{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2014:PLSYDJ2JQP4I5CMLWU22545EDW","short_pith_number":"pith:PLSYDJ2J","schema_version":"1.0","canonical_sha256":"7ae581a74983f88e898bb535aef3a41d836b8df6bf986ae6378f592c9a3413ed","source":{"kind":"arxiv","id":"1410.4557","version":2},"attestation_state":"computed","paper":{"title":"Pulsations of red supergiant pair-instability supernova progenitors leading to extreme mass loss","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"Norbert Langer, Takashi J. Moriya","submitted_at":"2014-10-16T20:00:01Z","abstract_excerpt":"Recent stellar evolution models show consistently that very massive metal-free stars evolve into red supergiants shortly before they explode. We argue that the envelopes of these stars, which will form pair-instability supernovae, become pulsationally unstable and that this will lead to extreme mass-loss rates despite the tiny metal content of the envelopes. We investigate the pulsational properties of such models and derive pulsationally induced mass-loss rates, which take the damping effects of the mass loss on the pulsations selfconsistently into account. We find that the pulsations may ind"},"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":"1410.4557","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2014-10-16T20:00:01Z","cross_cats_sorted":[],"title_canon_sha256":"62716417d9f04d8ab30074f5c928a8296ef73536ce0a07d7c373754ea31f2152","abstract_canon_sha256":"a6c25777beb740ccc7b7db327e29deb5672a18969c2472981abd41753c7dc5e3"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:31:20.505749Z","signature_b64":"5jrC3z6F/FWB3eUhdOYbDdfYhDq3LewKncksNkhxpqprnPMEGYY1srpNQFtYCbU/Qtv89YxunqA/A9i7m+E3DA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"7ae581a74983f88e898bb535aef3a41d836b8df6bf986ae6378f592c9a3413ed","last_reissued_at":"2026-05-18T02:31:20.505218Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:31:20.505218Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Pulsations of red supergiant pair-instability supernova progenitors leading to extreme mass loss","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"Norbert Langer, Takashi J. Moriya","submitted_at":"2014-10-16T20:00:01Z","abstract_excerpt":"Recent stellar evolution models show consistently that very massive metal-free stars evolve into red supergiants shortly before they explode. We argue that the envelopes of these stars, which will form pair-instability supernovae, become pulsationally unstable and that this will lead to extreme mass-loss rates despite the tiny metal content of the envelopes. We investigate the pulsational properties of such models and derive pulsationally induced mass-loss rates, which take the damping effects of the mass loss on the pulsations selfconsistently into account. We find that the pulsations may ind"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1410.4557","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":"1410.4557","created_at":"2026-05-18T02:31:20.505291+00:00"},{"alias_kind":"arxiv_version","alias_value":"1410.4557v2","created_at":"2026-05-18T02:31:20.505291+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1410.4557","created_at":"2026-05-18T02:31:20.505291+00:00"},{"alias_kind":"pith_short_12","alias_value":"PLSYDJ2JQP4I","created_at":"2026-05-18T12:28:43.426989+00:00"},{"alias_kind":"pith_short_16","alias_value":"PLSYDJ2JQP4I5CML","created_at":"2026-05-18T12:28:43.426989+00:00"},{"alias_kind":"pith_short_8","alias_value":"PLSYDJ2J","created_at":"2026-05-18T12:28:43.426989+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":161,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/PLSYDJ2JQP4I5CMLWU22545EDW","json":"https://pith.science/pith/PLSYDJ2JQP4I5CMLWU22545EDW.json","graph_json":"https://pith.science/api/pith-number/PLSYDJ2JQP4I5CMLWU22545EDW/graph.json","events_json":"https://pith.science/api/pith-number/PLSYDJ2JQP4I5CMLWU22545EDW/events.json","paper":"https://pith.science/paper/PLSYDJ2J"},"agent_actions":{"view_html":"https://pith.science/pith/PLSYDJ2JQP4I5CMLWU22545EDW","download_json":"https://pith.science/pith/PLSYDJ2JQP4I5CMLWU22545EDW.json","view_paper":"https://pith.science/paper/PLSYDJ2J","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1410.4557&json=true","fetch_graph":"https://pith.science/api/pith-number/PLSYDJ2JQP4I5CMLWU22545EDW/graph.json","fetch_events":"https://pith.science/api/pith-number/PLSYDJ2JQP4I5CMLWU22545EDW/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/PLSYDJ2JQP4I5CMLWU22545EDW/action/timestamp_anchor","attest_storage":"https://pith.science/pith/PLSYDJ2JQP4I5CMLWU22545EDW/action/storage_attestation","attest_author":"https://pith.science/pith/PLSYDJ2JQP4I5CMLWU22545EDW/action/author_attestation","sign_citation":"https://pith.science/pith/PLSYDJ2JQP4I5CMLWU22545EDW/action/citation_signature","submit_replication":"https://pith.science/pith/PLSYDJ2JQP4I5CMLWU22545EDW/action/replication_record"}},"created_at":"2026-05-18T02:31:20.505291+00:00","updated_at":"2026-05-18T02:31:20.505291+00:00"}