{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2012:HEFVSLEXBJUO6LO3BVW4Q6OAUE","short_pith_number":"pith:HEFVSLEX","schema_version":"1.0","canonical_sha256":"390b592c970a68ef2ddb0d6dc879c0a1193474d8bdebbb7949f664c591149574","source":{"kind":"arxiv","id":"1210.7880","version":1},"attestation_state":"computed","paper":{"title":"Inflation and Birth of Cosmological Perturbations","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["gr-qc","hep-th"],"primary_cat":"astro-ph.CO","authors_text":"Misao Sasaki","submitted_at":"2012-10-30T01:33:10Z","abstract_excerpt":"We review recent developments in the theory of inflation and cosmological perturbations produced from inflation. After a brief introduction of the standard, single-field slow-roll inflation, and the curvature and tensor perturbations produced from it, we discuss possible sources of nonlinear, non-Gaussian perturbations in other models of inflation. Then we describe the so-called $\\delta N$ formalism, which is a powerful tool for evaluating nonlinear curvature perturbations on super Hubble scales."},"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":"1210.7880","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2012-10-30T01:33:10Z","cross_cats_sorted":["gr-qc","hep-th"],"title_canon_sha256":"c7d14029093c93d32641143d1fa67da477067dfa43d9cde9081c97f6e11aec6b","abstract_canon_sha256":"3d37c1e602098a6c4b80be07397e279605559ddbfc15f580a246f1305ac5fc70"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T03:41:57.876335Z","signature_b64":"XgwNZ8LwOVXTbIGf3zuEAayDZY8vy2VERzA3EzUGobHR3bp0g4WZe7pXd0pJN93OqTPh6SkhEJRVqj3k4XdPDw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"390b592c970a68ef2ddb0d6dc879c0a1193474d8bdebbb7949f664c591149574","last_reissued_at":"2026-05-18T03:41:57.875508Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T03:41:57.875508Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Inflation and Birth of Cosmological Perturbations","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["gr-qc","hep-th"],"primary_cat":"astro-ph.CO","authors_text":"Misao Sasaki","submitted_at":"2012-10-30T01:33:10Z","abstract_excerpt":"We review recent developments in the theory of inflation and cosmological perturbations produced from inflation. After a brief introduction of the standard, single-field slow-roll inflation, and the curvature and tensor perturbations produced from it, we discuss possible sources of nonlinear, non-Gaussian perturbations in other models of inflation. Then we describe the so-called $\\delta N$ formalism, which is a powerful tool for evaluating nonlinear curvature perturbations on super Hubble scales."},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1210.7880","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":""},"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":"1210.7880","created_at":"2026-05-18T03:41:57.875649+00:00"},{"alias_kind":"arxiv_version","alias_value":"1210.7880v1","created_at":"2026-05-18T03:41:57.875649+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1210.7880","created_at":"2026-05-18T03:41:57.875649+00:00"},{"alias_kind":"pith_short_12","alias_value":"HEFVSLEXBJUO","created_at":"2026-05-18T12:27:09.501522+00:00"},{"alias_kind":"pith_short_16","alias_value":"HEFVSLEXBJUO6LO3","created_at":"2026-05-18T12:27:09.501522+00:00"},{"alias_kind":"pith_short_8","alias_value":"HEFVSLEX","created_at":"2026-05-18T12:27:09.501522+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2604.24944","citing_title":"A general formalism for coupling scalar fields to the Einstein equations without a variational principle","ref_index":30,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/HEFVSLEXBJUO6LO3BVW4Q6OAUE","json":"https://pith.science/pith/HEFVSLEXBJUO6LO3BVW4Q6OAUE.json","graph_json":"https://pith.science/api/pith-number/HEFVSLEXBJUO6LO3BVW4Q6OAUE/graph.json","events_json":"https://pith.science/api/pith-number/HEFVSLEXBJUO6LO3BVW4Q6OAUE/events.json","paper":"https://pith.science/paper/HEFVSLEX"},"agent_actions":{"view_html":"https://pith.science/pith/HEFVSLEXBJUO6LO3BVW4Q6OAUE","download_json":"https://pith.science/pith/HEFVSLEXBJUO6LO3BVW4Q6OAUE.json","view_paper":"https://pith.science/paper/HEFVSLEX","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1210.7880&json=true","fetch_graph":"https://pith.science/api/pith-number/HEFVSLEXBJUO6LO3BVW4Q6OAUE/graph.json","fetch_events":"https://pith.science/api/pith-number/HEFVSLEXBJUO6LO3BVW4Q6OAUE/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/HEFVSLEXBJUO6LO3BVW4Q6OAUE/action/timestamp_anchor","attest_storage":"https://pith.science/pith/HEFVSLEXBJUO6LO3BVW4Q6OAUE/action/storage_attestation","attest_author":"https://pith.science/pith/HEFVSLEXBJUO6LO3BVW4Q6OAUE/action/author_attestation","sign_citation":"https://pith.science/pith/HEFVSLEXBJUO6LO3BVW4Q6OAUE/action/citation_signature","submit_replication":"https://pith.science/pith/HEFVSLEXBJUO6LO3BVW4Q6OAUE/action/replication_record"}},"created_at":"2026-05-18T03:41:57.875649+00:00","updated_at":"2026-05-18T03:41:57.875649+00:00"}