{"paper":{"title":"Pebble dynamics and accretion onto rocky planets. I. Adiabatic and convective models","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.EP","authors_text":"{\\AA}. Nordlund, A. Popovas, Chris W. Ormel, Jon P. Ramsey","submitted_at":"2018-01-23T18:54:01Z","abstract_excerpt":"We present nested-grid, high-resolution hydrodynamic simulations of gas and particle dynamics in the vicinity of Mars- to Earth-mass planetary embryos. The simulations extend from the surface of the embryos to a few vertical disk scale heights, with \\rev{a spatial} dynamic range \\rev{of} $\\sim\\! 1.4\\times 10^5$. Our results confirm that \"pebble\"-sized particles are readily accreted, with accretion rates continuing to increase up to metre-size \"boulders\" for a 10\\% MMSN surface density model. The gas mass flux in and out of the Hill sphere is consistent with the Hill rate, $\\Sigma\\Omega R_\\math"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1801.07707","kind":"arxiv","version":4},"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"}