2019/11/01 by Alessia Franchini, Rebecca G. Martin, Stephen H. Lubow · 14 citations
Physics and Astronomy · #Astro and Planetary Science #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Circumbinary planet #Eccentricity (behavior) #Geometry #Orbit (dynamics) #Physics #Planet #Planetary system #Stellar, planetary, and galactic studies #Tilt (camera) #astro-ph.EP #astro-ph.SR
paper · pdf · doi:10.1093/mnras/stz3175
published in Monthly Notices of the Royal Astronomical Society 491(4), 5351-5360 (Oxford University Press) · Accepted for publication in MNRAS
arxiv created 2019/11/01 · openalex publication_date 2019/11/22 · arxiv updated 2020/01/08 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
ABSTRACT We investigate the evolution of a multiplanet–disc system orbiting one component of a binary star system. The planet–disc system is initially coplanar but misaligned to the binary orbital plane. The planets are assumed to be giants that open gaps in the disc. We first study the role of the disc in shaping the mutual evolution of the two planets using a secular model for low initial tilt. In general, we find that the planets and the disc do not remain coplanar, in agreement with previous work on the single planet case. Instead, the planets and the disc undergo tilt oscillations. A high-mass disc between the two planets causes the planets and the disc to nodally precess at the same average rate but they are generally misaligned. The amplitude of the tilt oscillations between the planets is larger while the disc is present. We then consider higher initial tilts using hydrodynamical simulations and explore the possibility of the formation of eccentric Kozai–Lidov (KL) planets. We find that the inner planet’s orbit undergoes eccentricity growth for a large range of disc masses and initial misalignments. For a low disc mass and large initial misalignment, both planets and the disc can undergo KL oscillations. Furthermore, we find that sufficiently massive discs can cause the inner planet to increase its inclination beyond 90° and therefore to orbit the binary in a retrograde fashion. The results have important implications for the explanation of very eccentric planets and retrograde planets observed in multiplanet systems.