{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2023:HI56FNVDIQP2DFRGVWQC55ASBE","short_pith_number":"pith:HI56FNVD","schema_version":"1.0","canonical_sha256":"3a3be2b6a3441fa19626ada02ef4120919be13dacf68bcd084a5fb422ecf04e8","source":{"kind":"arxiv","id":"2311.07777","version":1},"attestation_state":"computed","paper":{"title":"Constrained Spin Systems and KNdS Black Holes","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["gr-qc"],"primary_cat":"hep-th","authors_text":"Jennie Traschen, Muldrow Etheredge, Vivek Chakrabhavi, Yue Qiu","submitted_at":"2023-11-13T22:06:11Z","abstract_excerpt":"Kerr-Newman de Sitter (KNdS) spacetimes have a rich thermodynamic structure that involves multiple horizons, and so differs in key respects from asymptotically flat or AdS black holes. In this paper, we show that certain features of KNdS spacetimes can be reproduced by a constrained system of $N$ non-interacting spins in a magnetic field. Both the KNdS and spin systems have bounded energy and entropy, a maximum of the entropy in the interior of the energy range, and a symmetry that maps lower energy states to higher energy states with the same entropy. Consequently, both systems have a tempera"},"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":"2311.07777","kind":"arxiv","version":1},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"hep-th","submitted_at":"2023-11-13T22:06:11Z","cross_cats_sorted":["gr-qc"],"title_canon_sha256":"117a9359d2b9aacee9e6976e7076bbfb08b4ad799851d3d84e8d0ac710585a03","abstract_canon_sha256":"39bf96aa62025dd7d4f6a3c9ed7598b4f58c0d15011f5f64878410515d967365"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T07:12:23.636159Z","signature_b64":"Okg6n2TeFhoftJLSxtNOkeWqZghes+XEEchx4GhUwhgmAy+r5pRgZUlZM+qRlcOJN2TEISRwo4j+XkzTxGILBw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"3a3be2b6a3441fa19626ada02ef4120919be13dacf68bcd084a5fb422ecf04e8","last_reissued_at":"2026-07-05T07:12:23.635738Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T07:12:23.635738Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Constrained Spin Systems and KNdS Black Holes","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["gr-qc"],"primary_cat":"hep-th","authors_text":"Jennie Traschen, Muldrow Etheredge, Vivek Chakrabhavi, Yue Qiu","submitted_at":"2023-11-13T22:06:11Z","abstract_excerpt":"Kerr-Newman de Sitter (KNdS) spacetimes have a rich thermodynamic structure that involves multiple horizons, and so differs in key respects from asymptotically flat or AdS black holes. In this paper, we show that certain features of KNdS spacetimes can be reproduced by a constrained system of $N$ non-interacting spins in a magnetic field. Both the KNdS and spin systems have bounded energy and entropy, a maximum of the entropy in the interior of the energy range, and a symmetry that maps lower energy states to higher energy states with the same entropy. Consequently, both systems have a tempera"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2311.07777","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/2311.07777/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":"2311.07777","created_at":"2026-07-05T07:12:23.635796+00:00"},{"alias_kind":"arxiv_version","alias_value":"2311.07777v1","created_at":"2026-07-05T07:12:23.635796+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2311.07777","created_at":"2026-07-05T07:12:23.635796+00:00"},{"alias_kind":"pith_short_12","alias_value":"HI56FNVDIQP2","created_at":"2026-07-05T07:12:23.635796+00:00"},{"alias_kind":"pith_short_16","alias_value":"HI56FNVDIQP2DFRG","created_at":"2026-07-05T07:12:23.635796+00:00"},{"alias_kind":"pith_short_8","alias_value":"HI56FNVD","created_at":"2026-07-05T07:12:23.635796+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2507.23198","citing_title":"High-order QED correction impacts on phase transition of the Euler-Heisenberg dS spacetime","ref_index":42,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/HI56FNVDIQP2DFRGVWQC55ASBE","json":"https://pith.science/pith/HI56FNVDIQP2DFRGVWQC55ASBE.json","graph_json":"https://pith.science/api/pith-number/HI56FNVDIQP2DFRGVWQC55ASBE/graph.json","events_json":"https://pith.science/api/pith-number/HI56FNVDIQP2DFRGVWQC55ASBE/events.json","paper":"https://pith.science/paper/HI56FNVD"},"agent_actions":{"view_html":"https://pith.science/pith/HI56FNVDIQP2DFRGVWQC55ASBE","download_json":"https://pith.science/pith/HI56FNVDIQP2DFRGVWQC55ASBE.json","view_paper":"https://pith.science/paper/HI56FNVD","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2311.07777&json=true","fetch_graph":"https://pith.science/api/pith-number/HI56FNVDIQP2DFRGVWQC55ASBE/graph.json","fetch_events":"https://pith.science/api/pith-number/HI56FNVDIQP2DFRGVWQC55ASBE/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/HI56FNVDIQP2DFRGVWQC55ASBE/action/timestamp_anchor","attest_storage":"https://pith.science/pith/HI56FNVDIQP2DFRGVWQC55ASBE/action/storage_attestation","attest_author":"https://pith.science/pith/HI56FNVDIQP2DFRGVWQC55ASBE/action/author_attestation","sign_citation":"https://pith.science/pith/HI56FNVDIQP2DFRGVWQC55ASBE/action/citation_signature","submit_replication":"https://pith.science/pith/HI56FNVDIQP2DFRGVWQC55ASBE/action/replication_record"}},"created_at":"2026-07-05T07:12:23.635796+00:00","updated_at":"2026-07-05T07:12:23.635796+00:00"}