{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2020:NMXGXT4YMDRDDZSDW7NBNST5H7","short_pith_number":"pith:NMXGXT4Y","schema_version":"1.0","canonical_sha256":"6b2e6bcf9860e231e643b7da16ca7d3fcff2790229a371a95992fbaac5f65528","source":{"kind":"arxiv","id":"2011.09000","version":2},"attestation_state":"computed","paper":{"title":"Determining the Structure of Rotating Massive Stellar Cores with Gravitational Waves","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"Evan P. O'Connor, Kuo-Chuan Pan, MacKenzie L. Warren, Michael A. Pajkos, Sean M. Couch","submitted_at":"2020-11-17T23:21:00Z","abstract_excerpt":"The gravitational wave (GW) signal resulting from stellar core collapse encodes a wealth of information about the physical parameters of the progenitor star and the resulting core-collapse supernova (CCSN). We present a novel approach to constrain CCSN progenitor properties at collapse using two of the most detectable parts of the GW signal: the core-bounce signal and evolution of the dominant frequency mode from the protoneutron star. We focus on the period after core bounce but before explosion and investigate the predictive power of GWs from rotating CCSNe to constrain properties of the pro"},"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":"2011.09000","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2020-11-17T23:21:00Z","cross_cats_sorted":[],"title_canon_sha256":"ec7a1cfa169e85c6c78fee6e5092832f367b7d71e95ddb6a52e1f3bd0a782720","abstract_canon_sha256":"a796ea0a5accfc37758915ab11e8025b5bec568b7a7d1d25eefde00db84097ff"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T02:51:37.286627Z","signature_b64":"TX54CjiwnuLhLXv0Z131I02R6WplWbMMauQvxu0T/eNLTFjAqgjoMS/n07vvr/vKCx1PeW9MnlrGrXBQyfjQBg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"6b2e6bcf9860e231e643b7da16ca7d3fcff2790229a371a95992fbaac5f65528","last_reissued_at":"2026-07-05T02:51:37.286213Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T02:51:37.286213Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Determining the Structure of Rotating Massive Stellar Cores with Gravitational Waves","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"Evan P. O'Connor, Kuo-Chuan Pan, MacKenzie L. Warren, Michael A. Pajkos, Sean M. Couch","submitted_at":"2020-11-17T23:21:00Z","abstract_excerpt":"The gravitational wave (GW) signal resulting from stellar core collapse encodes a wealth of information about the physical parameters of the progenitor star and the resulting core-collapse supernova (CCSN). We present a novel approach to constrain CCSN progenitor properties at collapse using two of the most detectable parts of the GW signal: the core-bounce signal and evolution of the dominant frequency mode from the protoneutron star. We focus on the period after core bounce but before explosion and investigate the predictive power of GWs from rotating CCSNe to constrain properties of the pro"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2011.09000","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/2011.09000/integrity.json","findings":[],"available":true,"detectors_run":[],"snapshot_sha256":"c28c3603d3b5d939e8dc4c7e95fa8dfce3d595e45f758748cecf8e644a296938"},"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":"2011.09000","created_at":"2026-07-05T02:51:37.286270+00:00"},{"alias_kind":"arxiv_version","alias_value":"2011.09000v2","created_at":"2026-07-05T02:51:37.286270+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2011.09000","created_at":"2026-07-05T02:51:37.286270+00:00"},{"alias_kind":"pith_short_12","alias_value":"NMXGXT4YMDRD","created_at":"2026-07-05T02:51:37.286270+00:00"},{"alias_kind":"pith_short_16","alias_value":"NMXGXT4YMDRDDZSD","created_at":"2026-07-05T02:51:37.286270+00:00"},{"alias_kind":"pith_short_8","alias_value":"NMXGXT4Y","created_at":"2026-07-05T02:51:37.286270+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2605.04896","citing_title":"Parameter Estimation Horizon of Core-Collapse Supernovae with Current and Next-Generation Gravitational-Wave Detectors","ref_index":63,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/NMXGXT4YMDRDDZSDW7NBNST5H7","json":"https://pith.science/pith/NMXGXT4YMDRDDZSDW7NBNST5H7.json","graph_json":"https://pith.science/api/pith-number/NMXGXT4YMDRDDZSDW7NBNST5H7/graph.json","events_json":"https://pith.science/api/pith-number/NMXGXT4YMDRDDZSDW7NBNST5H7/events.json","paper":"https://pith.science/paper/NMXGXT4Y"},"agent_actions":{"view_html":"https://pith.science/pith/NMXGXT4YMDRDDZSDW7NBNST5H7","download_json":"https://pith.science/pith/NMXGXT4YMDRDDZSDW7NBNST5H7.json","view_paper":"https://pith.science/paper/NMXGXT4Y","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2011.09000&json=true","fetch_graph":"https://pith.science/api/pith-number/NMXGXT4YMDRDDZSDW7NBNST5H7/graph.json","fetch_events":"https://pith.science/api/pith-number/NMXGXT4YMDRDDZSDW7NBNST5H7/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/NMXGXT4YMDRDDZSDW7NBNST5H7/action/timestamp_anchor","attest_storage":"https://pith.science/pith/NMXGXT4YMDRDDZSDW7NBNST5H7/action/storage_attestation","attest_author":"https://pith.science/pith/NMXGXT4YMDRDDZSDW7NBNST5H7/action/author_attestation","sign_citation":"https://pith.science/pith/NMXGXT4YMDRDDZSDW7NBNST5H7/action/citation_signature","submit_replication":"https://pith.science/pith/NMXGXT4YMDRDDZSDW7NBNST5H7/action/replication_record"}},"created_at":"2026-07-05T02:51:37.286270+00:00","updated_at":"2026-07-05T02:51:37.286270+00:00"}