{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2024:WQJE4M7CNRYW2VFVPWGXC2XW3X","short_pith_number":"pith:WQJE4M7C","schema_version":"1.0","canonical_sha256":"b4124e33e26c716d54b57d8d716af6ddcc46fdf5ff055756498f0db30235495a","source":{"kind":"arxiv","id":"2403.09797","version":1},"attestation_state":"computed","paper":{"title":"Imprints of Barrow-Tsallis Cosmology in Primordial Gravitational Waves","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["hep-th"],"primary_cat":"gr-qc","authors_text":"Gaetano Lambiase, Giuseppe Gaetano Luciano, Leonardo Mastrototaro, Petr Jizba","submitted_at":"2024-03-14T18:30:41Z","abstract_excerpt":"Both the Barrow and Tsallis $\\delta$ entropies are one-parameter generalizations of the black-hole entropy, with the same microcanonical functional form. The ensuing deformation is quantified by a dimensionless parameter $\\Delta$, which in the case of Barrow entropy represents the anomalous dimension, while in Tsallis' case, it describes the deviation of the holographic scaling from extensivity. Here, we utilize the gravity-thermodynamics conjecture with the Barrow--Tsallis entropy to investigate the implications of the related modified Friedmann equations on the spectrum of primordial gravita"},"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":"2403.09797","kind":"arxiv","version":1},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"gr-qc","submitted_at":"2024-03-14T18:30:41Z","cross_cats_sorted":["hep-th"],"title_canon_sha256":"d7a383b9c02b86d375e21186c5dd4615421c5a00c159e6afec2b9bff48836b00","abstract_canon_sha256":"b0d74b8f702b2e0dc8f2bca00fed4cdb07ce3f0ce236f0f8cddef1edfe375c9d"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T09:25:41.493157Z","signature_b64":"PSK3FzFMRTtgHDaQR03GaISydFnX3DjXltVBNBJ+D0ixtcxjTTvmGdhgMwTjr1P3R/o/KIRHpHnr7figtwzCBw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"b4124e33e26c716d54b57d8d716af6ddcc46fdf5ff055756498f0db30235495a","last_reissued_at":"2026-07-05T09:25:41.492651Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T09:25:41.492651Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Imprints of Barrow-Tsallis Cosmology in Primordial Gravitational Waves","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["hep-th"],"primary_cat":"gr-qc","authors_text":"Gaetano Lambiase, Giuseppe Gaetano Luciano, Leonardo Mastrototaro, Petr Jizba","submitted_at":"2024-03-14T18:30:41Z","abstract_excerpt":"Both the Barrow and Tsallis $\\delta$ entropies are one-parameter generalizations of the black-hole entropy, with the same microcanonical functional form. The ensuing deformation is quantified by a dimensionless parameter $\\Delta$, which in the case of Barrow entropy represents the anomalous dimension, while in Tsallis' case, it describes the deviation of the holographic scaling from extensivity. Here, we utilize the gravity-thermodynamics conjecture with the Barrow--Tsallis entropy to investigate the implications of the related modified Friedmann equations on the spectrum of primordial gravita"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2403.09797","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/2403.09797/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":"2403.09797","created_at":"2026-07-05T09:25:41.492716+00:00"},{"alias_kind":"arxiv_version","alias_value":"2403.09797v1","created_at":"2026-07-05T09:25:41.492716+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2403.09797","created_at":"2026-07-05T09:25:41.492716+00:00"},{"alias_kind":"pith_short_12","alias_value":"WQJE4M7CNRYW","created_at":"2026-07-05T09:25:41.492716+00:00"},{"alias_kind":"pith_short_16","alias_value":"WQJE4M7CNRYW2VFV","created_at":"2026-07-05T09:25:41.492716+00:00"},{"alias_kind":"pith_short_8","alias_value":"WQJE4M7C","created_at":"2026-07-05T09:25:41.492716+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2603.03568","citing_title":"Observational constraints on Luciano-Saridakis entropic cosmology","ref_index":72,"is_internal_anchor":false},{"citing_arxiv_id":"2605.21050","citing_title":"Constraints on Kaniadakis Cosmology from Starobinsky Inflation and Primordial Tensor Perturbations","ref_index":17,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/WQJE4M7CNRYW2VFVPWGXC2XW3X","json":"https://pith.science/pith/WQJE4M7CNRYW2VFVPWGXC2XW3X.json","graph_json":"https://pith.science/api/pith-number/WQJE4M7CNRYW2VFVPWGXC2XW3X/graph.json","events_json":"https://pith.science/api/pith-number/WQJE4M7CNRYW2VFVPWGXC2XW3X/events.json","paper":"https://pith.science/paper/WQJE4M7C"},"agent_actions":{"view_html":"https://pith.science/pith/WQJE4M7CNRYW2VFVPWGXC2XW3X","download_json":"https://pith.science/pith/WQJE4M7CNRYW2VFVPWGXC2XW3X.json","view_paper":"https://pith.science/paper/WQJE4M7C","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2403.09797&json=true","fetch_graph":"https://pith.science/api/pith-number/WQJE4M7CNRYW2VFVPWGXC2XW3X/graph.json","fetch_events":"https://pith.science/api/pith-number/WQJE4M7CNRYW2VFVPWGXC2XW3X/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/WQJE4M7CNRYW2VFVPWGXC2XW3X/action/timestamp_anchor","attest_storage":"https://pith.science/pith/WQJE4M7CNRYW2VFVPWGXC2XW3X/action/storage_attestation","attest_author":"https://pith.science/pith/WQJE4M7CNRYW2VFVPWGXC2XW3X/action/author_attestation","sign_citation":"https://pith.science/pith/WQJE4M7CNRYW2VFVPWGXC2XW3X/action/citation_signature","submit_replication":"https://pith.science/pith/WQJE4M7CNRYW2VFVPWGXC2XW3X/action/replication_record"}},"created_at":"2026-07-05T09:25:41.492716+00:00","updated_at":"2026-07-05T09:25:41.492716+00:00"}