Collisional Growth Within the Solar System's Primordial Planetesimal Disk and the Timing of the Giant Planet Instability
arXiv:2107.10403 · doi:10.3847/2041-8213/ac1681
Abstract
The large scale structure of the Solar System has been shaped by a transient dynamical instability that may have been triggered by the interaction of the giants planets with a massive primordial disk of icy debris. In this work, we investigate the conditions under which this primordial disk could have coalesced into planets using analytic and numerical calculations. In particular, we perform numerical simulations of the Solar System's early dynamical evolution that account for the viscous stirring and collisional damping within the disk. We demonstrate that if collisional damping would have been sufficient to maintain a temperate velocity dispersion, Earth mass trans-Neptunian planets could have emerged within a timescale of 10 Myr. Therefore, our results favor a scenario wherein the dynamical instability of the outer Solar System began immediately upon the dissipation of the gaseous nebula to avoid the overproduction of Earth mass planets in the outer Solar System.
arXiv comment8 pages, 4 figures, 1 table, accepted for publication in ApJL
References in corpus (26)
- Array Programming with NumPy
- Rapid planetesimal formation in turbulent circumstellar discs
- Streaming Instabilities in Protoplanetary Disks
- Rapid growth of gas-giant cores by pebble accretion
- Origin of the Structure of the Kuiper Belt during a Dynamical Instability in the Orbits of Uranus and Neptune
- Statistical Study of the Early Solar System's Instability with 4, 5 and 6 Giant Planets
- On the orbital evolution and growth of protoplanets embedded in a gaseous disc
- Dynamical Evolution of the Early Solar System
- Capture of Trojans by Jumping Jupiter
- Mars' Growth Stunted by an Early Giant Planet Instability
- Debris disks as signposts of terrestrial planet formation
- Retention of a Primordial Cold Classical Kuiper Belt in an Instability-Driven Model of Solar System Formation
- WISE/NEOWISE Observations of the Jovian Trojans: Preliminary Results
- Jumping Neptune Can Explain the Kuiper Belt Kernel
- Early Dynamical Evolution of the Solar System: Pinning Down the Initial Condition of the Nice Model
- The early instability scenario: terrestrial planet formation during the giant planet instability, and the effect of collisional fragmentation
- The GENGA Code: Gravitational Encounters in N-body simulations with GPU Acceleration
- Dynamical evidence for an early giant planet instability
- Accretion among preplanetary bodies: the many faces of runaway growth
- The Role of Early Giant Planet Instability in the Terrestrial Planet Formation
- Instabilities in the Early Solar System due to a Self-gravitating Disk
- Checking the Compatibility of the Cold Kuiper Belt with a Planetary Instability Migration Model
- Simulations of the Solar System's Early Dynamical Evolution with a Self-Gravitating Planetesimal Disk
- Limits on the number of primordial Scattered Disk objects at Pluto mass and higher from the absence of their dynamical signatures on the present day trans-Neptunian Populations
- Stability of the Outer Planets in Multiresonant Configurations with a Self-gravitating Planetesimal Disk
- Superparticle Method for Simulating Collisions