{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2019:JKMASWOQLFKSG63QFZN7KMNBWV","short_pith_number":"pith:JKMASWOQ","schema_version":"1.0","canonical_sha256":"4a980959d05955237b702e5bf531a1b566a4f0730b3c00172178aba667dc592a","source":{"kind":"arxiv","id":"1902.00547","version":3},"attestation_state":"computed","paper":{"title":"Three-Dimensional Supernova Explosion Simulations of 9-, 10-, 11-, 12-, and 13-M$_{\\odot}$ Stars","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"astro-ph.SR","authors_text":"Adam Burrows, David Radice, David Vartanyan","submitted_at":"2019-02-01T20:16:44Z","abstract_excerpt":"Using the new state-of-the-art core-collapse supernova (CCSN) code F{\\sc{ornax}}, we have simulated the three-dimensional dynamical evolution of the cores of 9-, 10-, 11-, 12-, and 13-M$_{\\odot}$ stars from the onset of collapse. Stars from 8-M$_{\\odot}$ to 13-M$_{\\odot}$ constitute roughly 50% of all massive stars, so the explosive potential for this mass range is important to the overall theory of CCSNe. We find that the 9-, 10-, 11-, and 12-M$_{\\odot}$ models explode in 3D easily, but that the 13-M$_{\\odot}$ model does not. From these findings, and the fact that slightly more massive progen"},"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":"1902.00547","kind":"arxiv","version":3},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2019-02-01T20:16:44Z","cross_cats_sorted":["astro-ph.HE"],"title_canon_sha256":"c6d3fc7975ab2352af59cc8a3fe8900909baaf1d769de2b2b963bfd2a9ccad17","abstract_canon_sha256":"50101e8553c86c2684253fcb07e26556a0155faeb00c389981a8203a9f6da7c4"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-17T23:51:19.099463Z","signature_b64":"lUt/miPhYMrdqeLO2QdlyDAx5lM5K6I4iVBeryWakWb3mEutolj+dPTpzijbZCjYn7Ckj/N+J255n6+mmuv2BA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"4a980959d05955237b702e5bf531a1b566a4f0730b3c00172178aba667dc592a","last_reissued_at":"2026-05-17T23:51:19.098881Z","signature_status":"signed_v1","first_computed_at":"2026-05-17T23:51:19.098881Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Three-Dimensional Supernova Explosion Simulations of 9-, 10-, 11-, 12-, and 13-M$_{\\odot}$ Stars","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"astro-ph.SR","authors_text":"Adam Burrows, David Radice, David Vartanyan","submitted_at":"2019-02-01T20:16:44Z","abstract_excerpt":"Using the new state-of-the-art core-collapse supernova (CCSN) code F{\\sc{ornax}}, we have simulated the three-dimensional dynamical evolution of the cores of 9-, 10-, 11-, 12-, and 13-M$_{\\odot}$ stars from the onset of collapse. Stars from 8-M$_{\\odot}$ to 13-M$_{\\odot}$ constitute roughly 50% of all massive stars, so the explosive potential for this mass range is important to the overall theory of CCSNe. We find that the 9-, 10-, 11-, and 12-M$_{\\odot}$ models explode in 3D easily, but that the 13-M$_{\\odot}$ model does not. From these findings, and the fact that slightly more massive progen"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1902.00547","kind":"arxiv","version":3},"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":"1902.00547","created_at":"2026-05-17T23:51:19.098978+00:00"},{"alias_kind":"arxiv_version","alias_value":"1902.00547v3","created_at":"2026-05-17T23:51:19.098978+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1902.00547","created_at":"2026-05-17T23:51:19.098978+00:00"},{"alias_kind":"pith_short_12","alias_value":"JKMASWOQLFKS","created_at":"2026-05-18T12:33:21.387695+00:00"},{"alias_kind":"pith_short_16","alias_value":"JKMASWOQLFKSG63Q","created_at":"2026-05-18T12:33:21.387695+00:00"},{"alias_kind":"pith_short_8","alias_value":"JKMASWOQ","created_at":"2026-05-18T12:33:21.387695+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2605.16504","citing_title":"Neutrino Flavor Conversion Shapes the Rate of Failed Core-collapse Supernovae","ref_index":13,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/JKMASWOQLFKSG63QFZN7KMNBWV","json":"https://pith.science/pith/JKMASWOQLFKSG63QFZN7KMNBWV.json","graph_json":"https://pith.science/api/pith-number/JKMASWOQLFKSG63QFZN7KMNBWV/graph.json","events_json":"https://pith.science/api/pith-number/JKMASWOQLFKSG63QFZN7KMNBWV/events.json","paper":"https://pith.science/paper/JKMASWOQ"},"agent_actions":{"view_html":"https://pith.science/pith/JKMASWOQLFKSG63QFZN7KMNBWV","download_json":"https://pith.science/pith/JKMASWOQLFKSG63QFZN7KMNBWV.json","view_paper":"https://pith.science/paper/JKMASWOQ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1902.00547&json=true","fetch_graph":"https://pith.science/api/pith-number/JKMASWOQLFKSG63QFZN7KMNBWV/graph.json","fetch_events":"https://pith.science/api/pith-number/JKMASWOQLFKSG63QFZN7KMNBWV/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/JKMASWOQLFKSG63QFZN7KMNBWV/action/timestamp_anchor","attest_storage":"https://pith.science/pith/JKMASWOQLFKSG63QFZN7KMNBWV/action/storage_attestation","attest_author":"https://pith.science/pith/JKMASWOQLFKSG63QFZN7KMNBWV/action/author_attestation","sign_citation":"https://pith.science/pith/JKMASWOQLFKSG63QFZN7KMNBWV/action/citation_signature","submit_replication":"https://pith.science/pith/JKMASWOQLFKSG63QFZN7KMNBWV/action/replication_record"}},"created_at":"2026-05-17T23:51:19.098978+00:00","updated_at":"2026-05-17T23:51:19.098978+00:00"}