{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2025:U7KFEBLBQ5VHQM7L2IPMTIWVXT","short_pith_number":"pith:U7KFEBLB","schema_version":"1.0","canonical_sha256":"a7d4520561876a7833ebd21ec9a2d5bceecc5f6ea2f97ce49e3bb14e37f73c09","source":{"kind":"arxiv","id":"2502.17240","version":2},"attestation_state":"computed","paper":{"title":"Gray-body factors: Method matters","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO","hep-ph","hep-th"],"primary_cat":"gr-qc","authors_text":"Alexandre Arbey, Marco Calz\\`a, Yuber F. Perez-Gonzalez","submitted_at":"2025-02-24T15:17:08Z","abstract_excerpt":"The calculation of gray-body factors is essential for understanding Hawking radiation and black hole thermodynamics. While the formalism developed by Chandrasekhar is effective for static black holes, it faces significant challenges in Kerr spacetimes, particularly in the superradiant regime, where a specific choice of coordinates introduces numerical inaccuracies. To address these limitations, an alternative method based on re-scaling radial coordinates and employing Frobenius-like expansions has been investigated. We compare the gray-body factors obtained for a near-maximally rotating black "},"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":"2502.17240","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"gr-qc","submitted_at":"2025-02-24T15:17:08Z","cross_cats_sorted":["astro-ph.CO","hep-ph","hep-th"],"title_canon_sha256":"f0e544de5f47c0c28caf24ff18d42bc21b3154279439e98981e303a61f98a771","abstract_canon_sha256":"a023c3b7e6ec72126969a1c40f2a4a70535df9c8464e7521511df507697338d2"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T10:41:52.769077Z","signature_b64":"HJkWqqsD/JqzOBvaXptxk2ZR99k70HBg39PJI0/Jk/ESwDTLITHs/sjynu5/yjxSyaEJPHE/fs6qgRrgwUmODA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"a7d4520561876a7833ebd21ec9a2d5bceecc5f6ea2f97ce49e3bb14e37f73c09","last_reissued_at":"2026-07-05T10:41:52.768533Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T10:41:52.768533Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Gray-body factors: Method matters","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO","hep-ph","hep-th"],"primary_cat":"gr-qc","authors_text":"Alexandre Arbey, Marco Calz\\`a, Yuber F. Perez-Gonzalez","submitted_at":"2025-02-24T15:17:08Z","abstract_excerpt":"The calculation of gray-body factors is essential for understanding Hawking radiation and black hole thermodynamics. While the formalism developed by Chandrasekhar is effective for static black holes, it faces significant challenges in Kerr spacetimes, particularly in the superradiant regime, where a specific choice of coordinates introduces numerical inaccuracies. To address these limitations, an alternative method based on re-scaling radial coordinates and employing Frobenius-like expansions has been investigated. We compare the gray-body factors obtained for a near-maximally rotating black "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2502.17240","kind":"arxiv","version":2},"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/2502.17240/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":"2502.17240","created_at":"2026-07-05T10:41:52.768594+00:00"},{"alias_kind":"arxiv_version","alias_value":"2502.17240v2","created_at":"2026-07-05T10:41:52.768594+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2502.17240","created_at":"2026-07-05T10:41:52.768594+00:00"},{"alias_kind":"pith_short_12","alias_value":"U7KFEBLBQ5VH","created_at":"2026-07-05T10:41:52.768594+00:00"},{"alias_kind":"pith_short_16","alias_value":"U7KFEBLBQ5VHQM7L","created_at":"2026-07-05T10:41:52.768594+00:00"},{"alias_kind":"pith_short_8","alias_value":"U7KFEBLB","created_at":"2026-07-05T10:41:52.768594+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":3,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2606.08351","citing_title":"Hawking Emission from Black Holes Evaporating toward Wormholes and the Accuracy of the WKB Approximation","ref_index":23,"is_internal_anchor":false},{"citing_arxiv_id":"2606.06355","citing_title":"$\\tt BlackHawk$ $\\tt v3.0$: Hawking Radiation from Regular Black Holes","ref_index":254,"is_internal_anchor":false},{"citing_arxiv_id":"2512.23510","citing_title":"Quasinormal mode/grey-body factor correspondence for Kerr black holes","ref_index":60,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/U7KFEBLBQ5VHQM7L2IPMTIWVXT","json":"https://pith.science/pith/U7KFEBLBQ5VHQM7L2IPMTIWVXT.json","graph_json":"https://pith.science/api/pith-number/U7KFEBLBQ5VHQM7L2IPMTIWVXT/graph.json","events_json":"https://pith.science/api/pith-number/U7KFEBLBQ5VHQM7L2IPMTIWVXT/events.json","paper":"https://pith.science/paper/U7KFEBLB"},"agent_actions":{"view_html":"https://pith.science/pith/U7KFEBLBQ5VHQM7L2IPMTIWVXT","download_json":"https://pith.science/pith/U7KFEBLBQ5VHQM7L2IPMTIWVXT.json","view_paper":"https://pith.science/paper/U7KFEBLB","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2502.17240&json=true","fetch_graph":"https://pith.science/api/pith-number/U7KFEBLBQ5VHQM7L2IPMTIWVXT/graph.json","fetch_events":"https://pith.science/api/pith-number/U7KFEBLBQ5VHQM7L2IPMTIWVXT/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/U7KFEBLBQ5VHQM7L2IPMTIWVXT/action/timestamp_anchor","attest_storage":"https://pith.science/pith/U7KFEBLBQ5VHQM7L2IPMTIWVXT/action/storage_attestation","attest_author":"https://pith.science/pith/U7KFEBLBQ5VHQM7L2IPMTIWVXT/action/author_attestation","sign_citation":"https://pith.science/pith/U7KFEBLBQ5VHQM7L2IPMTIWVXT/action/citation_signature","submit_replication":"https://pith.science/pith/U7KFEBLBQ5VHQM7L2IPMTIWVXT/action/replication_record"}},"created_at":"2026-07-05T10:41:52.768594+00:00","updated_at":"2026-07-05T10:41:52.768594+00:00"}