{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2018:KKQVDAKCDH4GTW2YVV6Q23UGVB","short_pith_number":"pith:KKQVDAKC","schema_version":"1.0","canonical_sha256":"52a151814219f869db58ad7d0d6e86a844d1a49119a297680109714a3699d6b8","source":{"kind":"arxiv","id":"1810.02487","version":5},"attestation_state":"computed","paper":{"title":"Energy conditions in arbitrary dimensions","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["hep-th"],"primary_cat":"gr-qc","authors_text":"Cristian Martinez, Hideki Maeda","submitted_at":"2018-10-05T01:46:10Z","abstract_excerpt":"Energy conditions for matter fields are comprehensively investigated in arbitrary $n(\\ge 3)$ dimensions without specifying future and past directions locally. We classify an energy-momentum tensor into $n$-dimensional counterparts of the Hawking-Ellis type I to IV, where type III is defined by a more useful form than those adopted by Hawking and Ellis and other authors to identify the type-III energy-momentum tensor in a given spacetime. We also provide necessary and sufficient conditions for types I and II as inequalities for the orthonormal components of the energy-momentum tensor in a canon"},"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":"1810.02487","kind":"arxiv","version":5},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"gr-qc","submitted_at":"2018-10-05T01:46:10Z","cross_cats_sorted":["hep-th"],"title_canon_sha256":"e12a124d1a99eba02f90cf275b66c3f7e3ed5b0f5b733347acfe14123705ecf1","abstract_canon_sha256":"15f49fd4fe2ada87b4b67ca8763130236cdc5e8aeace59ca57f0c5ae27b32e2b"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T03:27:23.350714Z","signature_b64":"qMOApsUGF6Z6eU259Gzvz/OgT8/0yjof6jgZvGVFv9ayLVtVj/Y+jwxrdPETFvYRGWR9J6BFKJ0+gDM67nyOBA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"52a151814219f869db58ad7d0d6e86a844d1a49119a297680109714a3699d6b8","last_reissued_at":"2026-07-05T03:27:23.350259Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T03:27:23.350259Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Energy conditions in arbitrary dimensions","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["hep-th"],"primary_cat":"gr-qc","authors_text":"Cristian Martinez, Hideki Maeda","submitted_at":"2018-10-05T01:46:10Z","abstract_excerpt":"Energy conditions for matter fields are comprehensively investigated in arbitrary $n(\\ge 3)$ dimensions without specifying future and past directions locally. We classify an energy-momentum tensor into $n$-dimensional counterparts of the Hawking-Ellis type I to IV, where type III is defined by a more useful form than those adopted by Hawking and Ellis and other authors to identify the type-III energy-momentum tensor in a given spacetime. We also provide necessary and sufficient conditions for types I and II as inequalities for the orthonormal components of the energy-momentum tensor in a canon"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1810.02487","kind":"arxiv","version":5},"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/1810.02487/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":"1810.02487","created_at":"2026-07-05T03:27:23.350322+00:00"},{"alias_kind":"arxiv_version","alias_value":"1810.02487v5","created_at":"2026-07-05T03:27:23.350322+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1810.02487","created_at":"2026-07-05T03:27:23.350322+00:00"},{"alias_kind":"pith_short_12","alias_value":"KKQVDAKCDH4G","created_at":"2026-07-05T03:27:23.350322+00:00"},{"alias_kind":"pith_short_16","alias_value":"KKQVDAKCDH4GTW2Y","created_at":"2026-07-05T03:27:23.350322+00:00"},{"alias_kind":"pith_short_8","alias_value":"KKQVDAKC","created_at":"2026-07-05T03:27:23.350322+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2607.08088","citing_title":"An analytic model for a total process of gravitational collapse: From star to Schwarzschild black hole","ref_index":66,"is_internal_anchor":true},{"citing_arxiv_id":"2506.15798","citing_title":"Charged, rotating black holes in Einstein-Maxwell-dilaton theory","ref_index":42,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/KKQVDAKCDH4GTW2YVV6Q23UGVB","json":"https://pith.science/pith/KKQVDAKCDH4GTW2YVV6Q23UGVB.json","graph_json":"https://pith.science/api/pith-number/KKQVDAKCDH4GTW2YVV6Q23UGVB/graph.json","events_json":"https://pith.science/api/pith-number/KKQVDAKCDH4GTW2YVV6Q23UGVB/events.json","paper":"https://pith.science/paper/KKQVDAKC"},"agent_actions":{"view_html":"https://pith.science/pith/KKQVDAKCDH4GTW2YVV6Q23UGVB","download_json":"https://pith.science/pith/KKQVDAKCDH4GTW2YVV6Q23UGVB.json","view_paper":"https://pith.science/paper/KKQVDAKC","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1810.02487&json=true","fetch_graph":"https://pith.science/api/pith-number/KKQVDAKCDH4GTW2YVV6Q23UGVB/graph.json","fetch_events":"https://pith.science/api/pith-number/KKQVDAKCDH4GTW2YVV6Q23UGVB/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/KKQVDAKCDH4GTW2YVV6Q23UGVB/action/timestamp_anchor","attest_storage":"https://pith.science/pith/KKQVDAKCDH4GTW2YVV6Q23UGVB/action/storage_attestation","attest_author":"https://pith.science/pith/KKQVDAKCDH4GTW2YVV6Q23UGVB/action/author_attestation","sign_citation":"https://pith.science/pith/KKQVDAKCDH4GTW2YVV6Q23UGVB/action/citation_signature","submit_replication":"https://pith.science/pith/KKQVDAKCDH4GTW2YVV6Q23UGVB/action/replication_record"}},"created_at":"2026-07-05T03:27:23.350322+00:00","updated_at":"2026-07-05T03:27:23.350322+00:00"}