{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2006:646SP4TJTGVSLBTDT6AWPSZQFB","short_pith_number":"pith:646SP4TJ","schema_version":"1.0","canonical_sha256":"f73d27f26999ab2586639f8167cb30286256b1a343d6c8f3d70c81942db649ad","source":{"kind":"arxiv","id":"gr-qc/0605013","version":1},"attestation_state":"computed","paper":{"title":"Stability and quasinormal modes of the massive scalar field around Kerr black holes","license":"","headline":"","cross_cats":[],"primary_cat":"gr-qc","authors_text":"A. Zhidenko, R. A. Konoplya","submitted_at":"2006-05-01T20:55:31Z","abstract_excerpt":"We find quasinormal spectrum of the massive scalar field in the background of the Kerr black holes. We show that all found modes are damped under the quasinormal modes boundary conditions when $\\mu M$ is not large, thereby implying stability of the massive scalar field. This complements the region of stability determined by the Beyer inequality for large masses of the field. We show that, similar to the case of a non-rotating black holes, the massive term of the scalar field does not contribute in the regime of high damping. Thereby, the high damping asymptotic should be the same as for the ma"},"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/0605013","kind":"arxiv","version":1},"metadata":{"license":"","primary_cat":"gr-qc","submitted_at":"2006-05-01T20:55:31Z","cross_cats_sorted":[],"title_canon_sha256":"eb69246805d4fd4c1c8c05de2b477d4a1ec919183b4bb9da8fc5e1d1c531fe32","abstract_canon_sha256":"485c9c457122c6d8a6349be97c8162c2eae55332dc3eff257ee7fb9927d13c4e"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T17:01:27.697452Z","signature_b64":"B7+ShxqMuGtwcSB0tiRaWRaYV6qso8hUBiI/c/Dph8CkABlyNAB3om/wvBkgGMD+3Dn60JpcdUL/XStdvEuoBw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"f73d27f26999ab2586639f8167cb30286256b1a343d6c8f3d70c81942db649ad","last_reissued_at":"2026-07-04T17:01:27.697110Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T17:01:27.697110Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Stability and quasinormal modes of the massive scalar field around Kerr black holes","license":"","headline":"","cross_cats":[],"primary_cat":"gr-qc","authors_text":"A. Zhidenko, R. A. Konoplya","submitted_at":"2006-05-01T20:55:31Z","abstract_excerpt":"We find quasinormal spectrum of the massive scalar field in the background of the Kerr black holes. We show that all found modes are damped under the quasinormal modes boundary conditions when $\\mu M$ is not large, thereby implying stability of the massive scalar field. This complements the region of stability determined by the Beyer inequality for large masses of the field. We show that, similar to the case of a non-rotating black holes, the massive term of the scalar field does not contribute in the regime of high damping. Thereby, the high damping asymptotic should be the same as for the ma"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"gr-qc/0605013","kind":"arxiv","version":1},"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/gr-qc/0605013/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":"gr-qc/0605013","created_at":"2026-07-04T17:01:27.697166+00:00"},{"alias_kind":"arxiv_version","alias_value":"gr-qc/0605013v1","created_at":"2026-07-04T17:01:27.697166+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.gr-qc/0605013","created_at":"2026-07-04T17:01:27.697166+00:00"},{"alias_kind":"pith_short_12","alias_value":"646SP4TJTGVS","created_at":"2026-07-04T17:01:27.697166+00:00"},{"alias_kind":"pith_short_16","alias_value":"646SP4TJTGVSLBTD","created_at":"2026-07-04T17:01:27.697166+00:00"},{"alias_kind":"pith_short_8","alias_value":"646SP4TJ","created_at":"2026-07-04T17:01:27.697166+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":6,"internal_anchor_count":4,"sample":[{"citing_arxiv_id":"2605.25705","citing_title":"Ces\\`aro convergence of the high-order WKB method and its applications to black-hole overtones and long-lived modes","ref_index":43,"is_internal_anchor":true},{"citing_arxiv_id":"2505.20919","citing_title":"Scalarization and superradiant instability of black hole induced by dark matter halo in the scalar-tensor theory of gravity","ref_index":44,"is_internal_anchor":true},{"citing_arxiv_id":"2512.08116","citing_title":"Universality in quasinormal modes of a magnetized black hole","ref_index":15,"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":44,"is_internal_anchor":true},{"citing_arxiv_id":"1102.4014","citing_title":"Quasinormal modes of black holes: from astrophysics to string theory","ref_index":211,"is_internal_anchor":false},{"citing_arxiv_id":"2505.23895","citing_title":"Black hole spectroscopy: from theory to experiment","ref_index":161,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/646SP4TJTGVSLBTDT6AWPSZQFB","json":"https://pith.science/pith/646SP4TJTGVSLBTDT6AWPSZQFB.json","graph_json":"https://pith.science/api/pith-number/646SP4TJTGVSLBTDT6AWPSZQFB/graph.json","events_json":"https://pith.science/api/pith-number/646SP4TJTGVSLBTDT6AWPSZQFB/events.json","paper":"https://pith.science/paper/646SP4TJ"},"agent_actions":{"view_html":"https://pith.science/pith/646SP4TJTGVSLBTDT6AWPSZQFB","download_json":"https://pith.science/pith/646SP4TJTGVSLBTDT6AWPSZQFB.json","view_paper":"https://pith.science/paper/646SP4TJ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=gr-qc/0605013&json=true","fetch_graph":"https://pith.science/api/pith-number/646SP4TJTGVSLBTDT6AWPSZQFB/graph.json","fetch_events":"https://pith.science/api/pith-number/646SP4TJTGVSLBTDT6AWPSZQFB/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/646SP4TJTGVSLBTDT6AWPSZQFB/action/timestamp_anchor","attest_storage":"https://pith.science/pith/646SP4TJTGVSLBTDT6AWPSZQFB/action/storage_attestation","attest_author":"https://pith.science/pith/646SP4TJTGVSLBTDT6AWPSZQFB/action/author_attestation","sign_citation":"https://pith.science/pith/646SP4TJTGVSLBTDT6AWPSZQFB/action/citation_signature","submit_replication":"https://pith.science/pith/646SP4TJTGVSLBTDT6AWPSZQFB/action/replication_record"}},"created_at":"2026-07-04T17:01:27.697166+00:00","updated_at":"2026-07-04T17:01:27.697166+00:00"}