{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2014:P3XCWNAVAMF7GF4LQW7R3BG5XZ","short_pith_number":"pith:P3XCWNAV","schema_version":"1.0","canonical_sha256":"7eee2b3415030bf3178b85bf1d84ddbe60a4f6c40f0bf862da97a76ed2f08ac5","source":{"kind":"arxiv","id":"1410.5109","version":3},"attestation_state":"computed","paper":{"title":"Mass Transfer from Giant Donors","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"astro-ph.SR","authors_text":"K. Pavlovskii, N. Ivanova","submitted_at":"2014-10-19T20:15:44Z","abstract_excerpt":"The stability of mass transfer in binaries with convective giant donors remains an open question in modern astrophysics. There is a significant discrepancy between what the existing methods predict for a response to mass loss of the giant itself, as well as for the mass transfer rate during the Roche lobe overflow. Here we show that the recombination energy in the superadiabatic layer plays an important and hitherto unaccounted-for role in he donor's response to mass loss, in particular on its luminosity and effective temperature. Our improved optically thick nozzle method to calculate the mas"},"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":"1410.5109","kind":"arxiv","version":3},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2014-10-19T20:15:44Z","cross_cats_sorted":["astro-ph.HE"],"title_canon_sha256":"3ed42c0ae436650931f9c014125366e51952c70f07cfc4016f7eab5885d1b3b6","abstract_canon_sha256":"7ee63852923d10b262a4621e74870c432ac179c62561fe84a0b15886635e56ae"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:41:43.692266Z","signature_b64":"eq+p4MbjPTbdU83o266RHfoxVvF3V68N/wqPVHBUSjjkrZMvLTONRUKYfrxc1ZytiAbRL+Fi83JemWQJb+1JBw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"7eee2b3415030bf3178b85bf1d84ddbe60a4f6c40f0bf862da97a76ed2f08ac5","last_reissued_at":"2026-05-18T01:41:43.691647Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:41:43.691647Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Mass Transfer from Giant Donors","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"astro-ph.SR","authors_text":"K. Pavlovskii, N. Ivanova","submitted_at":"2014-10-19T20:15:44Z","abstract_excerpt":"The stability of mass transfer in binaries with convective giant donors remains an open question in modern astrophysics. There is a significant discrepancy between what the existing methods predict for a response to mass loss of the giant itself, as well as for the mass transfer rate during the Roche lobe overflow. Here we show that the recombination energy in the superadiabatic layer plays an important and hitherto unaccounted-for role in he donor's response to mass loss, in particular on its luminosity and effective temperature. Our improved optically thick nozzle method to calculate the mas"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1410.5109","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":"1410.5109","created_at":"2026-05-18T01:41:43.691746+00:00"},{"alias_kind":"arxiv_version","alias_value":"1410.5109v3","created_at":"2026-05-18T01:41:43.691746+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1410.5109","created_at":"2026-05-18T01:41:43.691746+00:00"},{"alias_kind":"pith_short_12","alias_value":"P3XCWNAVAMF7","created_at":"2026-05-18T12:28:43.426989+00:00"},{"alias_kind":"pith_short_16","alias_value":"P3XCWNAVAMF7GF4L","created_at":"2026-05-18T12:28:43.426989+00:00"},{"alias_kind":"pith_short_8","alias_value":"P3XCWNAV","created_at":"2026-05-18T12:28:43.426989+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":2,"sample":[{"citing_arxiv_id":"2605.21580","citing_title":"Massquerade: Impacts of Mass Ratio Reversals on Binary Black Hole Merger Rates and Mass Distributions","ref_index":134,"is_internal_anchor":true},{"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":219,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/P3XCWNAVAMF7GF4LQW7R3BG5XZ","json":"https://pith.science/pith/P3XCWNAVAMF7GF4LQW7R3BG5XZ.json","graph_json":"https://pith.science/api/pith-number/P3XCWNAVAMF7GF4LQW7R3BG5XZ/graph.json","events_json":"https://pith.science/api/pith-number/P3XCWNAVAMF7GF4LQW7R3BG5XZ/events.json","paper":"https://pith.science/paper/P3XCWNAV"},"agent_actions":{"view_html":"https://pith.science/pith/P3XCWNAVAMF7GF4LQW7R3BG5XZ","download_json":"https://pith.science/pith/P3XCWNAVAMF7GF4LQW7R3BG5XZ.json","view_paper":"https://pith.science/paper/P3XCWNAV","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1410.5109&json=true","fetch_graph":"https://pith.science/api/pith-number/P3XCWNAVAMF7GF4LQW7R3BG5XZ/graph.json","fetch_events":"https://pith.science/api/pith-number/P3XCWNAVAMF7GF4LQW7R3BG5XZ/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/P3XCWNAVAMF7GF4LQW7R3BG5XZ/action/timestamp_anchor","attest_storage":"https://pith.science/pith/P3XCWNAVAMF7GF4LQW7R3BG5XZ/action/storage_attestation","attest_author":"https://pith.science/pith/P3XCWNAVAMF7GF4LQW7R3BG5XZ/action/author_attestation","sign_citation":"https://pith.science/pith/P3XCWNAVAMF7GF4LQW7R3BG5XZ/action/citation_signature","submit_replication":"https://pith.science/pith/P3XCWNAVAMF7GF4LQW7R3BG5XZ/action/replication_record"}},"created_at":"2026-05-18T01:41:43.691746+00:00","updated_at":"2026-05-18T01:41:43.691746+00:00"}