{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2012:TK3LAZKSUE73PLYKIVOT4CVEAS","short_pith_number":"pith:TK3LAZKS","schema_version":"1.0","canonical_sha256":"9ab6b06552a13fb7af0a455d3e0aa404a35ed36b1e3fe4b1a475be30cf710bc9","source":{"kind":"arxiv","id":"1202.2620","version":1},"attestation_state":"computed","paper":{"title":"Rubidium, zirconium, and lithium production in intermediate-mass asymptotic giant branch stars","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"Amanda I. Karakas, David Yong, Domingo A. Garcia-Hernandez, Mark A. van Raai, M. Lugaro","submitted_at":"2012-02-13T04:17:53Z","abstract_excerpt":"A recent survey of a large sample of Galactic intermediate-mass (>3 Msun) asymptotic giant branch (AGB) stars shows that they exhibit large overabundances of rubidium (Rb) up to 100--1000 times solar. These observations set constraints on our theoretical notion of the slow neutron capture process (s process) that occurs inside intermediate-mass AGB stars. Lithium (Li) abundances are also reported for these stars. In intermediate-mass AGB stars, Li can be produced by proton captures occuring at the base of the convective envelope. For this reason the observations of Rb, Zr, and Li set complemen"},"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":"1202.2620","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2012-02-13T04:17:53Z","cross_cats_sorted":[],"title_canon_sha256":"5955a5f14066dcbf8e2fb3b2505491f24311f06f7640276d5d70194c0cff32f8","abstract_canon_sha256":"6ba3c2e68efca4be39c6d04b088d6f0ecc4ec43946e205ba72647108278abb11"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:58:30.820116Z","signature_b64":"J0pHwa+ucbUvVm7ln5M1UGpY91ErG951x/YpZl4+PkDJp6HeuZ7gf41Q80Pd+lNXCN36FzGBAOLT9OuGZSkfAg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"9ab6b06552a13fb7af0a455d3e0aa404a35ed36b1e3fe4b1a475be30cf710bc9","last_reissued_at":"2026-05-18T01:58:30.819673Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:58:30.819673Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Rubidium, zirconium, and lithium production in intermediate-mass asymptotic giant branch stars","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"Amanda I. Karakas, David Yong, Domingo A. Garcia-Hernandez, Mark A. van Raai, M. Lugaro","submitted_at":"2012-02-13T04:17:53Z","abstract_excerpt":"A recent survey of a large sample of Galactic intermediate-mass (>3 Msun) asymptotic giant branch (AGB) stars shows that they exhibit large overabundances of rubidium (Rb) up to 100--1000 times solar. These observations set constraints on our theoretical notion of the slow neutron capture process (s process) that occurs inside intermediate-mass AGB stars. Lithium (Li) abundances are also reported for these stars. In intermediate-mass AGB stars, Li can be produced by proton captures occuring at the base of the convective envelope. For this reason the observations of Rb, Zr, and Li set complemen"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1202.2620","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":"1202.2620","created_at":"2026-05-18T01:58:30.819743+00:00"},{"alias_kind":"arxiv_version","alias_value":"1202.2620v1","created_at":"2026-05-18T01:58:30.819743+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1202.2620","created_at":"2026-05-18T01:58:30.819743+00:00"},{"alias_kind":"pith_short_12","alias_value":"TK3LAZKSUE73","created_at":"2026-05-18T12:27:23.164592+00:00"},{"alias_kind":"pith_short_16","alias_value":"TK3LAZKSUE73PLYK","created_at":"2026-05-18T12:27:23.164592+00:00"},{"alias_kind":"pith_short_8","alias_value":"TK3LAZKS","created_at":"2026-05-18T12:27:23.164592+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2604.09205","citing_title":"Tracing the s-Process: Spectroscopic Insights into Chemical Abundances in O- and C-rich Evolved Stars","ref_index":62,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/TK3LAZKSUE73PLYKIVOT4CVEAS","json":"https://pith.science/pith/TK3LAZKSUE73PLYKIVOT4CVEAS.json","graph_json":"https://pith.science/api/pith-number/TK3LAZKSUE73PLYKIVOT4CVEAS/graph.json","events_json":"https://pith.science/api/pith-number/TK3LAZKSUE73PLYKIVOT4CVEAS/events.json","paper":"https://pith.science/paper/TK3LAZKS"},"agent_actions":{"view_html":"https://pith.science/pith/TK3LAZKSUE73PLYKIVOT4CVEAS","download_json":"https://pith.science/pith/TK3LAZKSUE73PLYKIVOT4CVEAS.json","view_paper":"https://pith.science/paper/TK3LAZKS","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1202.2620&json=true","fetch_graph":"https://pith.science/api/pith-number/TK3LAZKSUE73PLYKIVOT4CVEAS/graph.json","fetch_events":"https://pith.science/api/pith-number/TK3LAZKSUE73PLYKIVOT4CVEAS/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/TK3LAZKSUE73PLYKIVOT4CVEAS/action/timestamp_anchor","attest_storage":"https://pith.science/pith/TK3LAZKSUE73PLYKIVOT4CVEAS/action/storage_attestation","attest_author":"https://pith.science/pith/TK3LAZKSUE73PLYKIVOT4CVEAS/action/author_attestation","sign_citation":"https://pith.science/pith/TK3LAZKSUE73PLYKIVOT4CVEAS/action/citation_signature","submit_replication":"https://pith.science/pith/TK3LAZKSUE73PLYKIVOT4CVEAS/action/replication_record"}},"created_at":"2026-05-18T01:58:30.819743+00:00","updated_at":"2026-05-18T01:58:30.819743+00:00"}