{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2010:ZUD2UYWWT6HEK6WQ5WJCAMGGCZ","short_pith_number":"pith:ZUD2UYWW","schema_version":"1.0","canonical_sha256":"cd07aa62d69f8e457ad0ed922030c61676e9afe2440f149e683efabff4af7c94","source":{"kind":"arxiv","id":"1006.1632","version":3},"attestation_state":"computed","paper":{"title":"Notes on the integration of numerical relativity waveforms","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"gr-qc","authors_text":"Christian Reisswig, Denis Pollney","submitted_at":"2010-06-08T18:26:08Z","abstract_excerpt":"A primary goal of numerical relativity is to provide estimates of the wave strain, $h$, from strong gravitational wave sources, to be used in detector templates. The simulations, however, typically measure waves in terms of the Weyl curvature component, $\\psi_4$. Assuming Bondi gauge, transforming to the strain $h$ reduces to integration of $\\psi_4$ twice in time. Integrations performed in either the time or frequency domain, however, lead to secular non-linear drifts in the resulting strain $h$. These non-linear drifts are not explained by the two unknown integration constants which can at mo"},"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":"1006.1632","kind":"arxiv","version":3},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"gr-qc","submitted_at":"2010-06-08T18:26:08Z","cross_cats_sorted":[],"title_canon_sha256":"7ad7f4ae08acea17884f83e80c51b5f39d8c65379f7501addf694335f076caad","abstract_canon_sha256":"70646a219c7e67048902ebc1167d4d7b815e9f7b5ecd346688b2092256ef185b"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T04:12:34.022081Z","signature_b64":"5xW5RphUwbWvJckY5binKdEaW2ew2IqFwxhwtDBZRS/oUpFMiHwBy9eWD+FL3kqn3LRxFCWPjAWtj957nO5zBA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"cd07aa62d69f8e457ad0ed922030c61676e9afe2440f149e683efabff4af7c94","last_reissued_at":"2026-05-18T04:12:34.021460Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T04:12:34.021460Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Notes on the integration of numerical relativity waveforms","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"gr-qc","authors_text":"Christian Reisswig, Denis Pollney","submitted_at":"2010-06-08T18:26:08Z","abstract_excerpt":"A primary goal of numerical relativity is to provide estimates of the wave strain, $h$, from strong gravitational wave sources, to be used in detector templates. The simulations, however, typically measure waves in terms of the Weyl curvature component, $\\psi_4$. Assuming Bondi gauge, transforming to the strain $h$ reduces to integration of $\\psi_4$ twice in time. Integrations performed in either the time or frequency domain, however, lead to secular non-linear drifts in the resulting strain $h$. These non-linear drifts are not explained by the two unknown integration constants which can at mo"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1006.1632","kind":"arxiv","version":3},"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":"1006.1632","created_at":"2026-05-18T04:12:34.021557+00:00"},{"alias_kind":"arxiv_version","alias_value":"1006.1632v3","created_at":"2026-05-18T04:12:34.021557+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1006.1632","created_at":"2026-05-18T04:12:34.021557+00:00"},{"alias_kind":"pith_short_12","alias_value":"ZUD2UYWWT6HE","created_at":"2026-05-18T12:26:18.847500+00:00"},{"alias_kind":"pith_short_16","alias_value":"ZUD2UYWWT6HEK6WQ","created_at":"2026-05-18T12:26:18.847500+00:00"},{"alias_kind":"pith_short_8","alias_value":"ZUD2UYWW","created_at":"2026-05-18T12:26:18.847500+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":2,"sample":[{"citing_arxiv_id":"2605.30430","citing_title":"Exact Mass Conservation in Binary Neutron Star Merger Simulations","ref_index":40,"is_internal_anchor":true},{"citing_arxiv_id":"2510.17967","citing_title":"Scalar fields around black hole binaries in LIGO-Virgo-KAGRA","ref_index":108,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/ZUD2UYWWT6HEK6WQ5WJCAMGGCZ","json":"https://pith.science/pith/ZUD2UYWWT6HEK6WQ5WJCAMGGCZ.json","graph_json":"https://pith.science/api/pith-number/ZUD2UYWWT6HEK6WQ5WJCAMGGCZ/graph.json","events_json":"https://pith.science/api/pith-number/ZUD2UYWWT6HEK6WQ5WJCAMGGCZ/events.json","paper":"https://pith.science/paper/ZUD2UYWW"},"agent_actions":{"view_html":"https://pith.science/pith/ZUD2UYWWT6HEK6WQ5WJCAMGGCZ","download_json":"https://pith.science/pith/ZUD2UYWWT6HEK6WQ5WJCAMGGCZ.json","view_paper":"https://pith.science/paper/ZUD2UYWW","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1006.1632&json=true","fetch_graph":"https://pith.science/api/pith-number/ZUD2UYWWT6HEK6WQ5WJCAMGGCZ/graph.json","fetch_events":"https://pith.science/api/pith-number/ZUD2UYWWT6HEK6WQ5WJCAMGGCZ/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/ZUD2UYWWT6HEK6WQ5WJCAMGGCZ/action/timestamp_anchor","attest_storage":"https://pith.science/pith/ZUD2UYWWT6HEK6WQ5WJCAMGGCZ/action/storage_attestation","attest_author":"https://pith.science/pith/ZUD2UYWWT6HEK6WQ5WJCAMGGCZ/action/author_attestation","sign_citation":"https://pith.science/pith/ZUD2UYWWT6HEK6WQ5WJCAMGGCZ/action/citation_signature","submit_replication":"https://pith.science/pith/ZUD2UYWWT6HEK6WQ5WJCAMGGCZ/action/replication_record"}},"created_at":"2026-05-18T04:12:34.021557+00:00","updated_at":"2026-05-18T04:12:34.021557+00:00"}