{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2023:EHFCGNYSBBUTOMLPNC6UDZ3JXU","short_pith_number":"pith:EHFCGNYS","schema_version":"1.0","canonical_sha256":"21ca233712086937316f68bd41e769bd2be95b2e9cf109d728f56ad064f8ffbc","source":{"kind":"arxiv","id":"2311.13742","version":2},"attestation_state":"computed","paper":{"title":"Extremal Black Hole Decay in de Sitter Space","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["gr-qc"],"primary_cat":"hep-th","authors_text":"Jan Pieter van der Schaar, Lars Aalsma, Manus Visser","submitted_at":"2023-11-23T00:23:04Z","abstract_excerpt":"The decay of extremal charged black holes has been a useful guidance to derive consistency conditions in quantum gravity. In de Sitter space it has been argued that requiring (extremal) charged Nariai black holes to decay without forming a big crunch singularity yields the Festina Lente (FL) bound: particles with mass $m_s$ and charge $q$ should satisfy $m_s^2 \\gg M_pHq$, where $M_p$ is the Planck mass and $H$ the Hubble parameter. Using a tunneling approach we show that the decay probability of charged black holes in de Sitter space in the s-wave sector is $P\\sim \\exp(\\Delta S_b)$, where~$\\De"},"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":"2311.13742","kind":"arxiv","version":2},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"hep-th","submitted_at":"2023-11-23T00:23:04Z","cross_cats_sorted":["gr-qc"],"title_canon_sha256":"8edef7fcabb17fd504126d113882cf65d79aceefd58ecae74f13b28276082335","abstract_canon_sha256":"aafb5603a44765a6ca84d5d4c8f498e1959498dabd2778dd54d1177628c0dba5"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T08:59:49.468965Z","signature_b64":"cDFr+bDjbXiMVoIQlCOavyb1TJK3Gyu8A0Sfe4tehR55IYPUfDVKwTv1XxCtSwLWKBeBUF3/ar0XpsEKDRd1Aw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"21ca233712086937316f68bd41e769bd2be95b2e9cf109d728f56ad064f8ffbc","last_reissued_at":"2026-07-05T08:59:49.468584Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T08:59:49.468584Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Extremal Black Hole Decay in de Sitter Space","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["gr-qc"],"primary_cat":"hep-th","authors_text":"Jan Pieter van der Schaar, Lars Aalsma, Manus Visser","submitted_at":"2023-11-23T00:23:04Z","abstract_excerpt":"The decay of extremal charged black holes has been a useful guidance to derive consistency conditions in quantum gravity. In de Sitter space it has been argued that requiring (extremal) charged Nariai black holes to decay without forming a big crunch singularity yields the Festina Lente (FL) bound: particles with mass $m_s$ and charge $q$ should satisfy $m_s^2 \\gg M_pHq$, where $M_p$ is the Planck mass and $H$ the Hubble parameter. Using a tunneling approach we show that the decay probability of charged black holes in de Sitter space in the s-wave sector is $P\\sim \\exp(\\Delta S_b)$, where~$\\De"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2311.13742","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/2311.13742/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":"2311.13742","created_at":"2026-07-05T08:59:49.468640+00:00"},{"alias_kind":"arxiv_version","alias_value":"2311.13742v2","created_at":"2026-07-05T08:59:49.468640+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2311.13742","created_at":"2026-07-05T08:59:49.468640+00:00"},{"alias_kind":"pith_short_12","alias_value":"EHFCGNYSBBUT","created_at":"2026-07-05T08:59:49.468640+00:00"},{"alias_kind":"pith_short_16","alias_value":"EHFCGNYSBBUTOMLP","created_at":"2026-07-05T08:59:49.468640+00:00"},{"alias_kind":"pith_short_8","alias_value":"EHFCGNYS","created_at":"2026-07-05T08:59:49.468640+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2605.20349","citing_title":"The fate of Reissner--Nordstr\\\"om--de Sitter black holes: nonequilibrium discharge and evaporation","ref_index":32,"is_internal_anchor":false},{"citing_arxiv_id":"2511.03867","citing_title":"Limits on the Statistical Description of Charged de Sitter Black Holes","ref_index":22,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/EHFCGNYSBBUTOMLPNC6UDZ3JXU","json":"https://pith.science/pith/EHFCGNYSBBUTOMLPNC6UDZ3JXU.json","graph_json":"https://pith.science/api/pith-number/EHFCGNYSBBUTOMLPNC6UDZ3JXU/graph.json","events_json":"https://pith.science/api/pith-number/EHFCGNYSBBUTOMLPNC6UDZ3JXU/events.json","paper":"https://pith.science/paper/EHFCGNYS"},"agent_actions":{"view_html":"https://pith.science/pith/EHFCGNYSBBUTOMLPNC6UDZ3JXU","download_json":"https://pith.science/pith/EHFCGNYSBBUTOMLPNC6UDZ3JXU.json","view_paper":"https://pith.science/paper/EHFCGNYS","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2311.13742&json=true","fetch_graph":"https://pith.science/api/pith-number/EHFCGNYSBBUTOMLPNC6UDZ3JXU/graph.json","fetch_events":"https://pith.science/api/pith-number/EHFCGNYSBBUTOMLPNC6UDZ3JXU/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/EHFCGNYSBBUTOMLPNC6UDZ3JXU/action/timestamp_anchor","attest_storage":"https://pith.science/pith/EHFCGNYSBBUTOMLPNC6UDZ3JXU/action/storage_attestation","attest_author":"https://pith.science/pith/EHFCGNYSBBUTOMLPNC6UDZ3JXU/action/author_attestation","sign_citation":"https://pith.science/pith/EHFCGNYSBBUTOMLPNC6UDZ3JXU/action/citation_signature","submit_replication":"https://pith.science/pith/EHFCGNYSBBUTOMLPNC6UDZ3JXU/action/replication_record"}},"created_at":"2026-07-05T08:59:49.468640+00:00","updated_at":"2026-07-05T08:59:49.468640+00:00"}