{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2017:R34NEN7L4XCI6FJAFCSIWXNEL6","short_pith_number":"pith:R34NEN7L","schema_version":"1.0","canonical_sha256":"8ef8d237ebe5c48f152028a48b5da45fb477522e004aab5063c579de4b40d8c0","source":{"kind":"arxiv","id":"1708.05252","version":2},"attestation_state":"computed","paper":{"title":"Correlated Signatures of Gravitational-Wave and Neutrino Emission in Three-Dimensional General-Relativistic Core-Collapse Supernova Simulations","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"Kazuhiro Hayama, Kei Kotake, Takami Kuroda, Tomoya Takiwaki","submitted_at":"2017-08-17T13:04:06Z","abstract_excerpt":"We present results from general-relativistic (GR) three-dimensional (3D) core-collapse simulations with approximate neutrino transport for three non-rotating progenitors (11.2, 15, and 40 Msun) using different nuclear equations of state (EOSs). We find that the combination of progenitor's higher compactness at bounce and the use of softer EOS leads to stronger activity of the standing accretion shock instability (SASI). We confirm previous predications that the SASI produces characteristic time modulations both in neutrino and gravitational-wave (GW) signals. By performing a correlation analys"},"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":"1708.05252","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2017-08-17T13:04:06Z","cross_cats_sorted":[],"title_canon_sha256":"365b3602f12c042f3e3beefb992c8e0d383f277dae2093205c76f3001e56d37f","abstract_canon_sha256":"d95cddcd1055227c6a7d0adededd2f51ea5e1600b2c4f3538393e38cf3eff1f8"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:27:19.172848Z","signature_b64":"Oo3n0wl68PI8HVSu7eUYZ1berKBboOU6IzhJohkS7GU8Q3fnMa4QdbkMt/v9ywUoBTOzhrnL2NbILZvKCvfnCA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"8ef8d237ebe5c48f152028a48b5da45fb477522e004aab5063c579de4b40d8c0","last_reissued_at":"2026-05-18T00:27:19.172365Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:27:19.172365Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Correlated Signatures of Gravitational-Wave and Neutrino Emission in Three-Dimensional General-Relativistic Core-Collapse Supernova Simulations","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"Kazuhiro Hayama, Kei Kotake, Takami Kuroda, Tomoya Takiwaki","submitted_at":"2017-08-17T13:04:06Z","abstract_excerpt":"We present results from general-relativistic (GR) three-dimensional (3D) core-collapse simulations with approximate neutrino transport for three non-rotating progenitors (11.2, 15, and 40 Msun) using different nuclear equations of state (EOSs). We find that the combination of progenitor's higher compactness at bounce and the use of softer EOS leads to stronger activity of the standing accretion shock instability (SASI). We confirm previous predications that the SASI produces characteristic time modulations both in neutrino and gravitational-wave (GW) signals. By performing a correlation analys"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1708.05252","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":"1708.05252","created_at":"2026-05-18T00:27:19.172436+00:00"},{"alias_kind":"arxiv_version","alias_value":"1708.05252v2","created_at":"2026-05-18T00:27:19.172436+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1708.05252","created_at":"2026-05-18T00:27:19.172436+00:00"},{"alias_kind":"pith_short_12","alias_value":"R34NEN7L4XCI","created_at":"2026-05-18T12:31:39.905425+00:00"},{"alias_kind":"pith_short_16","alias_value":"R34NEN7L4XCI6FJA","created_at":"2026-05-18T12:31:39.905425+00:00"},{"alias_kind":"pith_short_8","alias_value":"R34NEN7L","created_at":"2026-05-18T12:31:39.905425+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":3,"internal_anchor_count":2,"sample":[{"citing_arxiv_id":"2605.21310","citing_title":"Contrastive self-supervised convolutional autoencoder for core-collapse supernova gravitational-wave detection","ref_index":171,"is_internal_anchor":true},{"citing_arxiv_id":"1912.02622","citing_title":"Science Case for the Einstein Telescope","ref_index":143,"is_internal_anchor":true},{"citing_arxiv_id":"2605.04896","citing_title":"Parameter Estimation Horizon of Core-Collapse Supernovae with Current and Next-Generation Gravitational-Wave Detectors","ref_index":42,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/R34NEN7L4XCI6FJAFCSIWXNEL6","json":"https://pith.science/pith/R34NEN7L4XCI6FJAFCSIWXNEL6.json","graph_json":"https://pith.science/api/pith-number/R34NEN7L4XCI6FJAFCSIWXNEL6/graph.json","events_json":"https://pith.science/api/pith-number/R34NEN7L4XCI6FJAFCSIWXNEL6/events.json","paper":"https://pith.science/paper/R34NEN7L"},"agent_actions":{"view_html":"https://pith.science/pith/R34NEN7L4XCI6FJAFCSIWXNEL6","download_json":"https://pith.science/pith/R34NEN7L4XCI6FJAFCSIWXNEL6.json","view_paper":"https://pith.science/paper/R34NEN7L","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1708.05252&json=true","fetch_graph":"https://pith.science/api/pith-number/R34NEN7L4XCI6FJAFCSIWXNEL6/graph.json","fetch_events":"https://pith.science/api/pith-number/R34NEN7L4XCI6FJAFCSIWXNEL6/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/R34NEN7L4XCI6FJAFCSIWXNEL6/action/timestamp_anchor","attest_storage":"https://pith.science/pith/R34NEN7L4XCI6FJAFCSIWXNEL6/action/storage_attestation","attest_author":"https://pith.science/pith/R34NEN7L4XCI6FJAFCSIWXNEL6/action/author_attestation","sign_citation":"https://pith.science/pith/R34NEN7L4XCI6FJAFCSIWXNEL6/action/citation_signature","submit_replication":"https://pith.science/pith/R34NEN7L4XCI6FJAFCSIWXNEL6/action/replication_record"}},"created_at":"2026-05-18T00:27:19.172436+00:00","updated_at":"2026-05-18T00:27:19.172436+00:00"}