{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2012:GCOFL5D35QZCMOMGZ4OYXYNQHH","short_pith_number":"pith:GCOFL5D3","schema_version":"1.0","canonical_sha256":"309c55f47bec32263986cf1d8be1b039e252b3d5357c1a2e21c399ddddcc738a","source":{"kind":"arxiv","id":"1202.4893","version":5},"attestation_state":"computed","paper":{"title":"Black hole perturbation in the most general scalar-tensor theory with second-order field equations I: The odd-parity sector","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO","hep-th"],"primary_cat":"gr-qc","authors_text":"Hayato Motohashi, Teruaki Suyama, Tsutomu Kobayashi","submitted_at":"2012-02-22T12:45:58Z","abstract_excerpt":"We perform a fully relativistic analysis of odd-type linear perturbations around a static and spherically symmetric solution in the most general scalar-tensor theory with second-order field equations in four-dimensional spacetime. It is shown that, as in the case of general relativity, the quadratic action for the perturbations reduces to the one having only a single dynamical variable, from which concise formulas for no-ghost and no-gradient instability conditions are derived. Our result is applicable to all the theories of gravity with an extra scalar degree of freedom. We demonstrate how th"},"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":"1202.4893","kind":"arxiv","version":5},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"gr-qc","submitted_at":"2012-02-22T12:45:58Z","cross_cats_sorted":["astro-ph.CO","hep-th"],"title_canon_sha256":"d0f0c92c179b582307b737dc49c3dc89c06578b25e7102aefc7e18e72175bfda","abstract_canon_sha256":"a14e369da054fbbdaeab4358ad3e63ca435f9b6fe144b92ef801552d07400f54"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:30:49.852701Z","signature_b64":"AOZU5olrM3uVbHh20vshEd65Afv608hxGMMw6I048khwDSf6t/WLX5MjqygXCyC8YffTbBycNVxhjHS5QelFDg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"309c55f47bec32263986cf1d8be1b039e252b3d5357c1a2e21c399ddddcc738a","last_reissued_at":"2026-05-18T00:30:49.852102Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:30:49.852102Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Black hole perturbation in the most general scalar-tensor theory with second-order field equations I: The odd-parity sector","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO","hep-th"],"primary_cat":"gr-qc","authors_text":"Hayato Motohashi, Teruaki Suyama, Tsutomu Kobayashi","submitted_at":"2012-02-22T12:45:58Z","abstract_excerpt":"We perform a fully relativistic analysis of odd-type linear perturbations around a static and spherically symmetric solution in the most general scalar-tensor theory with second-order field equations in four-dimensional spacetime. It is shown that, as in the case of general relativity, the quadratic action for the perturbations reduces to the one having only a single dynamical variable, from which concise formulas for no-ghost and no-gradient instability conditions are derived. Our result is applicable to all the theories of gravity with an extra scalar degree of freedom. We demonstrate how th"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1202.4893","kind":"arxiv","version":5},"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":"1202.4893","created_at":"2026-05-18T00:30:49.852181+00:00"},{"alias_kind":"arxiv_version","alias_value":"1202.4893v5","created_at":"2026-05-18T00:30:49.852181+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1202.4893","created_at":"2026-05-18T00:30:49.852181+00:00"},{"alias_kind":"pith_short_12","alias_value":"GCOFL5D35QZC","created_at":"2026-05-18T12:27:06.952714+00:00"},{"alias_kind":"pith_short_16","alias_value":"GCOFL5D35QZCMOMG","created_at":"2026-05-18T12:27:06.952714+00:00"},{"alias_kind":"pith_short_8","alias_value":"GCOFL5D3","created_at":"2026-05-18T12:27:06.952714+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":4,"internal_anchor_count":2,"sample":[{"citing_arxiv_id":"2603.22398","citing_title":"Stable black hole solutions with cosmological hair","ref_index":96,"is_internal_anchor":true},{"citing_arxiv_id":"2605.13036","citing_title":"Inspiral gravitational waveforms from charged compact binaries with scalar hair","ref_index":39,"is_internal_anchor":true},{"citing_arxiv_id":"1501.07274","citing_title":"Testing General Relativity with Present and Future Astrophysical Observations","ref_index":95,"is_internal_anchor":false},{"citing_arxiv_id":"2604.21962","citing_title":"Perturbation Dynamics and Structure Formation in Extended Proca-Nuevo Gravity","ref_index":46,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/GCOFL5D35QZCMOMGZ4OYXYNQHH","json":"https://pith.science/pith/GCOFL5D35QZCMOMGZ4OYXYNQHH.json","graph_json":"https://pith.science/api/pith-number/GCOFL5D35QZCMOMGZ4OYXYNQHH/graph.json","events_json":"https://pith.science/api/pith-number/GCOFL5D35QZCMOMGZ4OYXYNQHH/events.json","paper":"https://pith.science/paper/GCOFL5D3"},"agent_actions":{"view_html":"https://pith.science/pith/GCOFL5D35QZCMOMGZ4OYXYNQHH","download_json":"https://pith.science/pith/GCOFL5D35QZCMOMGZ4OYXYNQHH.json","view_paper":"https://pith.science/paper/GCOFL5D3","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1202.4893&json=true","fetch_graph":"https://pith.science/api/pith-number/GCOFL5D35QZCMOMGZ4OYXYNQHH/graph.json","fetch_events":"https://pith.science/api/pith-number/GCOFL5D35QZCMOMGZ4OYXYNQHH/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/GCOFL5D35QZCMOMGZ4OYXYNQHH/action/timestamp_anchor","attest_storage":"https://pith.science/pith/GCOFL5D35QZCMOMGZ4OYXYNQHH/action/storage_attestation","attest_author":"https://pith.science/pith/GCOFL5D35QZCMOMGZ4OYXYNQHH/action/author_attestation","sign_citation":"https://pith.science/pith/GCOFL5D35QZCMOMGZ4OYXYNQHH/action/citation_signature","submit_replication":"https://pith.science/pith/GCOFL5D35QZCMOMGZ4OYXYNQHH/action/replication_record"}},"created_at":"2026-05-18T00:30:49.852181+00:00","updated_at":"2026-05-18T00:30:49.852181+00:00"}