From EGI.eu case studies: How grid computing helps astronomers to explain the origins of main-belt comets?

Comets such as the Halley or the Hale-Bopp are small objects travelling through the solar system in long elliptical orbits. Their characteristic tail appears every time they get close to the Sun, when heat and solar winds combine to melt their frozen core surface.

The asteroids circling the Sun on the Main Belt between Mars and Jupiter do not have tails. Their regular orbit keeps them closer to the Sun at all times, which means that any ice they might have had on the surface evaporated a long time ago.

So says conventional wisdom.

But astronomers have recently discovered at least seven examples of asteroids with a comet-like tail within the main belt. How does that work? Where does the tail come from?

These strange objects are called main-belt comets and they are thought to be the remnants of a larger body smashed to pieces by a recent impact. One way to prove the theory is to look for examples of an asteroid family that shares their origin with a main-belt comet.

The telling tail of the P/2006 VW₁₃₉ main-belt comet was discovered by the Pan-STARRS1 telescope. This picture is a long-exposure image taken by the New Technology Telescope at La Silla Observatory in Chile. (Credit: Sam Duddy and Stephen Lowry, University of Kent).

Building an asteroid family tree

Serbian astronomer Bojan Novakovic, from theUniversity of Belgrade, is working on this problem with colleagues Henry Hsieh and Alberto Cellino. The team focused on the P/2006 VW₁₃₉ main-belt comet and their goal was to see if it could be assigned to a family of asteroids.

First described as an asteroid, it was reclassified as a main-belt comet in 2011 when astronomers working on the Pan-STARRS1 survey telescope in Hawaii discovered its tail.

P/2006 VW₁₃₉ is special as one of the only seven known examples of main-belt comets, but finding other members of its family among hundreds of thousands of possible candidates is not an easy task.

Bojan started his search at the AstDys database, a catalogue of 398,841 asteroids, using the hierarchical clustering method and the cut-off distance parameter to sort through the candidates. This narrowed down the possibilities to 24 asteroids.

The next step was to refine the group by looking at the detailed orbital characteristics of these 24 asteroids. For this task, Bojan used a method called backward integration, "which can be used to distinguish real family members from interlopers," he explains.

To investigate the orbital characteristics of potential family members Bojan needed to go through a large number of calculations, which were "computationally expensive and would take months to be done on a typical PC," he adds.

The solution to this problem was to use grid computing. "In particular for this work we used infrastructure of Academic and Educational Grid Initiative of Serbia," Bojan says.

After looking at the complete orbital histories of 24 objects with the help of grid computing, Bojan was able to reduce the P/2006 VW₁₃₉ family to just 11 members.

P/2006 VW₁₃₉ and its young family of 11

The most important conclusion of Bojan's research, published in the Monthly Notices of the Royal Astronomical Society, is that P/2006 VW₁₃₉ and its 11 partners are part of a real asteroid family formed about 7.5 million years ago. "[Asteroid] families are consider to be young if they are less than about 10 million years old," he explains.

This suggests that 7.5 million years ago, a large asteroid crashed with another object and disintegrated into 11 smaller pieces: P/2006 VW₁₃₉ and its 10 family members. P/2006 VW₁₃₉ is special because it inherited the deeply buried ice of the parent asteroid. It's this ice that vaporises producing the characteristic tail of a comet.

"The fact that ice still exists close to the surface of P/2006 VW₁₃₉ means that its surface is relatively young," says Bojan. This means P/2006 VW₁₃₉ and its siblings were formed long after the asteroid belt supporting the theory that main-belt comets are born in collision events within the asteroid belt and not through some other means.