2019/11/19 by Claudia Toci, Giuseppe Lodato, Davide Fedele +2 · 35 citations
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysics and Star Formation Studies #Brightness #Circumstellar dust #Debris disk #Dust lane #Giant planet #Planet #Planetary system #Planetesimal #Radiative transfer #Stellar, planetary, and galactic studies #astro-ph.EP #astro-ph.SR
paper · pdf · doi:10.3847/2041-8213/ab5c87
published in The Astrophysical Journal Letters 888(1), L4 (IOP Publishing) · 8 pages, 5 figures, accepted Apj Letters
arxiv created 2019/11/19 · openalex created_date 2019/12/05 · openalex publication_date 2019/12/27 · arxiv updated 2020/01/08 · openalex updated_date 2026/08/05
Abstract Recent Atacama Large Millimeter/submillimeter Array (ALMA) observations of the protoplanetary disk around HD 169142 reveal a peculiar structure made of concentric dusty rings: a main ring at ∼20 au, a triple system of rings at ∼55–75 au in millimetric continuum emission, and a perturbed gas surface density from the 12 CO, 13 CO, and C 18 O ( J = 2–1) surface brightness profile. In this Letter, we perform 3D numerical simulations and radiative transfer modeling exploring the possibility that two giant planets interacting with the disk and orbiting in resonant locking can be responsible for the origin of the observed dust inner rings structure. We find that in this configuration the dust structure is actually long lived while the gas mass of the disk is accreted onto the star and the giant planets, emptying the inner region. In addition, we also find that the innermost planet is located at the inner edge of the dust ring, and can accrete mass from the disk, generating a signature in the dust ring shape that can be observed in mm ALMA observations.