{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2002:NSAEWH2SVQGUCOWO2VPQEJTR47","short_pith_number":"pith:NSAEWH2S","schema_version":"1.0","canonical_sha256":"6c804b1f52ac0d413aced55f022671e7d1d5abfc22b10b6f0b0e9d98382fa722","source":{"kind":"arxiv","id":"astro-ph/0205257","version":1},"attestation_state":"computed","paper":{"title":"A simple model for magnetic reconnection heated corona","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"B. F. Liu (1), K. Shibata (2) ((1)Yukawa Institute for Theoretical Physics, Kyoto Univ.), Kyoto Univ. (2)Kwasan Observatory, S. Mineshige (1)","submitted_at":"2002-05-16T11:37:42Z","abstract_excerpt":"We construct a simple model for a magnetic reconnection heated corona above a thin accretion disk in AGNs and Galactic black hole candidates(GBHCs). The basic assumptions are that (1) the magnetic reconnection heat is cooled down overwhelmingly by Compton scattering in the corona and that (2) thermal conduction is dominantly cooled by evaporation of the chromospheric plasma in the disk-corona interface before Compton cooling sets in. With these two basic equations as well as equi-partition of magnetic energy with gas energy in the disk, we can consistently determine the fraction of accretion e"},"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":"astro-ph/0205257","kind":"arxiv","version":1},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2002-05-16T11:37:42Z","cross_cats_sorted":[],"title_canon_sha256":"6431530b5ec1060d80b3be93eae829f6b79118dd61e5e6a1662cc3c203654fe8","abstract_canon_sha256":"0a64e129f30284024887b0333228141ab5ca83fa10a88b737b283dd4bd19e78e"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T16:30:01.382254Z","signature_b64":"pX35gaNTuniaFPRTv9EWxngxn+bN+iVssv2AhKqzZGX4I8O/RfJGl/fVuPoXcSbuKwY/3HrIQI7DFNPM4quoDA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"6c804b1f52ac0d413aced55f022671e7d1d5abfc22b10b6f0b0e9d98382fa722","last_reissued_at":"2026-07-04T16:30:01.381844Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T16:30:01.381844Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"A simple model for magnetic reconnection heated corona","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"B. F. Liu (1), K. Shibata (2) ((1)Yukawa Institute for Theoretical Physics, Kyoto Univ.), Kyoto Univ. (2)Kwasan Observatory, S. Mineshige (1)","submitted_at":"2002-05-16T11:37:42Z","abstract_excerpt":"We construct a simple model for a magnetic reconnection heated corona above a thin accretion disk in AGNs and Galactic black hole candidates(GBHCs). The basic assumptions are that (1) the magnetic reconnection heat is cooled down overwhelmingly by Compton scattering in the corona and that (2) thermal conduction is dominantly cooled by evaporation of the chromospheric plasma in the disk-corona interface before Compton cooling sets in. With these two basic equations as well as equi-partition of magnetic energy with gas energy in the disk, we can consistently determine the fraction of accretion e"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0205257","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/astro-ph/0205257/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":"astro-ph/0205257","created_at":"2026-07-04T16:30:01.381904+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/0205257v1","created_at":"2026-07-04T16:30:01.381904+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/0205257","created_at":"2026-07-04T16:30:01.381904+00:00"},{"alias_kind":"pith_short_12","alias_value":"NSAEWH2SVQGU","created_at":"2026-07-04T16:30:01.381904+00:00"},{"alias_kind":"pith_short_16","alias_value":"NSAEWH2SVQGUCOWO","created_at":"2026-07-04T16:30:01.381904+00:00"},{"alias_kind":"pith_short_8","alias_value":"NSAEWH2S","created_at":"2026-07-04T16:30:01.381904+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":2,"sample":[{"citing_arxiv_id":"2607.01604","citing_title":"Bolometric correction factor and radiative efficiency for the super-Eddington accretion flow in tidal disruption events","ref_index":92,"is_internal_anchor":true},{"citing_arxiv_id":"2410.12638","citing_title":"Neutrino and pair creation in reconnection-powered coronae of accreting black holes","ref_index":5,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/NSAEWH2SVQGUCOWO2VPQEJTR47","json":"https://pith.science/pith/NSAEWH2SVQGUCOWO2VPQEJTR47.json","graph_json":"https://pith.science/api/pith-number/NSAEWH2SVQGUCOWO2VPQEJTR47/graph.json","events_json":"https://pith.science/api/pith-number/NSAEWH2SVQGUCOWO2VPQEJTR47/events.json","paper":"https://pith.science/paper/NSAEWH2S"},"agent_actions":{"view_html":"https://pith.science/pith/NSAEWH2SVQGUCOWO2VPQEJTR47","download_json":"https://pith.science/pith/NSAEWH2SVQGUCOWO2VPQEJTR47.json","view_paper":"https://pith.science/paper/NSAEWH2S","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/0205257&json=true","fetch_graph":"https://pith.science/api/pith-number/NSAEWH2SVQGUCOWO2VPQEJTR47/graph.json","fetch_events":"https://pith.science/api/pith-number/NSAEWH2SVQGUCOWO2VPQEJTR47/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/NSAEWH2SVQGUCOWO2VPQEJTR47/action/timestamp_anchor","attest_storage":"https://pith.science/pith/NSAEWH2SVQGUCOWO2VPQEJTR47/action/storage_attestation","attest_author":"https://pith.science/pith/NSAEWH2SVQGUCOWO2VPQEJTR47/action/author_attestation","sign_citation":"https://pith.science/pith/NSAEWH2SVQGUCOWO2VPQEJTR47/action/citation_signature","submit_replication":"https://pith.science/pith/NSAEWH2SVQGUCOWO2VPQEJTR47/action/replication_record"}},"created_at":"2026-07-04T16:30:01.381904+00:00","updated_at":"2026-07-04T16:30:01.381904+00:00"}