{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2009:GCKLFR4P57KUHN3E72FLGQTPBT","short_pith_number":"pith:GCKLFR4P","schema_version":"1.0","canonical_sha256":"3094b2c78fefd543b764fe8ab3426f0cf324f02d5a066b807ea408502ed80555","source":{"kind":"arxiv","id":"0909.0179","version":2},"attestation_state":"computed","paper":{"title":"Improved estimate of electron capture rates on nuclei during stellar core collapse","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"nucl-th","authors_text":"A. Juodagalvis, G. Mart\\'inez-Pinedo, J.M. Sampaio, K. Langanke, W.R. Hix","submitted_at":"2009-09-01T13:17:20Z","abstract_excerpt":"Electron captures on nuclei play an important role in the dynamics of the collapsing core of a massive star that leads to a supernova explosion. Recent calculations of these capture rates were based on microscopic models which account for relevant degrees of freedom. Due to computational restrictions such calculations were limited to a modest number of nuclei, mainly in the mass range A=45-110. Recent supernova simulations show that this pool of nuclei, however, omits the very neutron-rich and heavy nuclei which dominate the nuclear composition during the last phase of the collapse before neut"},"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":"0909.0179","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"nucl-th","submitted_at":"2009-09-01T13:17:20Z","cross_cats_sorted":[],"title_canon_sha256":"97a1717e0df9373af74026e6232cf3147a28bdf6a01ca6587fd26e9f2209d1d8","abstract_canon_sha256":"85e86ce2bdd2e0622409d8f1320bcc1ff7391aa1b13fe68c05a9051696f22ac4"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T04:35:05.283951Z","signature_b64":"NMimHkP20PFcCNrFWIuocv09TR3HhElFPoOSKe6JYtAhEg+bcb5KZo6X8nXVuFjFupyr/Iy88MeGFFX+qnagAA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"3094b2c78fefd543b764fe8ab3426f0cf324f02d5a066b807ea408502ed80555","last_reissued_at":"2026-05-18T04:35:05.283565Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T04:35:05.283565Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Improved estimate of electron capture rates on nuclei during stellar core collapse","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"nucl-th","authors_text":"A. Juodagalvis, G. Mart\\'inez-Pinedo, J.M. Sampaio, K. Langanke, W.R. Hix","submitted_at":"2009-09-01T13:17:20Z","abstract_excerpt":"Electron captures on nuclei play an important role in the dynamics of the collapsing core of a massive star that leads to a supernova explosion. Recent calculations of these capture rates were based on microscopic models which account for relevant degrees of freedom. Due to computational restrictions such calculations were limited to a modest number of nuclei, mainly in the mass range A=45-110. Recent supernova simulations show that this pool of nuclei, however, omits the very neutron-rich and heavy nuclei which dominate the nuclear composition during the last phase of the collapse before neut"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"0909.0179","kind":"arxiv","version":2},"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":"0909.0179","created_at":"2026-05-18T04:35:05.283624+00:00"},{"alias_kind":"arxiv_version","alias_value":"0909.0179v2","created_at":"2026-05-18T04:35:05.283624+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.0909.0179","created_at":"2026-05-18T04:35:05.283624+00:00"},{"alias_kind":"pith_short_12","alias_value":"GCKLFR4P57KU","created_at":"2026-05-18T12:25:59.703012+00:00"},{"alias_kind":"pith_short_16","alias_value":"GCKLFR4P57KUHN3E","created_at":"2026-05-18T12:25:59.703012+00:00"},{"alias_kind":"pith_short_8","alias_value":"GCKLFR4P","created_at":"2026-05-18T12:25:59.703012+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2601.08269","citing_title":"Bifurcated Impact of Neutrino Fast Flavor Conversion on Core-collapse Supernovae Informed by Multi-angle Neutrino Radiation Hydrodynamics","ref_index":37,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/GCKLFR4P57KUHN3E72FLGQTPBT","json":"https://pith.science/pith/GCKLFR4P57KUHN3E72FLGQTPBT.json","graph_json":"https://pith.science/api/pith-number/GCKLFR4P57KUHN3E72FLGQTPBT/graph.json","events_json":"https://pith.science/api/pith-number/GCKLFR4P57KUHN3E72FLGQTPBT/events.json","paper":"https://pith.science/paper/GCKLFR4P"},"agent_actions":{"view_html":"https://pith.science/pith/GCKLFR4P57KUHN3E72FLGQTPBT","download_json":"https://pith.science/pith/GCKLFR4P57KUHN3E72FLGQTPBT.json","view_paper":"https://pith.science/paper/GCKLFR4P","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=0909.0179&json=true","fetch_graph":"https://pith.science/api/pith-number/GCKLFR4P57KUHN3E72FLGQTPBT/graph.json","fetch_events":"https://pith.science/api/pith-number/GCKLFR4P57KUHN3E72FLGQTPBT/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/GCKLFR4P57KUHN3E72FLGQTPBT/action/timestamp_anchor","attest_storage":"https://pith.science/pith/GCKLFR4P57KUHN3E72FLGQTPBT/action/storage_attestation","attest_author":"https://pith.science/pith/GCKLFR4P57KUHN3E72FLGQTPBT/action/author_attestation","sign_citation":"https://pith.science/pith/GCKLFR4P57KUHN3E72FLGQTPBT/action/citation_signature","submit_replication":"https://pith.science/pith/GCKLFR4P57KUHN3E72FLGQTPBT/action/replication_record"}},"created_at":"2026-05-18T04:35:05.283624+00:00","updated_at":"2026-05-18T04:35:05.283624+00:00"}