{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2003:2WIK3Y42GDHKUG4CAVUWY33VO3","short_pith_number":"pith:2WIK3Y42","schema_version":"1.0","canonical_sha256":"d590ade39a30ceaa1b8205696c6f7576c42761f1258ba066df8afd37fd998edd","source":{"kind":"arxiv","id":"gr-qc/0303052","version":6},"attestation_state":"computed","paper":{"title":"Quasinormal behavior of the D-dimensional Schwarzshild black hole and higher order WKB approach","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"gr-qc","authors_text":"R.A.Konoplya","submitted_at":"2003-03-12T17:16:55Z","abstract_excerpt":"We study characteristic (quasinormal) modes of a $D$-dimensional Schwarzshild black hole. It proves out that the real parts of the complex quasinormal modes, representing the real oscillation frequencies, are proportional to the product of the number of dimensions and inverse horizon radius $\\sim D r_{0}^{-1}$. The asymptotic formula for large multipole number $l$ and arbitrary $D$ is derived. In addition the WKB formula for computing QN modes, developed to the 3rd order beyond the eikonal approximation, is extended to the 6th order here. This gives us an accurate and economic way to compute q"},"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":"gr-qc/0303052","kind":"arxiv","version":6},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"gr-qc","submitted_at":"2003-03-12T17:16:55Z","cross_cats_sorted":[],"title_canon_sha256":"e9d7fcaa9fd48b2453dbb0e68ca5acb51fc79da38d93c6ce874ff6756d233b4c","abstract_canon_sha256":"c7e2382f0594c9b132fe77fbd71e55bfd6862b7af9b7d6ce6f39dc7d30d51913"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:19:31.373646Z","signature_b64":"cg9Ms4OA1mPwLf8vDIZLulLtD7tvG5QnSzuuf19UMYJreEG1EofmYUo5yon2+k6D+FrxEIoss/jrWhKa5cT/CQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"d590ade39a30ceaa1b8205696c6f7576c42761f1258ba066df8afd37fd998edd","last_reissued_at":"2026-05-18T00:19:31.373052Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:19:31.373052Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Quasinormal behavior of the D-dimensional Schwarzshild black hole and higher order WKB approach","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"gr-qc","authors_text":"R.A.Konoplya","submitted_at":"2003-03-12T17:16:55Z","abstract_excerpt":"We study characteristic (quasinormal) modes of a $D$-dimensional Schwarzshild black hole. It proves out that the real parts of the complex quasinormal modes, representing the real oscillation frequencies, are proportional to the product of the number of dimensions and inverse horizon radius $\\sim D r_{0}^{-1}$. The asymptotic formula for large multipole number $l$ and arbitrary $D$ is derived. In addition the WKB formula for computing QN modes, developed to the 3rd order beyond the eikonal approximation, is extended to the 6th order here. This gives us an accurate and economic way to compute q"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"gr-qc/0303052","kind":"arxiv","version":6},"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":"gr-qc/0303052","created_at":"2026-05-18T00:19:31.373130+00:00"},{"alias_kind":"arxiv_version","alias_value":"gr-qc/0303052v6","created_at":"2026-05-18T00:19:31.373130+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.gr-qc/0303052","created_at":"2026-05-18T00:19:31.373130+00:00"},{"alias_kind":"pith_short_12","alias_value":"2WIK3Y42GDHK","created_at":"2026-05-18T12:25:51.375804+00:00"},{"alias_kind":"pith_short_16","alias_value":"2WIK3Y42GDHKUG4C","created_at":"2026-05-18T12:25:51.375804+00:00"},{"alias_kind":"pith_short_8","alias_value":"2WIK3Y42","created_at":"2026-05-18T12:25:51.375804+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":31,"internal_anchor_count":16,"sample":[{"citing_arxiv_id":"2601.22340","citing_title":"Grey-body factors of higher dimensional regular black holes in quasi-topological theories","ref_index":86,"is_internal_anchor":true},{"citing_arxiv_id":"2601.22340","citing_title":"Grey-body factors of higher dimensional regular black holes in quasi-topological theories","ref_index":86,"is_internal_anchor":true},{"citing_arxiv_id":"2603.19168","citing_title":"Quasinormal Modes of Extremal Reissner-Nordstrom Black Holes via Seiberg-Witten Quantization","ref_index":25,"is_internal_anchor":true},{"citing_arxiv_id":"2605.14528","citing_title":"Quasinormal modes of massless scalar and electromagnetic perturbations for Euler-Heisenberg black holes surrounded by perfect fluid dark matter","ref_index":22,"is_internal_anchor":true},{"citing_arxiv_id":"2506.16217","citing_title":"Quasinormal modes and grey-body factors of axial gravitational perturbations of regular black holes in asymptotically safe gravity","ref_index":61,"is_internal_anchor":true},{"citing_arxiv_id":"2510.27320","citing_title":"The quasinormal modes of the rotating quantum corrected black holes","ref_index":62,"is_internal_anchor":true},{"citing_arxiv_id":"2512.17786","citing_title":"Quasinormal modes of rotating black holes beyond general relativity in the WKB approximation","ref_index":45,"is_internal_anchor":true},{"citing_arxiv_id":"2512.23510","citing_title":"Quasinormal mode/grey-body factor correspondence for Kerr black holes","ref_index":67,"is_internal_anchor":true},{"citing_arxiv_id":"2601.17906","citing_title":"Telling tails and quasi-resonances in the vicinity of Dymnikova regular black hole","ref_index":146,"is_internal_anchor":true},{"citing_arxiv_id":"2601.18613","citing_title":"Correspondence between quasinormal modes and grey-body factors of Schwarzschild--Tangherlini black holes","ref_index":23,"is_internal_anchor":true},{"citing_arxiv_id":"2602.06947","citing_title":"The gravitational Compton amplitude at third post-Minkowskian order","ref_index":151,"is_internal_anchor":true},{"citing_arxiv_id":"2602.11001","citing_title":"Two types of quasinormal modes of Casadio-Fabbri-Mazzacurati brane-world black holes","ref_index":95,"is_internal_anchor":true},{"citing_arxiv_id":"2602.16972","citing_title":"Anomalous Decay Rate and Greybody Factors for Regular Black Holes with Scalar Hair","ref_index":56,"is_internal_anchor":true},{"citing_arxiv_id":"2603.10844","citing_title":"Long-lived quasinormal modes, shadows and particle motion in four-dimensional quasi-topological gravity","ref_index":175,"is_internal_anchor":true},{"citing_arxiv_id":"2605.14528","citing_title":"Quasinormal modes of massless scalar and electromagnetic perturbations for Euler-Heisenberg black holes surrounded by perfect fluid dark matter","ref_index":22,"is_internal_anchor":true},{"citing_arxiv_id":"2604.24349","citing_title":"Scalar, electromagnetic, and Dirac perturbations of regular black holes constituting primordial dark matter","ref_index":76,"is_internal_anchor":true},{"citing_arxiv_id":"2605.12113","citing_title":"Quasinormal Spectra of Fields of Various Spin in Asymptotically de Sitter Black Holes within Generalized Proca Theory","ref_index":40,"is_internal_anchor":false},{"citing_arxiv_id":"2605.11364","citing_title":"Bardeen spacetime as quantum corrected black hole: Grey-body factors and quasinormal modes of gravitational perturbations","ref_index":69,"is_internal_anchor":false},{"citing_arxiv_id":"1102.4014","citing_title":"Quasinormal modes of black holes: from astrophysics to string theory","ref_index":44,"is_internal_anchor":false},{"citing_arxiv_id":"2605.11013","citing_title":"Massive Scalar Quasinormal Modes, Greybody Factors, and Absorption Cross Section of a Parity-Symmetric Beyond-Horndeski Black Hole","ref_index":102,"is_internal_anchor":false},{"citing_arxiv_id":"2605.03137","citing_title":"Scattering of scalar, electromagnetic, and Dirac fields in an asymptotically flat regular black hole supported by primordial dark matter","ref_index":57,"is_internal_anchor":false},{"citing_arxiv_id":"2605.03659","citing_title":"Long-lived massive scalar modes, grey-body factors, and absorption cross sections of the Reissner--Nordstr\\\"om-like brane-world black hole","ref_index":59,"is_internal_anchor":false},{"citing_arxiv_id":"2604.14999","citing_title":"A First-Order Eikonal Framework for Quasinormal Modes, Shadows, Strong Lensing, and Grey-Body Factors in a Scalarized Black-Hole Metric","ref_index":68,"is_internal_anchor":false},{"citing_arxiv_id":"2505.23895","citing_title":"Black hole spectroscopy: from theory to experiment","ref_index":221,"is_internal_anchor":false},{"citing_arxiv_id":"0905.2975","citing_title":"Quasinormal modes of black holes and black branes","ref_index":217,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/2WIK3Y42GDHKUG4CAVUWY33VO3","json":"https://pith.science/pith/2WIK3Y42GDHKUG4CAVUWY33VO3.json","graph_json":"https://pith.science/api/pith-number/2WIK3Y42GDHKUG4CAVUWY33VO3/graph.json","events_json":"https://pith.science/api/pith-number/2WIK3Y42GDHKUG4CAVUWY33VO3/events.json","paper":"https://pith.science/paper/2WIK3Y42"},"agent_actions":{"view_html":"https://pith.science/pith/2WIK3Y42GDHKUG4CAVUWY33VO3","download_json":"https://pith.science/pith/2WIK3Y42GDHKUG4CAVUWY33VO3.json","view_paper":"https://pith.science/paper/2WIK3Y42","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=gr-qc/0303052&json=true","fetch_graph":"https://pith.science/api/pith-number/2WIK3Y42GDHKUG4CAVUWY33VO3/graph.json","fetch_events":"https://pith.science/api/pith-number/2WIK3Y42GDHKUG4CAVUWY33VO3/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/2WIK3Y42GDHKUG4CAVUWY33VO3/action/timestamp_anchor","attest_storage":"https://pith.science/pith/2WIK3Y42GDHKUG4CAVUWY33VO3/action/storage_attestation","attest_author":"https://pith.science/pith/2WIK3Y42GDHKUG4CAVUWY33VO3/action/author_attestation","sign_citation":"https://pith.science/pith/2WIK3Y42GDHKUG4CAVUWY33VO3/action/citation_signature","submit_replication":"https://pith.science/pith/2WIK3Y42GDHKUG4CAVUWY33VO3/action/replication_record"}},"created_at":"2026-05-18T00:19:31.373130+00:00","updated_at":"2026-05-18T00:19:31.373130+00:00"}