Formation of planetary systems by pebble accretion and migration: Hot super-Earth systems from breaking compact resonant chains

2019/01/01 by André Izidoro, Bertram Bitsch, Sean N. Raymond +5 · 1 citation
Physics and Astronomy · #Accretion (finance) #Astro and Planetary Science #Astrobiology #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Earth (classical element) #Geology #Giant planet #Physics #Planet #Planetary migration #Planetary system #Stellar, planetary, and galactic studies #Super-Earth #astro-ph.EP

paper · pdf · doi:10.1051/0004-6361/201935336

published as A&A 650, A152 (2021) · Accepted in A&A, version including language editing

openalex publication_date 2019/01/01 · arxiv created 2021/04/19 · arxiv updated 2021/06/23 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/08

Abstract

At least 30% of main sequence stars host planets with sizes between 1 and 4 Earth radii and orbital periods of less than 100 days. We use N-body simulations including a model for gas-assisted pebble accretion and disk-planet tidal interaction to study the formation of super-Earth systems. We show that the integrated pebble mass reservoir creates a bifurcation between hot super-Earths or hot-Neptunes ( lesssim15M_\⊕) and super-massive planetary cores potentially able to become gas giant planets ( gtrsim15M_\⊕). Simulations with moderate pebble fluxes grow multiple super-Earth-mass planets that migrate inwards and pile up at the disk's inner edge forming long resonant chains. We follow the long-term dynamical evolution of these systems and use the period ratio distribution of observed planet-pairs to constrain our model. Up to \∼95% of resonant chains become dynamically unstable after the gas disk dispersal, leading to a phase of late collisions that breaks the resonant configuration. Our simulations match observations if we combine a dominant fraction ( gtrsim95 %) of unstable systems with a sprinkling ( lesssim5 %) of stable resonant chains (the Trappist-1 system represents one such example). Our results demonstrate that super-Earth systems are inherently multiple ( rm N\≥2) and that the observed excess of single-planet transits is a consequence of the mutual inclinations excited by the planet-planet instability. In simulations in which planetary seeds are initially distributed in the inner and outer disk, close-in super-Earths are systematically ice-rich. This contrasts with the interpretation that most super-Earths are rocky based on bulk density measurements of super-Earths and photo-evaporation modeling of their bimodal radius distribution. We investigate the conditions needed to form rocky super-Earths. The formation of rocky super-Earths (abridged)

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