{"paper":{"title":"The California-Kepler Survey. III. A Gap in the Radius Distribution of Small Planets","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.EP","authors_text":"Andrew W. Howard, Benjamin J. Fulton, Erik A. Petigura, Evan Sinukoff, Geoffrey W. Marcy, Howard Isaacson, Ian J. M. Crossfield, John Asher Johnson, Lauren M. Weiss, Lea A. Hirsch, Leslie Hebb, Phillip A. Cargile, Timothy D. Morton","submitted_at":"2017-03-30T09:25:04Z","abstract_excerpt":"The size of a planet is an observable property directly connected to the physics of its formation and evolution. We used precise radius measurements from the California-Kepler Survey (CKS) to study the size distribution of 2025 $\\textit{Kepler}$ planets in fine detail. We detect a factor of $\\geq$2 deficit in the occurrence rate distribution at 1.5-2.0 R$_{\\oplus}$. This gap splits the population of close-in ($P$ < 100 d) small planets into two size regimes: R$_P$ < 1.5 R$_{\\oplus}$ and R$_P$ = 2.0-3.0 R$_{\\oplus}$, with few planets in between. Planets in these two regimes have nearly the same"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1703.10375","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"}