Using the Atacama Large Millimeter/submillimeter Array (ALMA), astronomers observed a dust trap in a system called Oph-IRS 48 where dust grains were trapped and could grow much larger by colliding and sticking together.
Astronomers have imaged a region around a young star where dust particles can grow by clumping together. This is the first time that such a dust trap has been clearly observed and modeled. It solves a long-standing mystery about how dust particles in discs grow to larger sizes so that they can eventually form comets, planets, and other rocky bodies. The results are published in the journal Science on June 7, 2013.
Astronomers now know that planets around other stars are plentiful. But they do not fully understand how they form and there are many aspects of the formation of comets, planets, and other rocky bodies that remain a mystery. However, new observations exploiting the power of ALMA are now answering one of the biggest questions: how do tiny grains of dust in the disc around a young star grow bigger and bigger — to eventually become rubble, and even boulders well beyond a meter in size?
Computer models suggest that dust grains grow when they collide and stick together. However, when these bigger grains collide again at high speed they are often smashed to pieces and sent back to square one. Even when this does not happen, the models show that the larger grains would quickly move inwards because of friction between the dust and gas and fall onto their parent star, leaving no chance that they could grow even further.
This artist’s rendering shows the behavior of different-sized particles in the disc of dust that surrounds Oph-IRS 48 system. The bigger particles, millimeters in diameter, tend to clump together in a safe haven that allows them to grow even further, eventually forming boulders and then comets.
Somehow the dust needs a safe haven where the particles can continue growing until they are big enough to survive on their own . Such “dust traps” have been proposed, but there was no observational proof of their existence up to now.
Nienke van der Marel, a PhD student at Leiden Observatory in the Netherlands, and lead author of the article, was using ALMA along with her co-workers, to study the disc in a system called Oph-IRS 48 . They found that the star was circled by a ring of gas with a central hole that was probably created by an unseen planet or companion star. Earlier observations using ESO’s Very Large Telescope had already shown that the small dust particles also formed a similar ring structure. But the new ALMA view of where the larger millimeter-sized dust particles were found was very different!
“At first the shape of the dust in the image came as a complete surprise to us,” says van der Marel. “Instead of the ring we had expected to see, we found a very clear cashew-nut shape! We had to convince ourselves that this feature was real, but the strong signal and sharpness of the ALMA observations left no doubt about the structure. Then we realized what we had found.”
What had been discovered was a region where bigger dust grains were trapped and could grow much larger by colliding and sticking together. This was a dust trap — just what the theorists were looking for.
As van der Marel explains: “It’s likely that we are looking at a kind of comet factory as the conditions are right for the particles to grow from millimeter to comet size. The dust is not likely to form full-sized planets at this distance from the star. But in the near future ALMA will be able to observe dust traps closer to their parent stars, where the same mechanisms are at work. Such dust traps really would be the cradles for new-born planets.”
The dust trap forms as bigger dust particles move in the direction of regions of higher pressure. Computer modeling has shown that such a high pressure region can originate from the motions of the gas at the edge of a gas hole — just like the one found in this disc.
This computer simulation shows how a vortex can form when a massive planet is interacting with a disc around a young star. It shows how the gas density evolves when there is a planet, with a mass ten times that of Jupiter, located at 20 times the Earth-Sun distance from the central star. A large-scale vortex is created at the outer edge of the gap, which can live for more than 1000 of the planet’s orbits. This vortex can trap millimeter-sized particles over million years timescales and explain the high contrast structure observed with ALMA in the disc around Oph-IRS 48.
“The combination of modeling work and high quality observations of ALMA makes this a unique project”, says Cornelis Dullemond from the Institute for Theoretical Astrophysics in Heidelberg, Germany, who is an expert on dust evolution and disc modeling, and a member of the team. “Around the time that these observations were obtained, we were working on models predicting exactly these kinds of structures: a very lucky coincidence.”
The observations were made while the ALMA array was still being constructed. They made use of the ALMA Band 9 receivers  — European-made devices that allow ALMA to create its so far sharpest images.
“These observations show that ALMA is capable of delivering transformational science, even with less than half of the full array in use,” says Ewine van Dishoeck of the Leiden Observatory, who has been a major contributor to the ALMA project for more than 20 years. “The incredible jump in both sensitivity and image sharpness in Band 9 gives us the opportunity to study basic aspects of planet formation in ways that were simply not possible before.”
The detection of this “dust trap” solves a long-standing mystery: how dust particles around stars sum up to form planets, comets, and other rocky bodies. ESOcast 58 goes deep into the dust trap to explore how this comet factory works.
 The cause of the dust trap, in this case a vortex in the disc’s gas’, has a typical life span of hundreds of thousands of years. Even when the dust trap ceases to work, the dust accumulated in the trap would take millions of years to disperse providing ample time for the dust grains to grow larger.
 The name is a combination of the constellation name of the star-forming region where the system is found and the type of source, so Oph stands for the constellation of Ophiuchus (The Serpent Bearer), and the IRS stands for infrared source. The distance from Earth to Oph-IRS 48 is about 400 light-years.
 ALMA can observe in different frequency bands. Band 9, operating at wavelengths of about 0.4–0.5 millimeters, is the mode that so far provides the sharpest images.
Reference: “A Major Asymmetric Dust Trap in a Transition Disk” by Nienke van der Marel, Ewine F. van Dishoeck, Simon Bruderer, Til Birnstiel, Paola Pinilla, Cornelis P. Dullemond, Tim A. van Kempen, Markus Schmalzl, Joanna M. Brown, Gregory J. Herczeg, Geoffrey S. Mathews and Vincent Geers, 7 June 2013, Science.