{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2006:LYEVPGD3NNZWZXUKW4MTULLRYF","short_pith_number":"pith:LYEVPGD3","schema_version":"1.0","canonical_sha256":"5e0957987b6b736cde8ab7193a2d71c17c55456f2d2d8f1d47af504131120fdc","source":{"kind":"arxiv","id":"gr-qc/0604088","version":4},"attestation_state":"computed","paper":{"title":"Black Holes in Einstein-Aether Theory","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph","hep-th"],"primary_cat":"gr-qc","authors_text":"Christopher Eling, Ted Jacobson","submitted_at":"2006-04-20T19:49:09Z","abstract_excerpt":"We study black hole solutions in general relativity coupled to a unit timelike vector field dubbed the \"aether\". To be causally isolated a black hole interior must trap matter fields as well as all aether and metric modes. The theory possesses spin-0, spin-1, and spin-2 modes whose speeds depend on four coupling coefficients. We find that the full three-parameter family of local spherically symmetric static solutions is always regular at a metric horizon, but only a two-parameter subset is regular at a spin-0 horizon. Asymptotic flatness imposes another condition, leaving a one-parameter famil"},"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/0604088","kind":"arxiv","version":4},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"gr-qc","submitted_at":"2006-04-20T19:49:09Z","cross_cats_sorted":["astro-ph","hep-th"],"title_canon_sha256":"ed7d30f7c1e3620b6ead234d437603fa419d8c2f79dab8cdcc5fe327a162e055","abstract_canon_sha256":"15eeb3b04c7ca7ada8c47f30cc30a61c279485925b61a9b9cbd0e09e935df901"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T17:24:24.777658Z","signature_b64":"AVN+E8K75S3qFF4yI+orwhEifyxGfTVM2om06dAJPd5ZXK37hNp6RRkL6uAk0aElmmuWviHPPws8HxORRUkPAw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"5e0957987b6b736cde8ab7193a2d71c17c55456f2d2d8f1d47af504131120fdc","last_reissued_at":"2026-07-04T17:24:24.777240Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T17:24:24.777240Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Black Holes in Einstein-Aether Theory","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph","hep-th"],"primary_cat":"gr-qc","authors_text":"Christopher Eling, Ted Jacobson","submitted_at":"2006-04-20T19:49:09Z","abstract_excerpt":"We study black hole solutions in general relativity coupled to a unit timelike vector field dubbed the \"aether\". To be causally isolated a black hole interior must trap matter fields as well as all aether and metric modes. The theory possesses spin-0, spin-1, and spin-2 modes whose speeds depend on four coupling coefficients. We find that the full three-parameter family of local spherically symmetric static solutions is always regular at a metric horizon, but only a two-parameter subset is regular at a spin-0 horizon. Asymptotic flatness imposes another condition, leaving a one-parameter famil"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"gr-qc/0604088","kind":"arxiv","version":4},"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/0604088/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/0604088","created_at":"2026-07-04T17:24:24.777303+00:00"},{"alias_kind":"arxiv_version","alias_value":"gr-qc/0604088v4","created_at":"2026-07-04T17:24:24.777303+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.gr-qc/0604088","created_at":"2026-07-04T17:24:24.777303+00:00"},{"alias_kind":"pith_short_12","alias_value":"LYEVPGD3NNZW","created_at":"2026-07-04T17:24:24.777303+00:00"},{"alias_kind":"pith_short_16","alias_value":"LYEVPGD3NNZWZXUK","created_at":"2026-07-04T17:24:24.777303+00:00"},{"alias_kind":"pith_short_8","alias_value":"LYEVPGD3","created_at":"2026-07-04T17:24:24.777303+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":2,"sample":[{"citing_arxiv_id":"1501.07274","citing_title":"Testing General Relativity with Present and Future Astrophysical Observations","ref_index":97,"is_internal_anchor":true},{"citing_arxiv_id":"1102.4014","citing_title":"Quasinormal modes of black holes: from astrophysics to string theory","ref_index":63,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/LYEVPGD3NNZWZXUKW4MTULLRYF","json":"https://pith.science/pith/LYEVPGD3NNZWZXUKW4MTULLRYF.json","graph_json":"https://pith.science/api/pith-number/LYEVPGD3NNZWZXUKW4MTULLRYF/graph.json","events_json":"https://pith.science/api/pith-number/LYEVPGD3NNZWZXUKW4MTULLRYF/events.json","paper":"https://pith.science/paper/LYEVPGD3"},"agent_actions":{"view_html":"https://pith.science/pith/LYEVPGD3NNZWZXUKW4MTULLRYF","download_json":"https://pith.science/pith/LYEVPGD3NNZWZXUKW4MTULLRYF.json","view_paper":"https://pith.science/paper/LYEVPGD3","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=gr-qc/0604088&json=true","fetch_graph":"https://pith.science/api/pith-number/LYEVPGD3NNZWZXUKW4MTULLRYF/graph.json","fetch_events":"https://pith.science/api/pith-number/LYEVPGD3NNZWZXUKW4MTULLRYF/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/LYEVPGD3NNZWZXUKW4MTULLRYF/action/timestamp_anchor","attest_storage":"https://pith.science/pith/LYEVPGD3NNZWZXUKW4MTULLRYF/action/storage_attestation","attest_author":"https://pith.science/pith/LYEVPGD3NNZWZXUKW4MTULLRYF/action/author_attestation","sign_citation":"https://pith.science/pith/LYEVPGD3NNZWZXUKW4MTULLRYF/action/citation_signature","submit_replication":"https://pith.science/pith/LYEVPGD3NNZWZXUKW4MTULLRYF/action/replication_record"}},"created_at":"2026-07-04T17:24:24.777303+00:00","updated_at":"2026-07-04T17:24:24.777303+00:00"}