{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2022:PDMVTNNGD7AXGYJNMKCS6H7735","short_pith_number":"pith:PDMVTNNG","schema_version":"1.0","canonical_sha256":"78d959b5a61fc173612d62852f1fffdf7eeb800f7b148c757e5161eed1d47115","source":{"kind":"arxiv","id":"2202.08838","version":1},"attestation_state":"computed","paper":{"title":"Helium absorption in exoplanet atmospheres is connected to stellar coronal abundances","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.SR"],"primary_cat":"astro-ph.EP","authors_text":"K. Poppenhaeger","submitted_at":"2022-02-17T18:59:32Z","abstract_excerpt":"Transit observations in the helium triplet around 10830 Angstrom are a successful tool to study exoplanetary atmospheres and their mass loss. Forming those lines requires ionisation and recombination of helium in the exoplanetary atmosphere. This ionisation is caused by stellar photons at extreme ultra-violet (EUV) wavelengths; however, no currently active telescopes can observe this part of the stellar spectrum. The relevant part of the stellar EUV spectrum consists of individual emission lines, many of them being formed by iron at coronal temperatures. The stellar iron abundance in the coron"},"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":"2202.08838","kind":"arxiv","version":1},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.EP","submitted_at":"2022-02-17T18:59:32Z","cross_cats_sorted":["astro-ph.SR"],"title_canon_sha256":"7ebbbcfac656895ceea45e180e36b60b3ed2722b3ea8e7ce4f856c0a5be5181b","abstract_canon_sha256":"96c47e2d8a6c236788db822c742395b17dd189496bac00595d70c06ace8bb930"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T04:04:04.681757Z","signature_b64":"BLeSAlLGQnlnP49Jjj+cnhdzUULo92sQ9/Pp3Gyl02XvTraqy5HqssU3JLcI5u8TehfhCVS5m3Jv4t4evdm1Aw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"78d959b5a61fc173612d62852f1fffdf7eeb800f7b148c757e5161eed1d47115","last_reissued_at":"2026-07-05T04:04:04.681343Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T04:04:04.681343Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Helium absorption in exoplanet atmospheres is connected to stellar coronal abundances","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.SR"],"primary_cat":"astro-ph.EP","authors_text":"K. Poppenhaeger","submitted_at":"2022-02-17T18:59:32Z","abstract_excerpt":"Transit observations in the helium triplet around 10830 Angstrom are a successful tool to study exoplanetary atmospheres and their mass loss. Forming those lines requires ionisation and recombination of helium in the exoplanetary atmosphere. This ionisation is caused by stellar photons at extreme ultra-violet (EUV) wavelengths; however, no currently active telescopes can observe this part of the stellar spectrum. The relevant part of the stellar EUV spectrum consists of individual emission lines, many of them being formed by iron at coronal temperatures. The stellar iron abundance in the coron"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2202.08838","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/2202.08838/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":"2202.08838","created_at":"2026-07-05T04:04:04.681401+00:00"},{"alias_kind":"arxiv_version","alias_value":"2202.08838v1","created_at":"2026-07-05T04:04:04.681401+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2202.08838","created_at":"2026-07-05T04:04:04.681401+00:00"},{"alias_kind":"pith_short_12","alias_value":"PDMVTNNGD7AX","created_at":"2026-07-05T04:04:04.681401+00:00"},{"alias_kind":"pith_short_16","alias_value":"PDMVTNNGD7AXGYJN","created_at":"2026-07-05T04:04:04.681401+00:00"},{"alias_kind":"pith_short_8","alias_value":"PDMVTNNG","created_at":"2026-07-05T04:04:04.681401+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/PDMVTNNGD7AXGYJNMKCS6H7735","json":"https://pith.science/pith/PDMVTNNGD7AXGYJNMKCS6H7735.json","graph_json":"https://pith.science/api/pith-number/PDMVTNNGD7AXGYJNMKCS6H7735/graph.json","events_json":"https://pith.science/api/pith-number/PDMVTNNGD7AXGYJNMKCS6H7735/events.json","paper":"https://pith.science/paper/PDMVTNNG"},"agent_actions":{"view_html":"https://pith.science/pith/PDMVTNNGD7AXGYJNMKCS6H7735","download_json":"https://pith.science/pith/PDMVTNNGD7AXGYJNMKCS6H7735.json","view_paper":"https://pith.science/paper/PDMVTNNG","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2202.08838&json=true","fetch_graph":"https://pith.science/api/pith-number/PDMVTNNGD7AXGYJNMKCS6H7735/graph.json","fetch_events":"https://pith.science/api/pith-number/PDMVTNNGD7AXGYJNMKCS6H7735/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/PDMVTNNGD7AXGYJNMKCS6H7735/action/timestamp_anchor","attest_storage":"https://pith.science/pith/PDMVTNNGD7AXGYJNMKCS6H7735/action/storage_attestation","attest_author":"https://pith.science/pith/PDMVTNNGD7AXGYJNMKCS6H7735/action/author_attestation","sign_citation":"https://pith.science/pith/PDMVTNNGD7AXGYJNMKCS6H7735/action/citation_signature","submit_replication":"https://pith.science/pith/PDMVTNNGD7AXGYJNMKCS6H7735/action/replication_record"}},"created_at":"2026-07-05T04:04:04.681401+00:00","updated_at":"2026-07-05T04:04:04.681401+00:00"}