{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2010:XYLMXHEBOBCPXH7SMGXG2NUAGZ","short_pith_number":"pith:XYLMXHEB","schema_version":"1.0","canonical_sha256":"be16cb9c817044fb9ff261ae6d3680366b3df6381bca5be734afae0fe26907f3","source":{"kind":"arxiv","id":"1002.2346","version":1},"attestation_state":"computed","paper":{"title":"Charged-Particle and Neutron-Capture Processes in the High-Entropy Wind of Core-Collapse Supernovae","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"B. Pfeiffer, F.-K. Thilemann, J.W. Truran, K. Farouqi, K.-L. Kratz, T. Rauscher","submitted_at":"2010-02-11T14:30:10Z","abstract_excerpt":"The astrophysical site of the r-process is still uncertain, and a full exploration of the systematics of this process in terms of its dependence on nuclear properties from stability to the neutron drip-line within realistic stellar environments has still to be undertaken. Sufficiently high neutron to seed ratios can only be obtained either in very neutron-rich low-entropy environments or moderately neutron-rich high-entropy environments, related to neutron star mergers (or jets of neutron star matter) and the high-entropy wind of core-collapse supernova explosions. As chemical evolution models"},"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":"1002.2346","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2010-02-11T14:30:10Z","cross_cats_sorted":[],"title_canon_sha256":"1cb1cc7e753e71b88fa85611f37e40a6cf091de886702e85635546bc83364e2f","abstract_canon_sha256":"49050dc80275f33115a8887ca954c5668dcdcd65fd13a068a7afc746a2fd2fa9"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:09:09.318141Z","signature_b64":"I6quwKJ7Le0pXPpmPXBJpfrjmfbhZMqHb/TAZZ46cEwWeFd4qa0kWrcyX4X8bC0TiwJxoypudeMeh7n0MT+VDQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"be16cb9c817044fb9ff261ae6d3680366b3df6381bca5be734afae0fe26907f3","last_reissued_at":"2026-05-18T02:09:09.317677Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:09:09.317677Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Charged-Particle and Neutron-Capture Processes in the High-Entropy Wind of Core-Collapse Supernovae","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"B. Pfeiffer, F.-K. Thilemann, J.W. Truran, K. Farouqi, K.-L. Kratz, T. Rauscher","submitted_at":"2010-02-11T14:30:10Z","abstract_excerpt":"The astrophysical site of the r-process is still uncertain, and a full exploration of the systematics of this process in terms of its dependence on nuclear properties from stability to the neutron drip-line within realistic stellar environments has still to be undertaken. Sufficiently high neutron to seed ratios can only be obtained either in very neutron-rich low-entropy environments or moderately neutron-rich high-entropy environments, related to neutron star mergers (or jets of neutron star matter) and the high-entropy wind of core-collapse supernova explosions. As chemical evolution models"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1002.2346","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":"1002.2346","created_at":"2026-05-18T02:09:09.317736+00:00"},{"alias_kind":"arxiv_version","alias_value":"1002.2346v1","created_at":"2026-05-18T02:09:09.317736+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1002.2346","created_at":"2026-05-18T02:09:09.317736+00:00"},{"alias_kind":"pith_short_12","alias_value":"XYLMXHEBOBCP","created_at":"2026-05-18T12:26:17.028572+00:00"},{"alias_kind":"pith_short_16","alias_value":"XYLMXHEBOBCPXH7S","created_at":"2026-05-18T12:26:17.028572+00:00"},{"alias_kind":"pith_short_8","alias_value":"XYLMXHEB","created_at":"2026-05-18T12:26:17.028572+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2605.23690","citing_title":"The s- and r- components of the proto-solar composition","ref_index":69,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/XYLMXHEBOBCPXH7SMGXG2NUAGZ","json":"https://pith.science/pith/XYLMXHEBOBCPXH7SMGXG2NUAGZ.json","graph_json":"https://pith.science/api/pith-number/XYLMXHEBOBCPXH7SMGXG2NUAGZ/graph.json","events_json":"https://pith.science/api/pith-number/XYLMXHEBOBCPXH7SMGXG2NUAGZ/events.json","paper":"https://pith.science/paper/XYLMXHEB"},"agent_actions":{"view_html":"https://pith.science/pith/XYLMXHEBOBCPXH7SMGXG2NUAGZ","download_json":"https://pith.science/pith/XYLMXHEBOBCPXH7SMGXG2NUAGZ.json","view_paper":"https://pith.science/paper/XYLMXHEB","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1002.2346&json=true","fetch_graph":"https://pith.science/api/pith-number/XYLMXHEBOBCPXH7SMGXG2NUAGZ/graph.json","fetch_events":"https://pith.science/api/pith-number/XYLMXHEBOBCPXH7SMGXG2NUAGZ/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/XYLMXHEBOBCPXH7SMGXG2NUAGZ/action/timestamp_anchor","attest_storage":"https://pith.science/pith/XYLMXHEBOBCPXH7SMGXG2NUAGZ/action/storage_attestation","attest_author":"https://pith.science/pith/XYLMXHEBOBCPXH7SMGXG2NUAGZ/action/author_attestation","sign_citation":"https://pith.science/pith/XYLMXHEBOBCPXH7SMGXG2NUAGZ/action/citation_signature","submit_replication":"https://pith.science/pith/XYLMXHEBOBCPXH7SMGXG2NUAGZ/action/replication_record"}},"created_at":"2026-05-18T02:09:09.317736+00:00","updated_at":"2026-05-18T02:09:09.317736+00:00"}