{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2016:ZOEHT4XUJGMRV46LFCTEQURFGB","short_pith_number":"pith:ZOEHT4XU","schema_version":"1.0","canonical_sha256":"cb8879f2f449991af3cb28a6485225304d426f7a8e07d8d53c6f348da744c206","source":{"kind":"arxiv","id":"1605.03669","version":1},"attestation_state":"computed","paper":{"title":"Can the Subsonic Accretion Model Explain the Spin Period Distribution of Wind-fed X-ray Pulsars?","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"Tao Li, Xiang-Dong Li (NJU), Yong Shao","submitted_at":"2016-05-12T03:29:36Z","abstract_excerpt":"Neutron stars in high-mass X-ray binaries (HMXBs) generally accrete from the wind matter of their massive companion stars. Recently Shakura et al. (2012) suggested a subsonic accretion model for low-luminosity ($<4\\times 10^{36}$ ergs$^{-1}$), wind-fed X-ray pulsars. To test the feasibility of this model, we investigate the spin period distribution of wind-fed X-ray pulsars with a supergiant companion star, using a population synthesis method. We find that the modeled distribution of supergiant HMXBs in the spin period - orbital period diagram is consistent with observations provided that the "},"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":"1605.03669","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2016-05-12T03:29:36Z","cross_cats_sorted":[],"title_canon_sha256":"0c0e0900f454268a4a91214863f5a5fff34d586274a09a64cebdf565f881eb03","abstract_canon_sha256":"32a16598ee6aa7aafcf888ae4bbf9225b456ae768e51bfcc56ba0c1ea781061f"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:11:47.950193Z","signature_b64":"8RaxgW0x7W4axXnApe+je1P8Qksy8dxn019S0sImN3tXBrNMCo/WWqLxWm1p5bx1ACI+DOU0O8C21IEdRtQQCQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"cb8879f2f449991af3cb28a6485225304d426f7a8e07d8d53c6f348da744c206","last_reissued_at":"2026-05-18T01:11:47.949843Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:11:47.949843Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Can the Subsonic Accretion Model Explain the Spin Period Distribution of Wind-fed X-ray Pulsars?","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"Tao Li, Xiang-Dong Li (NJU), Yong Shao","submitted_at":"2016-05-12T03:29:36Z","abstract_excerpt":"Neutron stars in high-mass X-ray binaries (HMXBs) generally accrete from the wind matter of their massive companion stars. Recently Shakura et al. (2012) suggested a subsonic accretion model for low-luminosity ($<4\\times 10^{36}$ ergs$^{-1}$), wind-fed X-ray pulsars. To test the feasibility of this model, we investigate the spin period distribution of wind-fed X-ray pulsars with a supergiant companion star, using a population synthesis method. We find that the modeled distribution of supergiant HMXBs in the spin period - orbital period diagram is consistent with observations provided that the "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1605.03669","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":""},"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":"1605.03669","created_at":"2026-05-18T01:11:47.949908+00:00"},{"alias_kind":"arxiv_version","alias_value":"1605.03669v1","created_at":"2026-05-18T01:11:47.949908+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1605.03669","created_at":"2026-05-18T01:11:47.949908+00:00"},{"alias_kind":"pith_short_12","alias_value":"ZOEHT4XUJGMR","created_at":"2026-05-18T12:30:55.937587+00:00"},{"alias_kind":"pith_short_16","alias_value":"ZOEHT4XUJGMRV46L","created_at":"2026-05-18T12:30:55.937587+00:00"},{"alias_kind":"pith_short_8","alias_value":"ZOEHT4XU","created_at":"2026-05-18T12:30:55.937587+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":0,"internal_anchor_count":0,"sample":[]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/ZOEHT4XUJGMRV46LFCTEQURFGB","json":"https://pith.science/pith/ZOEHT4XUJGMRV46LFCTEQURFGB.json","graph_json":"https://pith.science/api/pith-number/ZOEHT4XUJGMRV46LFCTEQURFGB/graph.json","events_json":"https://pith.science/api/pith-number/ZOEHT4XUJGMRV46LFCTEQURFGB/events.json","paper":"https://pith.science/paper/ZOEHT4XU"},"agent_actions":{"view_html":"https://pith.science/pith/ZOEHT4XUJGMRV46LFCTEQURFGB","download_json":"https://pith.science/pith/ZOEHT4XUJGMRV46LFCTEQURFGB.json","view_paper":"https://pith.science/paper/ZOEHT4XU","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1605.03669&json=true","fetch_graph":"https://pith.science/api/pith-number/ZOEHT4XUJGMRV46LFCTEQURFGB/graph.json","fetch_events":"https://pith.science/api/pith-number/ZOEHT4XUJGMRV46LFCTEQURFGB/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/ZOEHT4XUJGMRV46LFCTEQURFGB/action/timestamp_anchor","attest_storage":"https://pith.science/pith/ZOEHT4XUJGMRV46LFCTEQURFGB/action/storage_attestation","attest_author":"https://pith.science/pith/ZOEHT4XUJGMRV46LFCTEQURFGB/action/author_attestation","sign_citation":"https://pith.science/pith/ZOEHT4XUJGMRV46LFCTEQURFGB/action/citation_signature","submit_replication":"https://pith.science/pith/ZOEHT4XUJGMRV46LFCTEQURFGB/action/replication_record"}},"created_at":"2026-05-18T01:11:47.949908+00:00","updated_at":"2026-05-18T01:11:47.949908+00:00"}