Pebble drift plays a central role in modern planet formation models. In this work we carry out planet formation simulations (including pebble accretion and migration) for a range of disc […]
![[LEFT] Final planet mass vs pebble flux across the snowline at time of insertion. Plots A and B are coloured by the planet’s initial and final semi-major axes respectively. Plot C is coloured by the planet’s insertion time 𝑡0, and plot D is coloured by the characteristic disk radius 𝑅0. Plot E is coloured by the disk’s 𝛼 parameter, and plot F is coloured by the fragmentation velocity 𝑣frag. All plots contain outlined numbered points, which correspond to the points numbered in Fig. 2. [RIGHT Final planet mass vs pebble flux across the snowline at 1 Myr. Plots A and B are coloured by the planet’s final and initial semi-major axes respectively. Plot C is coloured by the planet’s insertion time 𝑡0, and plot D is coloured by the characteristic disk radius 𝑅0. Plot E is coloured by the disk’s 𝛼 parameter, and plot F is coloured by the fragmentation velocity 𝑣frag. All plots contain outlined numbered points, which correspond to the points numbered in Fig. 2. -- astro-ph.EP](https://i0.wp.com/astrobiology.com/wp-content/uploads/2026/04/Simulating-the-interplay.png?resize=1200%2C760&ssl=1)
Pebble drift plays a central role in modern planet formation models. In this work we carry out planet formation simulations (including pebble accretion and migration) for a range of disc […]