{"paper":{"title":"Conserved Quantities in Perturbed Inflationary Universes","license":"","headline":"","cross_cats":[],"primary_cat":"gr-qc","authors_text":"Marco Bruni, Peter Dunsby","submitted_at":"1994-05-04T16:11:16Z","abstract_excerpt":"Given that observations seem to favour a \\index{density parameter} $\\Omega_0<1$, corresponding to an open universe, we consider gauge\\hs invariant perturbations of non\\hs flat Robertson\\hs Walker universes filled with a general imperfect fluid which can also be taken to represent a scalar field. Our aim is to set up the equations that govern the evolution of the density perturbations $\\Delta$ so that it can be determined through a {\\it first order differential equation} with a quantity $\\kk$ which is conserved at any length scale, even in non\\hs flat universe models, acting as a source term. T"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"gr-qc/9405008","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"}