{"citing_arxiv_id":"2605.18062","citing_title":"Chemistry and IR emission of acetylene in planet-forming regions of T Tauri disks. Impact of elemental abundances and dust properties","ref_index":163,"is_internal_anchor":true},{"citing_arxiv_id":"2605.18062","citing_title":"Chemistry and IR emission of acetylene in planet-forming regions of T Tauri disks. Impact of elemental abundances and dust properties","ref_index":163,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/PVGL2TPHUSJ3RJBKW5SKNRT2SN","json":"https://pith.science/pith/PVGL2TPHUSJ3RJBKW5SKNRT2SN.json","graph_json":"https://pith.science/api/pith-number/PVGL2TPHUSJ3RJBKW5SKNRT2SN/graph.json","events_json":"https://pith.science/api/pith-number/PVGL2TPHUSJ3RJBKW5SKNRT2SN/events.json","paper":"https://pith.science/paper/PVGL2TPH"},"agent_actions":{"view_html":"https://pith.science/pith/PVGL2TPHUSJ3RJBKW5SKNRT2SN","download_json":"https://pith.science/pith/PVGL2TPHUSJ3RJBKW5SKNRT2SN.json","view_paper":"https://pith.science/paper/PVGL2TPH","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=0909.0975&json=true","fetch_graph":"https://pith.science/api/pith-number/PVGL2TPHUSJ3RJBKW5SKNRT2SN/graph.json","fetch_events":"https://pith.science/api/pith-number/PVGL2TPHUSJ3RJBKW5SKNRT2SN/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/PVGL2TPHUSJ3RJBKW5SKNRT2SN/action/timestamp_anchor","attest_storage":"https://pith.science/pith/PVGL2TPHUSJ3RJBKW5SKNRT2SN/action/storage_attestation","attest_author":"https://pith.science/pith/PVGL2TPHUSJ3RJBKW5SKNRT2SN/action/author_attestation","sign_citation":"https://pith.science/pith/PVGL2TPHUSJ3RJBKW5SKNRT2SN/action/citation_signature","submit_replication":"https://pith.science/pith/PVGL2TPHUSJ3RJBKW5SKNRT2SN/action/replication_record"}},"created_at":"2026-05-18T02:34:30.996767+00:00","updated_at":"2026-05-18T02:34:30.996767+00:00"}