We also aim to compare the radial extent of the gas and dust emission in disks around VLMS, which can give us insight about radial drift. We aim to estimate if structures, such as cavities, rings, and gaps, are common in disks around VLMS and to test models of structure formation in these disks. Specifically, radial drift of dust particles is a catastrophic barrier in these disks, which prevents the formation of planetesimals and therefore planets.Īims. The discovery of giant planets orbiting very low mass stars (VLMS) and the recent observed substructures in disks around VLMS is challenging planet formation models. SUPA, School of Physics & Astronomy, University of St. Lunar and Planetary Laboratory, The University of Arizona,Įarths in Other Solar Systems Team, NASA Nexus for Exoplanet System Science, Tucson, Arizona, USAĭepartment of Physics and Astronomy, California State University Northridge, Unidad Mixta Internacional Franco-Chilena de Astronomía, CNRS/INSU UMI 3386, Departamento de Astronomía, Universidad de Chile, Camino El Observatorio 1515, Las Condes,ĭublin Institute for Advanced Studies, School of Cosmic Physics, Testi 5 ,11Į-mail: for Astrophysics ∣ Harvard & Smithsonian, Astronomical objects: linking to databases.Including author names using non-Roman alphabets.Suggested resources for more tips on language editing in the sciences
Punctuation and style concerns regarding equations, figures, tables, and footnotes
0 kommentar(er)
