{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2005:PHQEFHGAQIYBVLDFEIK6Q5N2DY","short_pith_number":"pith:PHQEFHGA","schema_version":"1.0","canonical_sha256":"79e0429cc082301aac652215e875ba1e29c2cee21cd9dd5601404b325467d53d","source":{"kind":"arxiv","id":"gr-qc/0510019","version":2},"attestation_state":"computed","paper":{"title":"Perturbations of Schwarzschild black holes in the Lorenz gauge: Formulation and numerical implementation","license":"","headline":"","cross_cats":[],"primary_cat":"gr-qc","authors_text":"Carlos O. Lousto, Leor Barack","submitted_at":"2005-10-05T18:41:05Z","abstract_excerpt":"We reformulate the theory of Schwarzschild black hole perturbations in terms of the metric perturbation in the Lorenz gauge. In this formulation, each tensor-harmonic mode of the perturbation is constructed algebraically from 10 scalar functions, satisfying a set of 10 wavelike equations, which are decoupled at their principal parts. We solve these equations using numerical evolution in the time domain, for the case of a pointlike test particle set in a circular geodesic orbit around the black hole. Our code uses characteristic coordinates, and incorporates a constraint damping scheme. The axi"},"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/0510019","kind":"arxiv","version":2},"metadata":{"license":"","primary_cat":"gr-qc","submitted_at":"2005-10-05T18:41:05Z","cross_cats_sorted":[],"title_canon_sha256":"2dca9920a06a022e6ce828057b4ed1c21b2a89511a5a81d8fb060ad8a42df3fb","abstract_canon_sha256":"39d6b540caa7e55790e7206f621e06f8cf6fcd886ae2fbede05bc5f45c65ea37"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T16:55:18.535181Z","signature_b64":"44KArqRQfNAKFIWFsJpWq2gDaEWWWmAXkj2SOy9gbPtwZ7CRkdZG1FAyuREUWtZXrwiErYyOfFuDO3ZHX0hzAQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"79e0429cc082301aac652215e875ba1e29c2cee21cd9dd5601404b325467d53d","last_reissued_at":"2026-07-04T16:55:18.534780Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T16:55:18.534780Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Perturbations of Schwarzschild black holes in the Lorenz gauge: Formulation and numerical implementation","license":"","headline":"","cross_cats":[],"primary_cat":"gr-qc","authors_text":"Carlos O. Lousto, Leor Barack","submitted_at":"2005-10-05T18:41:05Z","abstract_excerpt":"We reformulate the theory of Schwarzschild black hole perturbations in terms of the metric perturbation in the Lorenz gauge. In this formulation, each tensor-harmonic mode of the perturbation is constructed algebraically from 10 scalar functions, satisfying a set of 10 wavelike equations, which are decoupled at their principal parts. We solve these equations using numerical evolution in the time domain, for the case of a pointlike test particle set in a circular geodesic orbit around the black hole. Our code uses characteristic coordinates, and incorporates a constraint damping scheme. The axi"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"gr-qc/0510019","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/gr-qc/0510019/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/0510019","created_at":"2026-07-04T16:55:18.534848+00:00"},{"alias_kind":"arxiv_version","alias_value":"gr-qc/0510019v2","created_at":"2026-07-04T16:55:18.534848+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.gr-qc/0510019","created_at":"2026-07-04T16:55:18.534848+00:00"},{"alias_kind":"pith_short_12","alias_value":"PHQEFHGAQIYB","created_at":"2026-07-04T16:55:18.534848+00:00"},{"alias_kind":"pith_short_16","alias_value":"PHQEFHGAQIYBVLDF","created_at":"2026-07-04T16:55:18.534848+00:00"},{"alias_kind":"pith_short_8","alias_value":"PHQEFHGA","created_at":"2026-07-04T16:55:18.534848+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2606.09766","citing_title":"Modified Teukolsky Formalism for Extreme Mass-Ratio Inspirals in Higher-Derivative Gravity","ref_index":35,"is_internal_anchor":true},{"citing_arxiv_id":"2605.11080","citing_title":"Metric Reconstruction for Generic Black-Hole Perturbations","ref_index":61,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/PHQEFHGAQIYBVLDFEIK6Q5N2DY","json":"https://pith.science/pith/PHQEFHGAQIYBVLDFEIK6Q5N2DY.json","graph_json":"https://pith.science/api/pith-number/PHQEFHGAQIYBVLDFEIK6Q5N2DY/graph.json","events_json":"https://pith.science/api/pith-number/PHQEFHGAQIYBVLDFEIK6Q5N2DY/events.json","paper":"https://pith.science/paper/PHQEFHGA"},"agent_actions":{"view_html":"https://pith.science/pith/PHQEFHGAQIYBVLDFEIK6Q5N2DY","download_json":"https://pith.science/pith/PHQEFHGAQIYBVLDFEIK6Q5N2DY.json","view_paper":"https://pith.science/paper/PHQEFHGA","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=gr-qc/0510019&json=true","fetch_graph":"https://pith.science/api/pith-number/PHQEFHGAQIYBVLDFEIK6Q5N2DY/graph.json","fetch_events":"https://pith.science/api/pith-number/PHQEFHGAQIYBVLDFEIK6Q5N2DY/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/PHQEFHGAQIYBVLDFEIK6Q5N2DY/action/timestamp_anchor","attest_storage":"https://pith.science/pith/PHQEFHGAQIYBVLDFEIK6Q5N2DY/action/storage_attestation","attest_author":"https://pith.science/pith/PHQEFHGAQIYBVLDFEIK6Q5N2DY/action/author_attestation","sign_citation":"https://pith.science/pith/PHQEFHGAQIYBVLDFEIK6Q5N2DY/action/citation_signature","submit_replication":"https://pith.science/pith/PHQEFHGAQIYBVLDFEIK6Q5N2DY/action/replication_record"}},"created_at":"2026-07-04T16:55:18.534848+00:00","updated_at":"2026-07-04T16:55:18.534848+00:00"}