{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2017:2WQEDIV6FDFSO6URNA2ER5I4EO","short_pith_number":"pith:2WQEDIV6","schema_version":"1.0","canonical_sha256":"d5a041a2be28cb277a91683448f51c23878615c239062ae28d290e9f73a6a745","source":{"kind":"arxiv","id":"1704.08696","version":2},"attestation_state":"computed","paper":{"title":"Pre-Supernova Outbursts via Wave Heating in Massive Stars I: Red Supergiants","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"astro-ph.SR","authors_text":"Jim Fuller","submitted_at":"2017-04-27T18:00:04Z","abstract_excerpt":"Early observations of supernovae (SNe) indicate that enhanced mass loss and pre-SN outbursts may occur in progenitors of many types of SNe. We investigate the role of energy transport via waves driven by vigorous convection during late-stage nuclear burning of otherwise typical $15 \\, M_\\odot$ red supergiant SNe progenitors. Using MESA stellar evolution models including 1D hydrodynamics, we find that waves carry $\\sim \\! 10^7 \\, L_\\odot$ of power from the core to the envelope during core neon/oxygen burning in the final years before core collapse. The waves damp via shocks and radiative diffus"},"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":"1704.08696","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2017-04-27T18:00:04Z","cross_cats_sorted":["astro-ph.HE"],"title_canon_sha256":"d0fa2144683bc306db78043d1ff757b2e5d3db8d9623d294fb9d92357b0bed26","abstract_canon_sha256":"16babef607a74f961ae6f4ec6035803a880cc06f52189b722e34d94ed2baafb3"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:35:33.791633Z","signature_b64":"x8triT1vHBEzW2DXIJ2RcbfSst6ia9ax1kAHy3GqeK3KKs5NtU1pfhDBxRr4+c/kL+ZSI3GKUiBupsxnqvs8Dw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"d5a041a2be28cb277a91683448f51c23878615c239062ae28d290e9f73a6a745","last_reissued_at":"2026-05-18T00:35:33.790487Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:35:33.790487Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Pre-Supernova Outbursts via Wave Heating in Massive Stars I: Red Supergiants","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"astro-ph.SR","authors_text":"Jim Fuller","submitted_at":"2017-04-27T18:00:04Z","abstract_excerpt":"Early observations of supernovae (SNe) indicate that enhanced mass loss and pre-SN outbursts may occur in progenitors of many types of SNe. We investigate the role of energy transport via waves driven by vigorous convection during late-stage nuclear burning of otherwise typical $15 \\, M_\\odot$ red supergiant SNe progenitors. Using MESA stellar evolution models including 1D hydrodynamics, we find that waves carry $\\sim \\! 10^7 \\, L_\\odot$ of power from the core to the envelope during core neon/oxygen burning in the final years before core collapse. The waves damp via shocks and radiative diffus"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1704.08696","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":"1704.08696","created_at":"2026-05-18T00:35:33.790898+00:00"},{"alias_kind":"arxiv_version","alias_value":"1704.08696v2","created_at":"2026-05-18T00:35:33.790898+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1704.08696","created_at":"2026-05-18T00:35:33.790898+00:00"},{"alias_kind":"pith_short_12","alias_value":"2WQEDIV6FDFS","created_at":"2026-05-18T12:30:55.937587+00:00"},{"alias_kind":"pith_short_16","alias_value":"2WQEDIV6FDFSO6UR","created_at":"2026-05-18T12:30:55.937587+00:00"},{"alias_kind":"pith_short_8","alias_value":"2WQEDIV6","created_at":"2026-05-18T12:30:55.937587+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2605.21062","citing_title":"Neutron star-companion interaction in core collapse supernovae. Population synthesis based on detailed binary evolution models","ref_index":145,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/2WQEDIV6FDFSO6URNA2ER5I4EO","json":"https://pith.science/pith/2WQEDIV6FDFSO6URNA2ER5I4EO.json","graph_json":"https://pith.science/api/pith-number/2WQEDIV6FDFSO6URNA2ER5I4EO/graph.json","events_json":"https://pith.science/api/pith-number/2WQEDIV6FDFSO6URNA2ER5I4EO/events.json","paper":"https://pith.science/paper/2WQEDIV6"},"agent_actions":{"view_html":"https://pith.science/pith/2WQEDIV6FDFSO6URNA2ER5I4EO","download_json":"https://pith.science/pith/2WQEDIV6FDFSO6URNA2ER5I4EO.json","view_paper":"https://pith.science/paper/2WQEDIV6","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1704.08696&json=true","fetch_graph":"https://pith.science/api/pith-number/2WQEDIV6FDFSO6URNA2ER5I4EO/graph.json","fetch_events":"https://pith.science/api/pith-number/2WQEDIV6FDFSO6URNA2ER5I4EO/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/2WQEDIV6FDFSO6URNA2ER5I4EO/action/timestamp_anchor","attest_storage":"https://pith.science/pith/2WQEDIV6FDFSO6URNA2ER5I4EO/action/storage_attestation","attest_author":"https://pith.science/pith/2WQEDIV6FDFSO6URNA2ER5I4EO/action/author_attestation","sign_citation":"https://pith.science/pith/2WQEDIV6FDFSO6URNA2ER5I4EO/action/citation_signature","submit_replication":"https://pith.science/pith/2WQEDIV6FDFSO6URNA2ER5I4EO/action/replication_record"}},"created_at":"2026-05-18T00:35:33.790898+00:00","updated_at":"2026-05-18T00:35:33.790898+00:00"}