{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2021:EJGKCU5TPMTP55Z7YWWTSQBNFX","short_pith_number":"pith:EJGKCU5T","schema_version":"1.0","canonical_sha256":"224ca153b37b26fef73fc5ad39402d2dd07b7cb0c1ddcae04bfff776e62ab973","source":{"kind":"arxiv","id":"2102.04066","version":2},"attestation_state":"computed","paper":{"title":"Thermal behavior of a radially deformed black hole spacetime","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"gr-qc","authors_text":"Sajal Mukherjee, Subhajit Barman","submitted_at":"2021-02-08T09:06:31Z","abstract_excerpt":"In the present article, we study the Hawking effect and the bounds on greybody factor in a spacetime with radial deformation. This deformation is expected to carry the imprint of a non-Einsteinian theory of gravity, but shares some of the important characteristics of general relativity (GR). In particular, this radial deformation will restore the asymptotic behavior, and also allows for the separation of the scalar field equation in terms of the angular and radial coordinates -- making it suitable to study the Hawking effect and greybody factors. However, the radial deformation would introduce"},"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":"2102.04066","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"gr-qc","submitted_at":"2021-02-08T09:06:31Z","cross_cats_sorted":[],"title_canon_sha256":"3d04da9401f864c0d6958e103b0a5f3bb7ed60fc0315ee8214a19e268598f1e6","abstract_canon_sha256":"409bd77c5c2650f15d04810f3dbe05aeda7ace715c240cb96186f4d80a901322"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T05:31:42.077422Z","signature_b64":"KFhVab8VzNer0N31xyptLg7B72ol0jqrAsUFJA3NkQk00mO/gNvV7yZ4WiMq3f0b/12BEto7Z8w8ZHgFlh0uCg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"224ca153b37b26fef73fc5ad39402d2dd07b7cb0c1ddcae04bfff776e62ab973","last_reissued_at":"2026-07-05T05:31:42.076913Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T05:31:42.076913Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Thermal behavior of a radially deformed black hole spacetime","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"gr-qc","authors_text":"Sajal Mukherjee, Subhajit Barman","submitted_at":"2021-02-08T09:06:31Z","abstract_excerpt":"In the present article, we study the Hawking effect and the bounds on greybody factor in a spacetime with radial deformation. This deformation is expected to carry the imprint of a non-Einsteinian theory of gravity, but shares some of the important characteristics of general relativity (GR). In particular, this radial deformation will restore the asymptotic behavior, and also allows for the separation of the scalar field equation in terms of the angular and radial coordinates -- making it suitable to study the Hawking effect and greybody factors. However, the radial deformation would introduce"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2102.04066","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/2102.04066/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":"2102.04066","created_at":"2026-07-05T05:31:42.076979+00:00"},{"alias_kind":"arxiv_version","alias_value":"2102.04066v2","created_at":"2026-07-05T05:31:42.076979+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2102.04066","created_at":"2026-07-05T05:31:42.076979+00:00"},{"alias_kind":"pith_short_12","alias_value":"EJGKCU5TPMTP","created_at":"2026-07-05T05:31:42.076979+00:00"},{"alias_kind":"pith_short_16","alias_value":"EJGKCU5TPMTP55Z7","created_at":"2026-07-05T05:31:42.076979+00:00"},{"alias_kind":"pith_short_8","alias_value":"EJGKCU5T","created_at":"2026-07-05T05:31:42.076979+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2601.09607","citing_title":"Confronting eikonal and post-Kerr methods with numerical evolution of scalar field perturbations in spacetimes beyond Kerr","ref_index":58,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/EJGKCU5TPMTP55Z7YWWTSQBNFX","json":"https://pith.science/pith/EJGKCU5TPMTP55Z7YWWTSQBNFX.json","graph_json":"https://pith.science/api/pith-number/EJGKCU5TPMTP55Z7YWWTSQBNFX/graph.json","events_json":"https://pith.science/api/pith-number/EJGKCU5TPMTP55Z7YWWTSQBNFX/events.json","paper":"https://pith.science/paper/EJGKCU5T"},"agent_actions":{"view_html":"https://pith.science/pith/EJGKCU5TPMTP55Z7YWWTSQBNFX","download_json":"https://pith.science/pith/EJGKCU5TPMTP55Z7YWWTSQBNFX.json","view_paper":"https://pith.science/paper/EJGKCU5T","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2102.04066&json=true","fetch_graph":"https://pith.science/api/pith-number/EJGKCU5TPMTP55Z7YWWTSQBNFX/graph.json","fetch_events":"https://pith.science/api/pith-number/EJGKCU5TPMTP55Z7YWWTSQBNFX/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/EJGKCU5TPMTP55Z7YWWTSQBNFX/action/timestamp_anchor","attest_storage":"https://pith.science/pith/EJGKCU5TPMTP55Z7YWWTSQBNFX/action/storage_attestation","attest_author":"https://pith.science/pith/EJGKCU5TPMTP55Z7YWWTSQBNFX/action/author_attestation","sign_citation":"https://pith.science/pith/EJGKCU5TPMTP55Z7YWWTSQBNFX/action/citation_signature","submit_replication":"https://pith.science/pith/EJGKCU5TPMTP55Z7YWWTSQBNFX/action/replication_record"}},"created_at":"2026-07-05T05:31:42.076979+00:00","updated_at":"2026-07-05T05:31:42.076979+00:00"}