{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2017:RBCK5LLJ4TB2X6D3TTGWB3J6L3","short_pith_number":"pith:RBCK5LLJ","schema_version":"1.0","canonical_sha256":"8844aead69e4c3abf87b9ccd60ed3e5ec68ed3b4dcec877901afc226123d4a6a","source":{"kind":"arxiv","id":"1710.01763","version":4},"attestation_state":"computed","paper":{"title":"Pop III $\\textit{i}$-process Nucleosynthesis and the Elemental Abundances of SMSS J0313-6708 and the Most Iron-Poor Stars","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"F. Herwig, M. Pignatari, O. Clarkson","submitted_at":"2017-10-04T19:03:09Z","abstract_excerpt":"We have investigated a highly energetic H-ingestion event during shell He burning leading to H-burning luminosities of $\\log(L_\\mathrm{H}/\\mathrm{\\Lsun}) \\sim 13$ in a $45 \\Msun$ Pop III massive stellar model. In order to track the nucleosynthesis which may occur in such an event, we run a series of single-zone nucleosynthesis models for typical conditions found in the stellar evolution model. Such nucleosynthesis conditions may lead to $\\textit{i}-$process neutron densities of up to $ \\sim 10^{13} \\mathrm{cm}^{-3}$. The resulting simulation abundance pattern, where Mg comes from He burning an"},"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":"1710.01763","kind":"arxiv","version":4},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2017-10-04T19:03:09Z","cross_cats_sorted":[],"title_canon_sha256":"9ab0eca0b71ec23ee29e84620ac58e75799292013f8a1504a362f6bca0786a22","abstract_canon_sha256":"459e3bd4a04fde5a29c4d69c8da5c19ac200ae50ed367c57997459061ab329d1"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:27:18.800690Z","signature_b64":"wWzqqBhHVZu+nO25oZoazQM275mj6TFga5F1jLu5uzV2cQWoyMPLM41eeuJMorHLghe8IwgtO5of1sTZaykvAg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"8844aead69e4c3abf87b9ccd60ed3e5ec68ed3b4dcec877901afc226123d4a6a","last_reissued_at":"2026-05-18T00:27:18.800280Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:27:18.800280Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Pop III $\\textit{i}$-process Nucleosynthesis and the Elemental Abundances of SMSS J0313-6708 and the Most Iron-Poor Stars","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"F. Herwig, M. Pignatari, O. Clarkson","submitted_at":"2017-10-04T19:03:09Z","abstract_excerpt":"We have investigated a highly energetic H-ingestion event during shell He burning leading to H-burning luminosities of $\\log(L_\\mathrm{H}/\\mathrm{\\Lsun}) \\sim 13$ in a $45 \\Msun$ Pop III massive stellar model. In order to track the nucleosynthesis which may occur in such an event, we run a series of single-zone nucleosynthesis models for typical conditions found in the stellar evolution model. Such nucleosynthesis conditions may lead to $\\textit{i}-$process neutron densities of up to $ \\sim 10^{13} \\mathrm{cm}^{-3}$. The resulting simulation abundance pattern, where Mg comes from He burning an"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1710.01763","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":""},"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":"1710.01763","created_at":"2026-05-18T00:27:18.800344+00:00"},{"alias_kind":"arxiv_version","alias_value":"1710.01763v4","created_at":"2026-05-18T00:27:18.800344+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1710.01763","created_at":"2026-05-18T00:27:18.800344+00:00"},{"alias_kind":"pith_short_12","alias_value":"RBCK5LLJ4TB2","created_at":"2026-05-18T12:31:39.905425+00:00"},{"alias_kind":"pith_short_16","alias_value":"RBCK5LLJ4TB2X6D3","created_at":"2026-05-18T12:31:39.905425+00:00"},{"alias_kind":"pith_short_8","alias_value":"RBCK5LLJ","created_at":"2026-05-18T12:31:39.905425+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2605.11074","citing_title":"Observational Signatures and Constraints on the Intermediate Neutron-Capture Process. The Case of the CEMP star TYC 6044-714-1 (RAVE J094921.8-161722)","ref_index":196,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/RBCK5LLJ4TB2X6D3TTGWB3J6L3","json":"https://pith.science/pith/RBCK5LLJ4TB2X6D3TTGWB3J6L3.json","graph_json":"https://pith.science/api/pith-number/RBCK5LLJ4TB2X6D3TTGWB3J6L3/graph.json","events_json":"https://pith.science/api/pith-number/RBCK5LLJ4TB2X6D3TTGWB3J6L3/events.json","paper":"https://pith.science/paper/RBCK5LLJ"},"agent_actions":{"view_html":"https://pith.science/pith/RBCK5LLJ4TB2X6D3TTGWB3J6L3","download_json":"https://pith.science/pith/RBCK5LLJ4TB2X6D3TTGWB3J6L3.json","view_paper":"https://pith.science/paper/RBCK5LLJ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1710.01763&json=true","fetch_graph":"https://pith.science/api/pith-number/RBCK5LLJ4TB2X6D3TTGWB3J6L3/graph.json","fetch_events":"https://pith.science/api/pith-number/RBCK5LLJ4TB2X6D3TTGWB3J6L3/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/RBCK5LLJ4TB2X6D3TTGWB3J6L3/action/timestamp_anchor","attest_storage":"https://pith.science/pith/RBCK5LLJ4TB2X6D3TTGWB3J6L3/action/storage_attestation","attest_author":"https://pith.science/pith/RBCK5LLJ4TB2X6D3TTGWB3J6L3/action/author_attestation","sign_citation":"https://pith.science/pith/RBCK5LLJ4TB2X6D3TTGWB3J6L3/action/citation_signature","submit_replication":"https://pith.science/pith/RBCK5LLJ4TB2X6D3TTGWB3J6L3/action/replication_record"}},"created_at":"2026-05-18T00:27:18.800344+00:00","updated_at":"2026-05-18T00:27:18.800344+00:00"}