![CI mass as a function of radial distance from the host star, for a continuum of solid surface densities. Over-plotted is the FI1 mass (šĀ¤ = 10ā9 Mā yrā1 ) for a continuum of maximum Stokes numbers, as well as the MFI1 (opaque purple) and MFI2 (dashed red) masses and the PI mass (dotted black). The last three show no continuum of mass distributions, since we vary their initial mutual Hill spacing within the simulation. Thus, all initial simulations begin from the same mass distribution model, albeit with a different number of embryos at different spacings.-- [astro-ph.EP]](https://i0.wp.com/astrobiology.com/wp-content/uploads/2026/08/Effects-of-Pebble.png?resize=1200%2C715&ssl=1)
[astro-ph.EP] The Kepler Mission has discovered a plethora of planetary systems with super-Earth sized planets.
Planetesimal Accretion
Posted inAstrogeology, Exoplanets, -moons, -comets, Status Report, TRAPPIST-1
Forming Earth-like and Low-Mass Rocky Exoplanets Through Pebble and Planetesimal Accretion
The theory of pebble accretion (PA) has become a popular planet formation theory during the past decade. However, PA studies generally rely on large planetary embryos, much larger than those […]