2020/09/18 by Rebecca Nealon, Nicolás Cuello, Jean-François Gonzalez +9 · 22 citations
Physics and Astronomy · #Astro and Planetary Science #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Circular orbit #Orbit (dynamics) #Outer planets #Physics #Planet #Precession #Stellar, planetary, and galactic studies #astro-ph.EP #astro-ph.GA #astro-ph.SR
paper · pdf · doi:10.1093/mnras/staa2721
published in Monthly Notices of the Royal Astronomical Society 499(3), 3857-3867 (Oxford University Press) · Accepted for publication in MNRAS, 12 pages, 6 figures. Movie of simulations available at https://youtu.be/MvH8TO21W_4
openalex publication_date 2020/09/18 · arxiv created 2020/09/22 · arxiv updated 2020/10/07 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
ABSTRACT The protoplanetary disc HD 100453 exhibits a curious combination of spirals, shadows, and a relative misalignment between the observed outer disc and inferred inner disc. This disc is accompanied by a secondary star on a bound orbit exterior to the disc. Recent observations have suggested there may be an additional low-mass companion residing within the disc inner cavity. In our companion paper, the orbit of the secondary was shown to be misaligned by 61° to the plane of the outer disc. Here, we investigate the properties of the inner companion and the origin of the misalignment between the inner and outer discs. Using numerical simulations and synthetic observations, we show that the disc structure and kinematics are consistent with a ≲ 5 MJ planet located at 15 − 20 au. We find that the disc evolution over ∼50 binary orbits (∼105 yr) is governed by differential precession and to a lesser extent, the Kozai–Lidov effect. In our proposed model, the misalignment observed between the outer and inner disc arises naturally as a result of the misaligned outer companion driving the outer disc to precess more rapidly than the inner disc.