{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2017:JULSPJECA44E5VLJD2VKM5L2FQ","short_pith_number":"pith:JULSPJEC","schema_version":"1.0","canonical_sha256":"4d1727a48207384ed5691eaaa6757a2c07fcd5eb8dfe845630d957dc4114c419","source":{"kind":"arxiv","id":"1710.08890","version":1},"attestation_state":"computed","paper":{"title":"Population III X-Ray Binaries","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Rosalba Perna, Taeho Ryu, Takamitsu L. Tanaka","submitted_at":"2017-10-24T16:52:40Z","abstract_excerpt":"Understanding of the role of X-rays for driving the thermal evolution of the intergalactic medium (IGM) at high redshifts is one of important questions in astrophysics. High-mass X-ray binaries (HMXBs) in early stellar populations are prime X-ray source; however, their formation efficiency is not well understood. Using $N$-body simulations, we estimate the HMXB formation rate via mutual gravitational interactions of nascent, small groups of the Population~III stars. We find that HMXBs form at a rate of one per $\\gtrsim 10^{4}M_{\\odot}$ in newly born stars, and that they emit with a power of $\\"},"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":"1710.08890","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2017-10-24T16:52:40Z","cross_cats_sorted":[],"title_canon_sha256":"bbbcb4c868fe3883b4479088aec83df50aa4d7fd0e0110b15f84dcfb004a2ea2","abstract_canon_sha256":"681afdd404567c534d4e9465b80f65bae8da8512360090ca011967e60be2b65f"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:32:03.496078Z","signature_b64":"ViINzmHO/a1H/wgHlZtGJEL/Npe2E9NCGsLwXqnYtzTdHsNKQe6uQTl7b7vTKfgP7RUr44FuG7MSg1CAvNjfCw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"4d1727a48207384ed5691eaaa6757a2c07fcd5eb8dfe845630d957dc4114c419","last_reissued_at":"2026-05-18T00:32:03.495547Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:32:03.495547Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Population III X-Ray Binaries","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Rosalba Perna, Taeho Ryu, Takamitsu L. Tanaka","submitted_at":"2017-10-24T16:52:40Z","abstract_excerpt":"Understanding of the role of X-rays for driving the thermal evolution of the intergalactic medium (IGM) at high redshifts is one of important questions in astrophysics. High-mass X-ray binaries (HMXBs) in early stellar populations are prime X-ray source; however, their formation efficiency is not well understood. Using $N$-body simulations, we estimate the HMXB formation rate via mutual gravitational interactions of nascent, small groups of the Population~III stars. We find that HMXBs form at a rate of one per $\\gtrsim 10^{4}M_{\\odot}$ in newly born stars, and that they emit with a power of $\\"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1710.08890","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":"1710.08890","created_at":"2026-05-18T00:32:03.495637+00:00"},{"alias_kind":"arxiv_version","alias_value":"1710.08890v1","created_at":"2026-05-18T00:32:03.495637+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1710.08890","created_at":"2026-05-18T00:32:03.495637+00:00"},{"alias_kind":"pith_short_12","alias_value":"JULSPJECA44E","created_at":"2026-05-18T12:31:24.725408+00:00"},{"alias_kind":"pith_short_16","alias_value":"JULSPJECA44E5VLJ","created_at":"2026-05-18T12:31:24.725408+00:00"},{"alias_kind":"pith_short_8","alias_value":"JULSPJEC","created_at":"2026-05-18T12:31:24.725408+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/JULSPJECA44E5VLJD2VKM5L2FQ","json":"https://pith.science/pith/JULSPJECA44E5VLJD2VKM5L2FQ.json","graph_json":"https://pith.science/api/pith-number/JULSPJECA44E5VLJD2VKM5L2FQ/graph.json","events_json":"https://pith.science/api/pith-number/JULSPJECA44E5VLJD2VKM5L2FQ/events.json","paper":"https://pith.science/paper/JULSPJEC"},"agent_actions":{"view_html":"https://pith.science/pith/JULSPJECA44E5VLJD2VKM5L2FQ","download_json":"https://pith.science/pith/JULSPJECA44E5VLJD2VKM5L2FQ.json","view_paper":"https://pith.science/paper/JULSPJEC","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1710.08890&json=true","fetch_graph":"https://pith.science/api/pith-number/JULSPJECA44E5VLJD2VKM5L2FQ/graph.json","fetch_events":"https://pith.science/api/pith-number/JULSPJECA44E5VLJD2VKM5L2FQ/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/JULSPJECA44E5VLJD2VKM5L2FQ/action/timestamp_anchor","attest_storage":"https://pith.science/pith/JULSPJECA44E5VLJD2VKM5L2FQ/action/storage_attestation","attest_author":"https://pith.science/pith/JULSPJECA44E5VLJD2VKM5L2FQ/action/author_attestation","sign_citation":"https://pith.science/pith/JULSPJECA44E5VLJD2VKM5L2FQ/action/citation_signature","submit_replication":"https://pith.science/pith/JULSPJECA44E5VLJD2VKM5L2FQ/action/replication_record"}},"created_at":"2026-05-18T00:32:03.495637+00:00","updated_at":"2026-05-18T00:32:03.495637+00:00"}