A research team studies binaries to make heads or tails of planet formation

3D simulations of the streaming instability model of planet formation. Credit: HST/StSci/SwRI/Simon Porter.

A Southwest Research Institute-led team studied the orientation of distant solar system bodies to bolster the "streaming instability" theory of planet formation. 

"One of the least understood steps in planet growth is the formation of planetesimals, bodies more than a kilometer across, which are just large enough to be held together by gravity," said SwRI scientist Dr. David Nesvorny, the lead author of the paper "Trans-Neptunian Binaries as Evidence for Planetesimal Formation by the Streaming Instability" published in Nature Astronomy. 

During the initial stages of planet growth, dust grains gently collide and chemically stick to produce larger particles. However, as grains grow larger, collisions likely become more violent and destructive. Scientists have struggled to understand how planetary growth passes the 'meter-size barrier.' 

The streaming instability theory posits that as large dust grains interact with the gas that orbits young stars, streaming mechanisms cause grains to clump into dense regions and collapse under their own gravity to form planetesimals. 

The team studied objects beyond Neptune that orbit each other as binary pairs in the Kuiper Belt. Unlike comets flung by Jupiter or asteroids bombarded by collisions and radiation, the distant Kuiper Belt has not been disturbed much since it formed, so these primordial objects provide hints about the early solar system. If a pair orbits in the same direction as the planets orbit, it's considered heads-up. It's tails-up if it orbits in the opposite direction. 

An SwRI-led team performed 3D simulations of the streaming instability model of planet formation, where particle clumping triggers gravitational collapse into planetesimals. This snapshot from the simulation shows the vertically integrated density of solids, projected on the protoplanetary disk plane. Credit: HST/StSci/SwRI/Simon Porter.

Using the Hubble Space Telescope and the Keck Observatory in Hawaii, the team found that most binaries, about 80%, orbit heads-up, which astronomers call "prograde." This finding contradicted the theory that binaries form when two passing planetesimals are captured into a binary. That theory predicts mostly tails-up or "retrograde" orbits. 

To test whether the streaming instability could explain these Kuiper Belt binaries, the team analyzed simulations on large supercomputers. They found that the dense clumps formed by the streaming instability rotated heads-up 80% of the time, in agreement with the Kuiper Belt objects. 

"While our simulations can't yet follow the collapse all the way to forming binaries, it appears we are on the right track," said SwRI's Dr. Jacob B. Simon, who coauthored the paper. 

SwRI scientists used Hubble Space Telescope images of Kuiper belt binaries to determine that 80% orbit in the same direction as the planets. This research helps scientists improve planet formation models. Kuiper Belt object 2006 CH69 imaged on Jan. 26, 2017, is shown here. Credit: HST/StSci/SwRI/Simon Porter.

"The solar system offers many clues to how planets formed, both around our Sun and distant stars," Nesvorny said. "Although, these clues can be difficult to interpret, observers and theorists working together are starting to make heads or tails of these clues -- and the evidence is mostly heads." 

An SwRI-led team performed 3D simulations of the streaming instability model of planet formation, where particle clumping triggers gravitational collapse into planetesimals. This snapshot from the simulation shows the vertically integrated density of solids, projected on the protoplanetary disk plane. Credit: HST/StSci/SwRI/Simon Porter.

Source: Southwest Research Institute