{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2012:MLQGS3ELXHIKDVWRP47AJN4IFD","short_pith_number":"pith:MLQGS3EL","schema_version":"1.0","canonical_sha256":"62e0696c8bb9d0a1d6d17f3e04b78828ed85e3964aea3b81505931e6a0ba8c21","source":{"kind":"arxiv","id":"1211.6212","version":2},"attestation_state":"computed","paper":{"title":"Quasinormal modes of regular black holes","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"gr-qc","authors_text":"Antonino Flachi, Jos\\'e P. S. Lemos","submitted_at":"2012-11-27T04:36:39Z","abstract_excerpt":"Black hole quasinormal frequencies are complex numbers that encode information on how a black hole relaxes after it has been perturbed and depend on the features of the geometry and on the type of perturbations. On the one hand, the examples studied so far in the literature focused on the case of black hole geometries with singularities in their interior. On the other hand, it is expected that quantum or classical modifications of general relativity may correct the pathological singular behavior of classical black hole solutions. Despite the fact that we do not have at hand a complete theory o"},"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":"1211.6212","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"gr-qc","submitted_at":"2012-11-27T04:36:39Z","cross_cats_sorted":[],"title_canon_sha256":"201d5084a266ff80fbbd0d283776397a704aa06f37ecf9051a0b56b67266eb61","abstract_canon_sha256":"ddf07050ccea293d34c553e90ebfc46fc82e06270be8446e0bb8a4a54223987d"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:52:54.623279Z","signature_b64":"tFLjVXpJjNZqh12uNRqorOiWkMTkElywGnss2bLCO0g7dlJDRd/FoVIQVld36MeXvrIiQv1e+6tKOe/E0dIqDA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"62e0696c8bb9d0a1d6d17f3e04b78828ed85e3964aea3b81505931e6a0ba8c21","last_reissued_at":"2026-05-18T01:52:54.622659Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:52:54.622659Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Quasinormal modes of regular black holes","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"gr-qc","authors_text":"Antonino Flachi, Jos\\'e P. S. Lemos","submitted_at":"2012-11-27T04:36:39Z","abstract_excerpt":"Black hole quasinormal frequencies are complex numbers that encode information on how a black hole relaxes after it has been perturbed and depend on the features of the geometry and on the type of perturbations. On the one hand, the examples studied so far in the literature focused on the case of black hole geometries with singularities in their interior. On the other hand, it is expected that quantum or classical modifications of general relativity may correct the pathological singular behavior of classical black hole solutions. Despite the fact that we do not have at hand a complete theory o"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1211.6212","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":""},"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":"1211.6212","created_at":"2026-05-18T01:52:54.622745+00:00"},{"alias_kind":"arxiv_version","alias_value":"1211.6212v2","created_at":"2026-05-18T01:52:54.622745+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1211.6212","created_at":"2026-05-18T01:52:54.622745+00:00"},{"alias_kind":"pith_short_12","alias_value":"MLQGS3ELXHIK","created_at":"2026-05-18T12:27:14.488303+00:00"},{"alias_kind":"pith_short_16","alias_value":"MLQGS3ELXHIKDVWR","created_at":"2026-05-18T12:27:14.488303+00:00"},{"alias_kind":"pith_short_8","alias_value":"MLQGS3EL","created_at":"2026-05-18T12:27:14.488303+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":5,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2604.24349","citing_title":"Scalar, electromagnetic, and Dirac perturbations of regular black holes constituting primordial dark matter","ref_index":25,"is_internal_anchor":true},{"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":34,"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":11,"is_internal_anchor":false},{"citing_arxiv_id":"2604.25471","citing_title":"Massive scalar quasinormal modes of an asymptotically flat regular black hole supported by a phantom Dirac--Born--Infeld field","ref_index":105,"is_internal_anchor":false},{"citing_arxiv_id":"2604.24349","citing_title":"Scalar, electromagnetic, and Dirac perturbations of regular black holes constituting primordial dark matter","ref_index":25,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/MLQGS3ELXHIKDVWRP47AJN4IFD","json":"https://pith.science/pith/MLQGS3ELXHIKDVWRP47AJN4IFD.json","graph_json":"https://pith.science/api/pith-number/MLQGS3ELXHIKDVWRP47AJN4IFD/graph.json","events_json":"https://pith.science/api/pith-number/MLQGS3ELXHIKDVWRP47AJN4IFD/events.json","paper":"https://pith.science/paper/MLQGS3EL"},"agent_actions":{"view_html":"https://pith.science/pith/MLQGS3ELXHIKDVWRP47AJN4IFD","download_json":"https://pith.science/pith/MLQGS3ELXHIKDVWRP47AJN4IFD.json","view_paper":"https://pith.science/paper/MLQGS3EL","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1211.6212&json=true","fetch_graph":"https://pith.science/api/pith-number/MLQGS3ELXHIKDVWRP47AJN4IFD/graph.json","fetch_events":"https://pith.science/api/pith-number/MLQGS3ELXHIKDVWRP47AJN4IFD/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/MLQGS3ELXHIKDVWRP47AJN4IFD/action/timestamp_anchor","attest_storage":"https://pith.science/pith/MLQGS3ELXHIKDVWRP47AJN4IFD/action/storage_attestation","attest_author":"https://pith.science/pith/MLQGS3ELXHIKDVWRP47AJN4IFD/action/author_attestation","sign_citation":"https://pith.science/pith/MLQGS3ELXHIKDVWRP47AJN4IFD/action/citation_signature","submit_replication":"https://pith.science/pith/MLQGS3ELXHIKDVWRP47AJN4IFD/action/replication_record"}},"created_at":"2026-05-18T01:52:54.622745+00:00","updated_at":"2026-05-18T01:52:54.622745+00:00"}