{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2014:3YYL4WUHFCULTIY4YO2CJFR2TU","short_pith_number":"pith:3YYL4WUH","schema_version":"1.0","canonical_sha256":"de30be5a8728a8b9a31cc3b424963a9d2c4da9e93e0478f99b86febd64fb9c6f","source":{"kind":"arxiv","id":"1405.5538","version":2},"attestation_state":"computed","paper":{"title":"How Many $e$-Folds Should We Expect from High-Scale Inflation?","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO","gr-qc"],"primary_cat":"hep-th","authors_text":"Grant N. Remmen, Sean M. Carroll","submitted_at":"2014-05-21T20:00:15Z","abstract_excerpt":"We address the issue of how many $e$-folds we would naturally expect if inflation occurred at an energy scale of order $10^{16}$ GeV. We use the canonical measure on trajectories in classical phase space, specialized to the case of flat universes with a single scalar field. While there is no exact analytic expression for the measure, we are able to derive conditions that determine its behavior. For a quadratic potential $V(\\phi)=m^{2}\\phi^{2}/2$ with $m=2\\times10^{13}$ GeV and cutoff at $M_{{\\rm Pl}}=2.4\\times10^{18}$ GeV, we find an expectation value of $2\\times10^{10}$ $e$-folds on the set o"},"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":"1405.5538","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"hep-th","submitted_at":"2014-05-21T20:00:15Z","cross_cats_sorted":["astro-ph.CO","gr-qc"],"title_canon_sha256":"046f8a986da9391a69751ed14a38273685756920c3656d18ce8d77a40a321742","abstract_canon_sha256":"2fc10c32f723b0b494067e27e45e45b8bbc383327d0bcd2f640b2ad918777ad5"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:41:18.556518Z","signature_b64":"xDVhMWtRXNRYI8RlQV0kCB1x/jDJ5owEDARDUOGXTgj2PZ1hXDchuPjy4itO9Hs7/N/S5SAgQLDmUTOH7wKrDA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"de30be5a8728a8b9a31cc3b424963a9d2c4da9e93e0478f99b86febd64fb9c6f","last_reissued_at":"2026-05-18T02:41:18.556116Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:41:18.556116Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"How Many $e$-Folds Should We Expect from High-Scale Inflation?","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO","gr-qc"],"primary_cat":"hep-th","authors_text":"Grant N. Remmen, Sean M. Carroll","submitted_at":"2014-05-21T20:00:15Z","abstract_excerpt":"We address the issue of how many $e$-folds we would naturally expect if inflation occurred at an energy scale of order $10^{16}$ GeV. We use the canonical measure on trajectories in classical phase space, specialized to the case of flat universes with a single scalar field. While there is no exact analytic expression for the measure, we are able to derive conditions that determine its behavior. For a quadratic potential $V(\\phi)=m^{2}\\phi^{2}/2$ with $m=2\\times10^{13}$ GeV and cutoff at $M_{{\\rm Pl}}=2.4\\times10^{18}$ GeV, we find an expectation value of $2\\times10^{10}$ $e$-folds on the set o"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1405.5538","kind":"arxiv","version":2},"verdict":{"id":null,"model_set":{},"created_at":null,"strongest_claim":"","one_line_summary":"","pipeline_version":null,"weakest_assumption":"","pith_extraction_headline":""},"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":"1405.5538","created_at":"2026-05-18T02:41:18.556174+00:00"},{"alias_kind":"arxiv_version","alias_value":"1405.5538v2","created_at":"2026-05-18T02:41:18.556174+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1405.5538","created_at":"2026-05-18T02:41:18.556174+00:00"},{"alias_kind":"pith_short_12","alias_value":"3YYL4WUHFCUL","created_at":"2026-05-18T12:28:11.866339+00:00"},{"alias_kind":"pith_short_16","alias_value":"3YYL4WUHFCULTIY4","created_at":"2026-05-18T12:28:11.866339+00:00"},{"alias_kind":"pith_short_8","alias_value":"3YYL4WUH","created_at":"2026-05-18T12:28:11.866339+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2605.21050","citing_title":"Constraints on Kaniadakis Cosmology from Starobinsky Inflation and Primordial Tensor Perturbations","ref_index":78,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/3YYL4WUHFCULTIY4YO2CJFR2TU","json":"https://pith.science/pith/3YYL4WUHFCULTIY4YO2CJFR2TU.json","graph_json":"https://pith.science/api/pith-number/3YYL4WUHFCULTIY4YO2CJFR2TU/graph.json","events_json":"https://pith.science/api/pith-number/3YYL4WUHFCULTIY4YO2CJFR2TU/events.json","paper":"https://pith.science/paper/3YYL4WUH"},"agent_actions":{"view_html":"https://pith.science/pith/3YYL4WUHFCULTIY4YO2CJFR2TU","download_json":"https://pith.science/pith/3YYL4WUHFCULTIY4YO2CJFR2TU.json","view_paper":"https://pith.science/paper/3YYL4WUH","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1405.5538&json=true","fetch_graph":"https://pith.science/api/pith-number/3YYL4WUHFCULTIY4YO2CJFR2TU/graph.json","fetch_events":"https://pith.science/api/pith-number/3YYL4WUHFCULTIY4YO2CJFR2TU/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/3YYL4WUHFCULTIY4YO2CJFR2TU/action/timestamp_anchor","attest_storage":"https://pith.science/pith/3YYL4WUHFCULTIY4YO2CJFR2TU/action/storage_attestation","attest_author":"https://pith.science/pith/3YYL4WUHFCULTIY4YO2CJFR2TU/action/author_attestation","sign_citation":"https://pith.science/pith/3YYL4WUHFCULTIY4YO2CJFR2TU/action/citation_signature","submit_replication":"https://pith.science/pith/3YYL4WUHFCULTIY4YO2CJFR2TU/action/replication_record"}},"created_at":"2026-05-18T02:41:18.556174+00:00","updated_at":"2026-05-18T02:41:18.556174+00:00"}