New simulations show dust-trapping, ringlike structures could help explain our solar system’s architecture.
In protoplanetary disks — the gas and dust clouds from which planets are made — the orbits of millimeter-sized dust particles drift inward. If these pebbles don’t accumulate in certain regions of the disk where they can collide and stick together to grow planetesimals, which are kilometer-sized, planet-forming rocks, they will be engulfed by the star.
star’s disk that has pebbles concentrated in ringlike locations — a feature possibly shared by the disk that formed our own solar system.In protoplanetary disks, dust grains drift toward regions of higher pressure, typically occupied by the star. But this drift can decelerate or even reverse if the gas pressure in the disk increases locally.
There’s also the possibility that dust traps can form in regions of the disk where there are no planets. In a recent, André Izidoro, an astrophysicist at Rice University, and colleagues found that our solar system’s protoplanetary disk may have possessed up to three rings of planetesimals located at regions known as ‘snow lines,’ where compounds sublimate or transform from a solid to gas state.
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