Protoplanetary Disk Accretion (2D)

Disk Accretion

Time speed 6×

Dust density 220

Stickiness 55%

Gas disk

Snow line

Live Readout

Grains left

—

Sim time

0 kyr

Planetesimals

Protoplanets

Largest body

—

FPS

—

How it works

A top-down view of the same accretion model as the 3D version: every dust grain orbits the young star at a Keplerian angular speed (inner grains circle faster than outer ones), and grains that pass close enough merge with a probability set by the stickiness slider, conserving combined mass. As bodies cross size thresholds they graduate from dust to planetesimal to protoplanet.

Snow line — beyond it grains are icy (blue-white); inside it they're rocky (rust-brown).
Time speed — simulated millennia per real second.
Stickiness — probability that a close pass results in a merger.

Rocky grain Icy grain Planetesimal Protoplanet