{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2020:OOKYOXCY3UWAR56WNNCJ6ZOANQ","short_pith_number":"pith:OOKYOXCY","schema_version":"1.0","canonical_sha256":"7395875c58dd2c08f7d66b449f65c06c26eb883ea85afa76b8fa43bad0703dd3","source":{"kind":"arxiv","id":"2007.00731","version":1},"attestation_state":"computed","paper":{"title":"Horizon radiation reaction forces","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["gr-qc"],"primary_cat":"hep-th","authors_text":"Ira Z. Rothstein, Walter D. Goldberger","submitted_at":"2020-07-01T20:07:20Z","abstract_excerpt":"Using Effective Field Theory (EFT) methods, we compute the effects of horizon dissipation on the gravitational interactions of relativistic binary black hole systems. We assume that the dynamics is perturbative, i.e it admits an expansion in powers of Newton's constant (post-Minkowskian, or PM, approximation). As applications, we compute corrections to the scattering angle in a black hole collision due to dissipative effects to leading PM order, as well as the post-Newtonian (PN) corrections to the equations of motion of binary black holes in non-relativistic orbits, which represents the leadi"},"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":"2007.00731","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"hep-th","submitted_at":"2020-07-01T20:07:20Z","cross_cats_sorted":["gr-qc"],"title_canon_sha256":"cdfd321ff06fd3451a7428fdcec6bd91ecdf3729a358321155f2eb2ea2257903","abstract_canon_sha256":"9bdb4e336dd63197e9d2bbf66331b1d144fb20f1a56a092c40ac1e701bc3dd90"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T01:46:22.601790Z","signature_b64":"gsPBkMMqugdJfuzyXN2ZythuH9U6qrSrpfXpoefDYmNjmKgiD7qFtf1R8SBK9CgyJzWmO58dA6N+0F9g4bP1DQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"7395875c58dd2c08f7d66b449f65c06c26eb883ea85afa76b8fa43bad0703dd3","last_reissued_at":"2026-07-05T01:46:22.601367Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T01:46:22.601367Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Horizon radiation reaction forces","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["gr-qc"],"primary_cat":"hep-th","authors_text":"Ira Z. Rothstein, Walter D. Goldberger","submitted_at":"2020-07-01T20:07:20Z","abstract_excerpt":"Using Effective Field Theory (EFT) methods, we compute the effects of horizon dissipation on the gravitational interactions of relativistic binary black hole systems. We assume that the dynamics is perturbative, i.e it admits an expansion in powers of Newton's constant (post-Minkowskian, or PM, approximation). As applications, we compute corrections to the scattering angle in a black hole collision due to dissipative effects to leading PM order, as well as the post-Newtonian (PN) corrections to the equations of motion of binary black holes in non-relativistic orbits, which represents the leadi"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2007.00731","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/2007.00731/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":"2007.00731","created_at":"2026-07-05T01:46:22.601422+00:00"},{"alias_kind":"arxiv_version","alias_value":"2007.00731v1","created_at":"2026-07-05T01:46:22.601422+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2007.00731","created_at":"2026-07-05T01:46:22.601422+00:00"},{"alias_kind":"pith_short_12","alias_value":"OOKYOXCY3UWA","created_at":"2026-07-05T01:46:22.601422+00:00"},{"alias_kind":"pith_short_16","alias_value":"OOKYOXCY3UWAR56W","created_at":"2026-07-05T01:46:22.601422+00:00"},{"alias_kind":"pith_short_8","alias_value":"OOKYOXCY","created_at":"2026-07-05T01:46:22.601422+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":5,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2606.23450","citing_title":"NLO Angular Impulse and Leading Singularities to all orders in spin for Kerr Black Holes","ref_index":118,"is_internal_anchor":false},{"citing_arxiv_id":"2510.25866","citing_title":"Hawking Radiation meets the Double Copy","ref_index":8,"is_internal_anchor":false},{"citing_arxiv_id":"2512.02274","citing_title":"Gravitational radiation from hyperbolic orbits: comparison between self-force, post-Minkowskian, post-Newtonian, and numerical relativity results","ref_index":45,"is_internal_anchor":false},{"citing_arxiv_id":"2604.09545","citing_title":"Black Hole Dynamics at Fifth Post-Newtonian Order","ref_index":69,"is_internal_anchor":false},{"citing_arxiv_id":"2604.08653","citing_title":"Love numbers of black holes and compact objects","ref_index":162,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/OOKYOXCY3UWAR56WNNCJ6ZOANQ","json":"https://pith.science/pith/OOKYOXCY3UWAR56WNNCJ6ZOANQ.json","graph_json":"https://pith.science/api/pith-number/OOKYOXCY3UWAR56WNNCJ6ZOANQ/graph.json","events_json":"https://pith.science/api/pith-number/OOKYOXCY3UWAR56WNNCJ6ZOANQ/events.json","paper":"https://pith.science/paper/OOKYOXCY"},"agent_actions":{"view_html":"https://pith.science/pith/OOKYOXCY3UWAR56WNNCJ6ZOANQ","download_json":"https://pith.science/pith/OOKYOXCY3UWAR56WNNCJ6ZOANQ.json","view_paper":"https://pith.science/paper/OOKYOXCY","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2007.00731&json=true","fetch_graph":"https://pith.science/api/pith-number/OOKYOXCY3UWAR56WNNCJ6ZOANQ/graph.json","fetch_events":"https://pith.science/api/pith-number/OOKYOXCY3UWAR56WNNCJ6ZOANQ/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/OOKYOXCY3UWAR56WNNCJ6ZOANQ/action/timestamp_anchor","attest_storage":"https://pith.science/pith/OOKYOXCY3UWAR56WNNCJ6ZOANQ/action/storage_attestation","attest_author":"https://pith.science/pith/OOKYOXCY3UWAR56WNNCJ6ZOANQ/action/author_attestation","sign_citation":"https://pith.science/pith/OOKYOXCY3UWAR56WNNCJ6ZOANQ/action/citation_signature","submit_replication":"https://pith.science/pith/OOKYOXCY3UWAR56WNNCJ6ZOANQ/action/replication_record"}},"created_at":"2026-07-05T01:46:22.601422+00:00","updated_at":"2026-07-05T01:46:22.601422+00:00"}