{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2012:PYS4XSRFIR3XUSJ3QSOIVLTNQM","short_pith_number":"pith:PYS4XSRF","schema_version":"1.0","canonical_sha256":"7e25cbca2544777a493b849c8aae6d830b6358a182dee92bc10fb2858522425d","source":{"kind":"arxiv","id":"1208.1986","version":1},"attestation_state":"computed","paper":{"title":"Evaluating Systematic Dependencies of Type Ia Supernovae: The Influence of Central Density","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO","astro-ph.HE"],"primary_cat":"astro-ph.SR","authors_text":"Aaron P. Jackson, Alan C. Calder, Brendan K. Krueger, Dean M. Townsley, Edward F. Brown, Francis X. Timmes","submitted_at":"2012-08-09T18:08:54Z","abstract_excerpt":"We present a study exploring a systematic effect on the brightness of type Ia supernovae using numerical models that assume the single-degenerate paradigm. Our investigation varied the central density of the progenitor white dwarf at flame ignition, and considered its impact on the explosion yield, particularly the production and distribution of radioactive Ni-56, which powers the light curve. We performed a suite of two-dimensional simulations with randomized initial conditions, allowing us to characterize the statistical trends that we present. The simulations indicate that production of Fe-"},"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":"1208.1986","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2012-08-09T18:08:54Z","cross_cats_sorted":["astro-ph.CO","astro-ph.HE"],"title_canon_sha256":"9f7aa0ca8f2e95e79316a20b12ce345d9629bce536485d9b4bb5aee489b238a1","abstract_canon_sha256":"602f29cd77c62b41fc077cd25d1492fbbea971775c639b98225d709875c36bd2"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T03:45:22.658432Z","signature_b64":"ZYA8RmFoTsfpv/Vj0bBNQ4yaZEsHhZ+lJBsHl59QszcAdjfgVgNCQ/Mt5m1G+oqKOXOJhV7venImWxCJevfQDQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"7e25cbca2544777a493b849c8aae6d830b6358a182dee92bc10fb2858522425d","last_reissued_at":"2026-05-18T03:45:22.657978Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T03:45:22.657978Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Evaluating Systematic Dependencies of Type Ia Supernovae: The Influence of Central Density","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO","astro-ph.HE"],"primary_cat":"astro-ph.SR","authors_text":"Aaron P. Jackson, Alan C. Calder, Brendan K. Krueger, Dean M. Townsley, Edward F. Brown, Francis X. Timmes","submitted_at":"2012-08-09T18:08:54Z","abstract_excerpt":"We present a study exploring a systematic effect on the brightness of type Ia supernovae using numerical models that assume the single-degenerate paradigm. Our investigation varied the central density of the progenitor white dwarf at flame ignition, and considered its impact on the explosion yield, particularly the production and distribution of radioactive Ni-56, which powers the light curve. We performed a suite of two-dimensional simulations with randomized initial conditions, allowing us to characterize the statistical trends that we present. The simulations indicate that production of Fe-"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1208.1986","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":"1208.1986","created_at":"2026-05-18T03:45:22.658042+00:00"},{"alias_kind":"arxiv_version","alias_value":"1208.1986v1","created_at":"2026-05-18T03:45:22.658042+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1208.1986","created_at":"2026-05-18T03:45:22.658042+00:00"},{"alias_kind":"pith_short_12","alias_value":"PYS4XSRFIR3X","created_at":"2026-05-18T12:27:18.751474+00:00"},{"alias_kind":"pith_short_16","alias_value":"PYS4XSRFIR3XUSJ3","created_at":"2026-05-18T12:27:18.751474+00:00"},{"alias_kind":"pith_short_8","alias_value":"PYS4XSRF","created_at":"2026-05-18T12:27:18.751474+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2605.12596","citing_title":"Strong Progenitor Age Bias in Supernova Cosmology. III. Progenitor Age as the Physical Origin of the Type Ia Supernova Magnitude Steps with Host Properties","ref_index":56,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/PYS4XSRFIR3XUSJ3QSOIVLTNQM","json":"https://pith.science/pith/PYS4XSRFIR3XUSJ3QSOIVLTNQM.json","graph_json":"https://pith.science/api/pith-number/PYS4XSRFIR3XUSJ3QSOIVLTNQM/graph.json","events_json":"https://pith.science/api/pith-number/PYS4XSRFIR3XUSJ3QSOIVLTNQM/events.json","paper":"https://pith.science/paper/PYS4XSRF"},"agent_actions":{"view_html":"https://pith.science/pith/PYS4XSRFIR3XUSJ3QSOIVLTNQM","download_json":"https://pith.science/pith/PYS4XSRFIR3XUSJ3QSOIVLTNQM.json","view_paper":"https://pith.science/paper/PYS4XSRF","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1208.1986&json=true","fetch_graph":"https://pith.science/api/pith-number/PYS4XSRFIR3XUSJ3QSOIVLTNQM/graph.json","fetch_events":"https://pith.science/api/pith-number/PYS4XSRFIR3XUSJ3QSOIVLTNQM/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/PYS4XSRFIR3XUSJ3QSOIVLTNQM/action/timestamp_anchor","attest_storage":"https://pith.science/pith/PYS4XSRFIR3XUSJ3QSOIVLTNQM/action/storage_attestation","attest_author":"https://pith.science/pith/PYS4XSRFIR3XUSJ3QSOIVLTNQM/action/author_attestation","sign_citation":"https://pith.science/pith/PYS4XSRFIR3XUSJ3QSOIVLTNQM/action/citation_signature","submit_replication":"https://pith.science/pith/PYS4XSRFIR3XUSJ3QSOIVLTNQM/action/replication_record"}},"created_at":"2026-05-18T03:45:22.658042+00:00","updated_at":"2026-05-18T03:45:22.658042+00:00"}