{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2021:A5FYHSHAD2EYDUVEW3OAM7G6GA","short_pith_number":"pith:A5FYHSHA","schema_version":"1.0","canonical_sha256":"074b83c8e01e8981d2a4b6dc067cde300770d6d4c41be6f2246b4019105554d2","source":{"kind":"arxiv","id":"2110.01249","version":3},"attestation_state":"computed","paper":{"title":"A physical model for the broadband energy spectrum of X-ray illuminated accretion discs: fitting the spectral energy distribution of NGC 5548","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"E. S. Kammoun, I. E. Papadakis, M. Dovciak, W. Zhang","submitted_at":"2021-10-04T08:34:50Z","abstract_excerpt":"We develop a new physical model for the broadband spectral energy distribution (SED) of X-ray illuminated accretion discs, that takes into account the mutual interaction of the accretion disc and the X-ray corona, including all relativistic effects. We assume a Keplerian, optically thick and geometrically thin accretion disc and an X-ray source in the lamp-post geometry that emits an isotropic power-law spectrum with a high-energy cut-off. We assume that all the energy that would be released by thermal radiation in the standard disc model in its innermost part, is transported to the corona, ef"},"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":"2110.01249","kind":"arxiv","version":3},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2021-10-04T08:34:50Z","cross_cats_sorted":[],"title_canon_sha256":"1bc5441720df17f490e726cf43a0fc0f5228aab3e72dcc73d450af4d007ed4d8","abstract_canon_sha256":"1d07b802e5aaca12ea42eaa18cc32d17a0d404f7e2b1b013ef1990f6f7fdc21e"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T04:25:46.402567Z","signature_b64":"xQeiFyHFybF3oy5Qe7xdeDF7KKzXjyuaJX4uuC8pI6cpL/nPF1w8xxyEEL6yhGgoNogxsPd+Xq6eN4xM/BmoAA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"074b83c8e01e8981d2a4b6dc067cde300770d6d4c41be6f2246b4019105554d2","last_reissued_at":"2026-07-05T04:25:46.402110Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T04:25:46.402110Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"A physical model for the broadband energy spectrum of X-ray illuminated accretion discs: fitting the spectral energy distribution of NGC 5548","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"E. S. Kammoun, I. E. Papadakis, M. Dovciak, W. Zhang","submitted_at":"2021-10-04T08:34:50Z","abstract_excerpt":"We develop a new physical model for the broadband spectral energy distribution (SED) of X-ray illuminated accretion discs, that takes into account the mutual interaction of the accretion disc and the X-ray corona, including all relativistic effects. We assume a Keplerian, optically thick and geometrically thin accretion disc and an X-ray source in the lamp-post geometry that emits an isotropic power-law spectrum with a high-energy cut-off. We assume that all the energy that would be released by thermal radiation in the standard disc model in its innermost part, is transported to the corona, ef"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2110.01249","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/2110.01249/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":"2110.01249","created_at":"2026-07-05T04:25:46.402166+00:00"},{"alias_kind":"arxiv_version","alias_value":"2110.01249v3","created_at":"2026-07-05T04:25:46.402166+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2110.01249","created_at":"2026-07-05T04:25:46.402166+00:00"},{"alias_kind":"pith_short_12","alias_value":"A5FYHSHAD2EY","created_at":"2026-07-05T04:25:46.402166+00:00"},{"alias_kind":"pith_short_16","alias_value":"A5FYHSHAD2EYDUVE","created_at":"2026-07-05T04:25:46.402166+00:00"},{"alias_kind":"pith_short_8","alias_value":"A5FYHSHA","created_at":"2026-07-05T04:25:46.402166+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2607.03291","citing_title":"Physically motivated AGN emissivity profiles and their effects on quasar microlensing signatures. 1. Multi-epoch accretion disc size inference","ref_index":142,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/A5FYHSHAD2EYDUVEW3OAM7G6GA","json":"https://pith.science/pith/A5FYHSHAD2EYDUVEW3OAM7G6GA.json","graph_json":"https://pith.science/api/pith-number/A5FYHSHAD2EYDUVEW3OAM7G6GA/graph.json","events_json":"https://pith.science/api/pith-number/A5FYHSHAD2EYDUVEW3OAM7G6GA/events.json","paper":"https://pith.science/paper/A5FYHSHA"},"agent_actions":{"view_html":"https://pith.science/pith/A5FYHSHAD2EYDUVEW3OAM7G6GA","download_json":"https://pith.science/pith/A5FYHSHAD2EYDUVEW3OAM7G6GA.json","view_paper":"https://pith.science/paper/A5FYHSHA","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2110.01249&json=true","fetch_graph":"https://pith.science/api/pith-number/A5FYHSHAD2EYDUVEW3OAM7G6GA/graph.json","fetch_events":"https://pith.science/api/pith-number/A5FYHSHAD2EYDUVEW3OAM7G6GA/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/A5FYHSHAD2EYDUVEW3OAM7G6GA/action/timestamp_anchor","attest_storage":"https://pith.science/pith/A5FYHSHAD2EYDUVEW3OAM7G6GA/action/storage_attestation","attest_author":"https://pith.science/pith/A5FYHSHAD2EYDUVEW3OAM7G6GA/action/author_attestation","sign_citation":"https://pith.science/pith/A5FYHSHAD2EYDUVEW3OAM7G6GA/action/citation_signature","submit_replication":"https://pith.science/pith/A5FYHSHAD2EYDUVEW3OAM7G6GA/action/replication_record"}},"created_at":"2026-07-05T04:25:46.402166+00:00","updated_at":"2026-07-05T04:25:46.402166+00:00"}