{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:1994:75HBCUWEAFCRRZEF5SG5KQHZGF","short_pith_number":"pith:75HBCUWE","schema_version":"1.0","canonical_sha256":"ff4e1152c4014518e485ec8dd540f9317a77cdb6c668b307d49c95c19d9bac0f","source":{"kind":"arxiv","id":"astro-ph/9406013","version":2},"attestation_state":"computed","paper":{"title":"Perturbative Lagrangian Approach to Gravitational Instability","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"E. Hivon, F.R. Bouchet, R. Juszkiewicz, S. Colombi","submitted_at":"1994-06-06T10:30:24Z","abstract_excerpt":"This paper deals with the time evolution in the matter era of perturbations in Friedman-Lemaitre models with arbitrary density parameter $\\Omega$, with either a zero cosmological constant, $\\Lambda = 0$, or with a non-zero cosmological constant in a spatially flat Universe. Unlike the classical Eulerian approach where the density contrast is expanded in a perturbative series, this analysis relies instead on a perturbative expansion of particles trajectories in Lagrangian coordinates. This brings a number of advantages over the classical analysis. In particular, it enables the description of st"},"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":"astro-ph/9406013","kind":"arxiv","version":2},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"1994-06-06T10:30:24Z","cross_cats_sorted":[],"title_canon_sha256":"9d53c60dbe0f09c9ce9a8d2ccccb7821cc2336b042316d81a79c4d2ca9c96f56","abstract_canon_sha256":"ce3a23fe3ec132e4cdafca41a1163f08d26f1d99d8fee036603a95b990e2700b"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T04:21:41.242118Z","signature_b64":"JaBjMc6DYQwp3l7QUKBGkK8E+ZNAtT5XUtj85hlyuiVZm3sC7+FZR2//DeMZ1MhePOCp/uoF/CW4DTdiIVs8Cw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"ff4e1152c4014518e485ec8dd540f9317a77cdb6c668b307d49c95c19d9bac0f","last_reissued_at":"2026-05-18T04:21:41.241478Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T04:21:41.241478Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Perturbative Lagrangian Approach to Gravitational Instability","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"E. Hivon, F.R. Bouchet, R. Juszkiewicz, S. Colombi","submitted_at":"1994-06-06T10:30:24Z","abstract_excerpt":"This paper deals with the time evolution in the matter era of perturbations in Friedman-Lemaitre models with arbitrary density parameter $\\Omega$, with either a zero cosmological constant, $\\Lambda = 0$, or with a non-zero cosmological constant in a spatially flat Universe. Unlike the classical Eulerian approach where the density contrast is expanded in a perturbative series, this analysis relies instead on a perturbative expansion of particles trajectories in Lagrangian coordinates. This brings a number of advantages over the classical analysis. In particular, it enables the description of st"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/9406013","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":"astro-ph/9406013","created_at":"2026-05-18T04:21:41.241567+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/9406013v2","created_at":"2026-05-18T04:21:41.241567+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/9406013","created_at":"2026-05-18T04:21:41.241567+00:00"},{"alias_kind":"pith_short_12","alias_value":"75HBCUWEAFCR","created_at":"2026-05-18T12:25:47.102015+00:00"},{"alias_kind":"pith_short_16","alias_value":"75HBCUWEAFCRRZEF","created_at":"2026-05-18T12:25:47.102015+00:00"},{"alias_kind":"pith_short_8","alias_value":"75HBCUWE","created_at":"2026-05-18T12:25:47.102015+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":4,"internal_anchor_count":2,"sample":[{"citing_arxiv_id":"2301.09655","citing_title":"Perturbation-theory informed integrators for cosmological simulations","ref_index":41,"is_internal_anchor":true},{"citing_arxiv_id":"2509.18971","citing_title":"Post-collapse Lagrangian perturbation theory in three dimensions","ref_index":11,"is_internal_anchor":true},{"citing_arxiv_id":"2604.11481","citing_title":"Emergence of Complex Web Structures","ref_index":41,"is_internal_anchor":false},{"citing_arxiv_id":"2604.18209","citing_title":"Galaxy Populations in the IllustrisTNG Caustic Skeleton","ref_index":29,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/75HBCUWEAFCRRZEF5SG5KQHZGF","json":"https://pith.science/pith/75HBCUWEAFCRRZEF5SG5KQHZGF.json","graph_json":"https://pith.science/api/pith-number/75HBCUWEAFCRRZEF5SG5KQHZGF/graph.json","events_json":"https://pith.science/api/pith-number/75HBCUWEAFCRRZEF5SG5KQHZGF/events.json","paper":"https://pith.science/paper/75HBCUWE"},"agent_actions":{"view_html":"https://pith.science/pith/75HBCUWEAFCRRZEF5SG5KQHZGF","download_json":"https://pith.science/pith/75HBCUWEAFCRRZEF5SG5KQHZGF.json","view_paper":"https://pith.science/paper/75HBCUWE","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/9406013&json=true","fetch_graph":"https://pith.science/api/pith-number/75HBCUWEAFCRRZEF5SG5KQHZGF/graph.json","fetch_events":"https://pith.science/api/pith-number/75HBCUWEAFCRRZEF5SG5KQHZGF/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/75HBCUWEAFCRRZEF5SG5KQHZGF/action/timestamp_anchor","attest_storage":"https://pith.science/pith/75HBCUWEAFCRRZEF5SG5KQHZGF/action/storage_attestation","attest_author":"https://pith.science/pith/75HBCUWEAFCRRZEF5SG5KQHZGF/action/author_attestation","sign_citation":"https://pith.science/pith/75HBCUWEAFCRRZEF5SG5KQHZGF/action/citation_signature","submit_replication":"https://pith.science/pith/75HBCUWEAFCRRZEF5SG5KQHZGF/action/replication_record"}},"created_at":"2026-05-18T04:21:41.241567+00:00","updated_at":"2026-05-18T04:21:41.241567+00:00"}