{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2020:JE2ZEWU4CA7XP4SAC5WGDQENFO","short_pith_number":"pith:JE2ZEWU4","schema_version":"1.0","canonical_sha256":"4935925a9c103f77f240176c61c08d2ba455cc76831a2351b59c6509e5f1537c","source":{"kind":"arxiv","id":"2012.04342","version":1},"attestation_state":"computed","paper":{"title":"Non-minimal Higgs inflation within holographic cosmology","license":"http://creativecommons.org/publicdomain/zero/1.0/","headline":"","cross_cats":[],"primary_cat":"gr-qc","authors_text":"Aatifa Bargach, Farida Bargach, Mariam Bouhmadi-L\\'opez, Taoufik Ouali","submitted_at":"2020-12-08T10:30:49Z","abstract_excerpt":"We derive a Higgs inflationary model in the context of holographic cosmology, where we consider a universe filled with a Higgs field non-minimally coupled to gravity in a slow-roll regime. The amplitude of density (scalar) perturbations is calculated. In this regard, we show that the background and perturbative parameters characterising the inflationary era are related to the standard one through corrections terms. We found that for the e-fold number $N\\sim 58$, the spectral index,$n_{r}$, and the tensor-to-scalar ratio,$r$, values are $0.965$ and $0.021$, respectively, which are in agreement "},"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":"2012.04342","kind":"arxiv","version":1},"metadata":{"license":"http://creativecommons.org/publicdomain/zero/1.0/","primary_cat":"gr-qc","submitted_at":"2020-12-08T10:30:49Z","cross_cats_sorted":[],"title_canon_sha256":"e2d585c4bb6d36c3761dae893429c5eded71b77698a66a623d85d383b17a3b94","abstract_canon_sha256":"a475713b3e4253e898a0bdee8458098cc1043f57cc0b04888027a7eec0af6385"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T02:10:07.485661Z","signature_b64":"TphDj0sE20187hE/CegXfqxHZwP7Aoeo6PBrsK4SH64qnyy06ZqLzIyIGPjGclNqHMHLcb7ryU+ynTuXh11MAA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"4935925a9c103f77f240176c61c08d2ba455cc76831a2351b59c6509e5f1537c","last_reissued_at":"2026-07-05T02:10:07.485233Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T02:10:07.485233Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Non-minimal Higgs inflation within holographic cosmology","license":"http://creativecommons.org/publicdomain/zero/1.0/","headline":"","cross_cats":[],"primary_cat":"gr-qc","authors_text":"Aatifa Bargach, Farida Bargach, Mariam Bouhmadi-L\\'opez, Taoufik Ouali","submitted_at":"2020-12-08T10:30:49Z","abstract_excerpt":"We derive a Higgs inflationary model in the context of holographic cosmology, where we consider a universe filled with a Higgs field non-minimally coupled to gravity in a slow-roll regime. The amplitude of density (scalar) perturbations is calculated. In this regard, we show that the background and perturbative parameters characterising the inflationary era are related to the standard one through corrections terms. We found that for the e-fold number $N\\sim 58$, the spectral index,$n_{r}$, and the tensor-to-scalar ratio,$r$, values are $0.965$ and $0.021$, respectively, which are in agreement "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2012.04342","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/2012.04342/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":"2012.04342","created_at":"2026-07-05T02:10:07.485288+00:00"},{"alias_kind":"arxiv_version","alias_value":"2012.04342v1","created_at":"2026-07-05T02:10:07.485288+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2012.04342","created_at":"2026-07-05T02:10:07.485288+00:00"},{"alias_kind":"pith_short_12","alias_value":"JE2ZEWU4CA7X","created_at":"2026-07-05T02:10:07.485288+00:00"},{"alias_kind":"pith_short_16","alias_value":"JE2ZEWU4CA7XP4SA","created_at":"2026-07-05T02:10:07.485288+00:00"},{"alias_kind":"pith_short_8","alias_value":"JE2ZEWU4","created_at":"2026-07-05T02:10:07.485288+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2604.04764","citing_title":"Gravitational waves production during preheating within GB gravity with monomial coupling","ref_index":8,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/JE2ZEWU4CA7XP4SAC5WGDQENFO","json":"https://pith.science/pith/JE2ZEWU4CA7XP4SAC5WGDQENFO.json","graph_json":"https://pith.science/api/pith-number/JE2ZEWU4CA7XP4SAC5WGDQENFO/graph.json","events_json":"https://pith.science/api/pith-number/JE2ZEWU4CA7XP4SAC5WGDQENFO/events.json","paper":"https://pith.science/paper/JE2ZEWU4"},"agent_actions":{"view_html":"https://pith.science/pith/JE2ZEWU4CA7XP4SAC5WGDQENFO","download_json":"https://pith.science/pith/JE2ZEWU4CA7XP4SAC5WGDQENFO.json","view_paper":"https://pith.science/paper/JE2ZEWU4","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2012.04342&json=true","fetch_graph":"https://pith.science/api/pith-number/JE2ZEWU4CA7XP4SAC5WGDQENFO/graph.json","fetch_events":"https://pith.science/api/pith-number/JE2ZEWU4CA7XP4SAC5WGDQENFO/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/JE2ZEWU4CA7XP4SAC5WGDQENFO/action/timestamp_anchor","attest_storage":"https://pith.science/pith/JE2ZEWU4CA7XP4SAC5WGDQENFO/action/storage_attestation","attest_author":"https://pith.science/pith/JE2ZEWU4CA7XP4SAC5WGDQENFO/action/author_attestation","sign_citation":"https://pith.science/pith/JE2ZEWU4CA7XP4SAC5WGDQENFO/action/citation_signature","submit_replication":"https://pith.science/pith/JE2ZEWU4CA7XP4SAC5WGDQENFO/action/replication_record"}},"created_at":"2026-07-05T02:10:07.485288+00:00","updated_at":"2026-07-05T02:10:07.485288+00:00"}