{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2021:X7SN4O44TCSGICNZZEREOTWJVA","short_pith_number":"pith:X7SN4O44","schema_version":"1.0","canonical_sha256":"bfe4de3b9c98a46409b9c922474ec9a8233dcf11eecd4f950de5e845a8abb374","source":{"kind":"arxiv","id":"2109.08164","version":4},"attestation_state":"computed","paper":{"title":"Theory and Diagnostics of Hot Star Mass Loss","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.GA","astro-ph.HE"],"primary_cat":"astro-ph.SR","authors_text":"Jorick S. Vink (Armagh Observatory, Planetarium)","submitted_at":"2021-09-16T18:00:03Z","abstract_excerpt":"Massive stars have strong stellar winds that direct their evolution through the upper Hertzsprung-Russell diagram and determine the black hole mass function. Secondly, wind strength dictates the atmospheric structure that sets the ionising flux. Thirdly, the wind directly intervenes with the stellar envelope structure, which is decisive for both single star and binary evolution, affecting predictions for gravitational wave events. Key findings of current hot-star research include:\n  * The traditional line-driven wind theory is being updated with Monte Carlo and co-moving frame computations, re"},"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":"2109.08164","kind":"arxiv","version":4},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.SR","submitted_at":"2021-09-16T18:00:03Z","cross_cats_sorted":["astro-ph.GA","astro-ph.HE"],"title_canon_sha256":"6f038b42940a6db1c5fe0598025aaf4897bd6978e605c81aed9865eb544a6976","abstract_canon_sha256":"da925fafd40942e4f73eea657de992d87c11b056e12cf9a8b8be25279df6d460"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T04:30:52.701832Z","signature_b64":"/awEo5bWmuEnF/1iPbJY8grq9SSwmD2KFBmnRvi+RHkvnT81HUB4/pkw+2SAcLwH3Mdz4YAb+9LQo0v5zlP6Dg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"bfe4de3b9c98a46409b9c922474ec9a8233dcf11eecd4f950de5e845a8abb374","last_reissued_at":"2026-07-05T04:30:52.701300Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T04:30:52.701300Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Theory and Diagnostics of Hot Star Mass Loss","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.GA","astro-ph.HE"],"primary_cat":"astro-ph.SR","authors_text":"Jorick S. Vink (Armagh Observatory, Planetarium)","submitted_at":"2021-09-16T18:00:03Z","abstract_excerpt":"Massive stars have strong stellar winds that direct their evolution through the upper Hertzsprung-Russell diagram and determine the black hole mass function. Secondly, wind strength dictates the atmospheric structure that sets the ionising flux. Thirdly, the wind directly intervenes with the stellar envelope structure, which is decisive for both single star and binary evolution, affecting predictions for gravitational wave events. Key findings of current hot-star research include:\n  * The traditional line-driven wind theory is being updated with Monte Carlo and co-moving frame computations, re"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2109.08164","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/2109.08164/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":"2109.08164","created_at":"2026-07-05T04:30:52.701374+00:00"},{"alias_kind":"arxiv_version","alias_value":"2109.08164v4","created_at":"2026-07-05T04:30:52.701374+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2109.08164","created_at":"2026-07-05T04:30:52.701374+00:00"},{"alias_kind":"pith_short_12","alias_value":"X7SN4O44TCSG","created_at":"2026-07-05T04:30:52.701374+00:00"},{"alias_kind":"pith_short_16","alias_value":"X7SN4O44TCSGICNZ","created_at":"2026-07-05T04:30:52.701374+00:00"},{"alias_kind":"pith_short_8","alias_value":"X7SN4O44","created_at":"2026-07-05T04:30:52.701374+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2604.08175","citing_title":"How many VHE gamma-ray binaries with young pulsars can be observed?","ref_index":66,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/X7SN4O44TCSGICNZZEREOTWJVA","json":"https://pith.science/pith/X7SN4O44TCSGICNZZEREOTWJVA.json","graph_json":"https://pith.science/api/pith-number/X7SN4O44TCSGICNZZEREOTWJVA/graph.json","events_json":"https://pith.science/api/pith-number/X7SN4O44TCSGICNZZEREOTWJVA/events.json","paper":"https://pith.science/paper/X7SN4O44"},"agent_actions":{"view_html":"https://pith.science/pith/X7SN4O44TCSGICNZZEREOTWJVA","download_json":"https://pith.science/pith/X7SN4O44TCSGICNZZEREOTWJVA.json","view_paper":"https://pith.science/paper/X7SN4O44","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2109.08164&json=true","fetch_graph":"https://pith.science/api/pith-number/X7SN4O44TCSGICNZZEREOTWJVA/graph.json","fetch_events":"https://pith.science/api/pith-number/X7SN4O44TCSGICNZZEREOTWJVA/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/X7SN4O44TCSGICNZZEREOTWJVA/action/timestamp_anchor","attest_storage":"https://pith.science/pith/X7SN4O44TCSGICNZZEREOTWJVA/action/storage_attestation","attest_author":"https://pith.science/pith/X7SN4O44TCSGICNZZEREOTWJVA/action/author_attestation","sign_citation":"https://pith.science/pith/X7SN4O44TCSGICNZZEREOTWJVA/action/citation_signature","submit_replication":"https://pith.science/pith/X7SN4O44TCSGICNZZEREOTWJVA/action/replication_record"}},"created_at":"2026-07-05T04:30:52.701374+00:00","updated_at":"2026-07-05T04:30:52.701374+00:00"}