{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2017:PPPWEF65KISIHMAYWVTHF7DWXU","short_pith_number":"pith:PPPWEF65","schema_version":"1.0","canonical_sha256":"7bdf6217dd522483b018b56672fc76bd0b0f0b5d4c8d312b4e70918f242a2d03","source":{"kind":"arxiv","id":"1711.01153","version":1},"attestation_state":"computed","paper":{"title":"The shock-heated atmosphere of an asymptotic giant branch star resolved by ALMA","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"Aki Takigawa, Boy Lankhaar, Daniel Tafoya, Eamon O'Gorman, Elizabeth Humphreys, Elvire De Beck, Hans Olofsson, Matthias Maercker, Sofia Ramstedt, Theo Khouri, Wouter Vlemmings","submitted_at":"2017-11-03T13:30:00Z","abstract_excerpt":"Our current understanding of the chemistry and mass-loss processes in solar-like stars at the end of their evolution depends critically on the description of convection, pulsations and shocks in the extended stellar atmosphere. Three-dimensional hydrodynamical stellar atmosphere models provide observational predictions, but so far the resolution to constrain the complex temperature and velocity structures seen in the models has been lacking. Here we present submillimeter continuum and line observations that resolve the atmosphere of the asymptotic giant branch star W Hya. We show that hot gas "},"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":"1711.01153","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2017-11-03T13:30:00Z","cross_cats_sorted":[],"title_canon_sha256":"75d72263344c51f8813b2917264a11676653f0306a2003ed6a0a748b523510c7","abstract_canon_sha256":"d8e4fbd0403e2a322a0f0e91fcf831d0d71f0ab0f26384d6228f995682c111f4"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:31:23.280057Z","signature_b64":"psqk3PuxkEmu2P0Yo9SgB1tsCrLhJ/VLnuyn3Ki5N6hVWG4ANKqjs6VwvZTzcVhQ9RIJsuAFDydxCXfBmTBSDw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"7bdf6217dd522483b018b56672fc76bd0b0f0b5d4c8d312b4e70918f242a2d03","last_reissued_at":"2026-05-18T00:31:23.279391Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:31:23.279391Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The shock-heated atmosphere of an asymptotic giant branch star resolved by ALMA","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"Aki Takigawa, Boy Lankhaar, Daniel Tafoya, Eamon O'Gorman, Elizabeth Humphreys, Elvire De Beck, Hans Olofsson, Matthias Maercker, Sofia Ramstedt, Theo Khouri, Wouter Vlemmings","submitted_at":"2017-11-03T13:30:00Z","abstract_excerpt":"Our current understanding of the chemistry and mass-loss processes in solar-like stars at the end of their evolution depends critically on the description of convection, pulsations and shocks in the extended stellar atmosphere. Three-dimensional hydrodynamical stellar atmosphere models provide observational predictions, but so far the resolution to constrain the complex temperature and velocity structures seen in the models has been lacking. Here we present submillimeter continuum and line observations that resolve the atmosphere of the asymptotic giant branch star W Hya. We show that hot gas "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1711.01153","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":"1711.01153","created_at":"2026-05-18T00:31:23.279476+00:00"},{"alias_kind":"arxiv_version","alias_value":"1711.01153v1","created_at":"2026-05-18T00:31:23.279476+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1711.01153","created_at":"2026-05-18T00:31:23.279476+00:00"},{"alias_kind":"pith_short_12","alias_value":"PPPWEF65KISI","created_at":"2026-05-18T12:31:37.085036+00:00"},{"alias_kind":"pith_short_16","alias_value":"PPPWEF65KISIHMAY","created_at":"2026-05-18T12:31:37.085036+00:00"},{"alias_kind":"pith_short_8","alias_value":"PPPWEF65","created_at":"2026-05-18T12:31:37.085036+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/PPPWEF65KISIHMAYWVTHF7DWXU","json":"https://pith.science/pith/PPPWEF65KISIHMAYWVTHF7DWXU.json","graph_json":"https://pith.science/api/pith-number/PPPWEF65KISIHMAYWVTHF7DWXU/graph.json","events_json":"https://pith.science/api/pith-number/PPPWEF65KISIHMAYWVTHF7DWXU/events.json","paper":"https://pith.science/paper/PPPWEF65"},"agent_actions":{"view_html":"https://pith.science/pith/PPPWEF65KISIHMAYWVTHF7DWXU","download_json":"https://pith.science/pith/PPPWEF65KISIHMAYWVTHF7DWXU.json","view_paper":"https://pith.science/paper/PPPWEF65","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1711.01153&json=true","fetch_graph":"https://pith.science/api/pith-number/PPPWEF65KISIHMAYWVTHF7DWXU/graph.json","fetch_events":"https://pith.science/api/pith-number/PPPWEF65KISIHMAYWVTHF7DWXU/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/PPPWEF65KISIHMAYWVTHF7DWXU/action/timestamp_anchor","attest_storage":"https://pith.science/pith/PPPWEF65KISIHMAYWVTHF7DWXU/action/storage_attestation","attest_author":"https://pith.science/pith/PPPWEF65KISIHMAYWVTHF7DWXU/action/author_attestation","sign_citation":"https://pith.science/pith/PPPWEF65KISIHMAYWVTHF7DWXU/action/citation_signature","submit_replication":"https://pith.science/pith/PPPWEF65KISIHMAYWVTHF7DWXU/action/replication_record"}},"created_at":"2026-05-18T00:31:23.279476+00:00","updated_at":"2026-05-18T00:31:23.279476+00:00"}