{"paper":{"title":"3D AMR simulations of G2 as an outflow","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"A. Ballone, A. Burkert, E. M. George, F. Eisenhauer, M. Habibi, M. Schartmann, O. Pfuhl, P. M. Plewa, R. Genzel, S. Gillessen, T. Ott","submitted_at":"2016-09-23T11:27:29Z","abstract_excerpt":"We study the evolution of G2 in a \\textit{Compact Source Scenario}, where G2 is the outflow from a low-mass central star moving on the observed orbit. This is done through 3D AMR simulations of the hydrodynamic interaction of G2 with the surrounding hot accretion flow. A comparison with observations is done by means of mock position-velocity (PV) diagrams. We found that a massive ($\\dot{M}_\\mathrm{w}=5\\times 10^{-7} \\;M_{\\odot} \\; \\mathrm{yr^{-1}}$) and slow ($v_\\mathrm{w}=50 \\;\\mathrm{km\\; s^{-1}}$) outflow can reproduce G2's properties. A faster outflow ($v_\\mathrm{w}=400 \\;\\mathrm{km\\; s^{-"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1609.07318","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"}