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We find that only the eternal inflation of chaotic type is possible for $c \\sim {\\cal O}(0.01)$ and $1/\\mathcal{D} \\sim {\\cal O}(0.01)$, and that the Hubble parameter during the eternal inflation is parametrically close to the Planc"},"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":"1807.11938","kind":"arxiv","version":3},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"hep-th","submitted_at":"2018-07-31T17:56:24Z","cross_cats_sorted":["astro-ph.CO","gr-qc","hep-ph"],"title_canon_sha256":"1dad193daafd07cecbd3739790f561b7a6615aa717e441e93247377cfbf44245","abstract_canon_sha256":"88b5504c09ff318c00c00c7d0ef1a1e86c727f66eb757228db0f876ecf996466"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-17T23:55:03.395282Z","signature_b64":"YaYp5KhecklY5dpQEJ01TpAbhvoVVFgGvghdpCmauGqAxz+szsKZKXi0fZpNTB7Qcfx1PhjM1OBvZyIGqZjNBA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"4e1f18ebb36c121aa27154751022bf39892a1a828ba5f7774b673e921e8db32f","last_reissued_at":"2026-05-17T23:55:03.394869Z","signature_status":"signed_v1","first_computed_at":"2026-05-17T23:55:03.394869Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Eternal Inflation and Swampland Conjectures","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO","gr-qc","hep-ph"],"primary_cat":"hep-th","authors_text":"Fuminobu Takahashi, Hiroki Matsui","submitted_at":"2018-07-31T17:56:24Z","abstract_excerpt":"We study if eternal inflation is realized while satisfying the recently proposed string Swampland criteria concerning the range of scalar field excursion, $|\\Delta \\phi| < \\mathcal{D} \\cdot M_{\\rm P}$, and the potential gradient, $|\\nabla V| > c \\cdot V/M_{\\rm P}$, where $\\mathcal{D}$ and $c$ are constants of order unity, and $M_{\\rm P}$ is the reduced Planck mass. 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