{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2019:QRRRFSCQRHWSZ3OPXGCBXZXG4H","short_pith_number":"pith:QRRRFSCQ","schema_version":"1.0","canonical_sha256":"846312c85089ed2cedcfb9841be6e6e1c63bf48a0934a8e4186ffd56759d2384","source":{"kind":"arxiv","id":"1903.04995","version":1},"attestation_state":"computed","paper":{"title":"Nuclear timescale mass transfer in models of supergiant and ultra-luminous X-ray binaries","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"astro-ph.SR","authors_text":"Martin Quast, Norbert Langer, Thomas M. Tauris","submitted_at":"2019-03-12T15:29:08Z","abstract_excerpt":"We investigate how the proximity of supergiant donor stars to the Eddington-limit, and their advanced evolutionary stage, may influence the evolution of massive and ultra-luminous X-ray binaries with supergiant donor stars (SGXBs and ULXs). We construct models of massive stars with different internal hydrogen/helium gradients and different hydrogen-rich envelope masses, and expose them to slow mass loss to probe the response of the stellar radius. In addition, we compute the corresponding Roche-lobe overflow mass-transfer evolution with our detailed binary stellar evolution code, approximating"},"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":"1903.04995","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2019-03-12T15:29:08Z","cross_cats_sorted":["astro-ph.HE"],"title_canon_sha256":"41cf23436c5e384b21f66f4c84c62cf5e82ae85594ad92be99bf780e6f5c42f9","abstract_canon_sha256":"5a71d3bb493a5966c675ea93df46b9166f071201e88e398d96bd6db9c1e25df8"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T23:50:37.856440Z","signature_b64":"YfDRaCo85HtnEohicLCzg7+TU/9qvQ5nzMgUfVC8odSaSmmsCXvN80Q62dOzPqPjWsdEWDftkC3izPPyUjgXDQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"846312c85089ed2cedcfb9841be6e6e1c63bf48a0934a8e4186ffd56759d2384","last_reissued_at":"2026-07-04T23:50:37.855953Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T23:50:37.855953Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Nuclear timescale mass transfer in models of supergiant and ultra-luminous X-ray binaries","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"astro-ph.SR","authors_text":"Martin Quast, Norbert Langer, Thomas M. Tauris","submitted_at":"2019-03-12T15:29:08Z","abstract_excerpt":"We investigate how the proximity of supergiant donor stars to the Eddington-limit, and their advanced evolutionary stage, may influence the evolution of massive and ultra-luminous X-ray binaries with supergiant donor stars (SGXBs and ULXs). We construct models of massive stars with different internal hydrogen/helium gradients and different hydrogen-rich envelope masses, and expose them to slow mass loss to probe the response of the stellar radius. In addition, we compute the corresponding Roche-lobe overflow mass-transfer evolution with our detailed binary stellar evolution code, approximating"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1903.04995","kind":"arxiv","version":1},"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/1903.04995/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":"1903.04995","created_at":"2026-07-04T23:50:37.856010+00:00"},{"alias_kind":"arxiv_version","alias_value":"1903.04995v1","created_at":"2026-07-04T23:50:37.856010+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1903.04995","created_at":"2026-07-04T23:50:37.856010+00:00"},{"alias_kind":"pith_short_12","alias_value":"QRRRFSCQRHWS","created_at":"2026-07-04T23:50:37.856010+00:00"},{"alias_kind":"pith_short_16","alias_value":"QRRRFSCQRHWSZ3OP","created_at":"2026-07-04T23:50:37.856010+00:00"},{"alias_kind":"pith_short_8","alias_value":"QRRRFSCQ","created_at":"2026-07-04T23:50:37.856010+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"1909.02171","citing_title":"Discovery of a red supergiant donor star in SN2010da/NGC 300 ULX-1","ref_index":42,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/QRRRFSCQRHWSZ3OPXGCBXZXG4H","json":"https://pith.science/pith/QRRRFSCQRHWSZ3OPXGCBXZXG4H.json","graph_json":"https://pith.science/api/pith-number/QRRRFSCQRHWSZ3OPXGCBXZXG4H/graph.json","events_json":"https://pith.science/api/pith-number/QRRRFSCQRHWSZ3OPXGCBXZXG4H/events.json","paper":"https://pith.science/paper/QRRRFSCQ"},"agent_actions":{"view_html":"https://pith.science/pith/QRRRFSCQRHWSZ3OPXGCBXZXG4H","download_json":"https://pith.science/pith/QRRRFSCQRHWSZ3OPXGCBXZXG4H.json","view_paper":"https://pith.science/paper/QRRRFSCQ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1903.04995&json=true","fetch_graph":"https://pith.science/api/pith-number/QRRRFSCQRHWSZ3OPXGCBXZXG4H/graph.json","fetch_events":"https://pith.science/api/pith-number/QRRRFSCQRHWSZ3OPXGCBXZXG4H/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/QRRRFSCQRHWSZ3OPXGCBXZXG4H/action/timestamp_anchor","attest_storage":"https://pith.science/pith/QRRRFSCQRHWSZ3OPXGCBXZXG4H/action/storage_attestation","attest_author":"https://pith.science/pith/QRRRFSCQRHWSZ3OPXGCBXZXG4H/action/author_attestation","sign_citation":"https://pith.science/pith/QRRRFSCQRHWSZ3OPXGCBXZXG4H/action/citation_signature","submit_replication":"https://pith.science/pith/QRRRFSCQRHWSZ3OPXGCBXZXG4H/action/replication_record"}},"created_at":"2026-07-04T23:50:37.856010+00:00","updated_at":"2026-07-04T23:50:37.856010+00:00"}