Active pits on Rosetta’s comet
July 03, 2015
Researchers under the lead of Jean-Baptiste Vincent from the MPS have studied 18 peculiar pit-like depressions all occuring in the northern hemisphere of Rosetta’s comet 67P/Churyumov-Gerasimenko. The scientists analysed images of the comet obtained by OSIRIS, the scientific imaging system on board ESA’s Rosetta spacecraft, in the period from July to December 2014. The pits' diameters vary between ten and a few hundreds of meters. They exhibit nearly vertical sidewalls and are exceptionally deep with the largest ones extending up to two hundred meters into the comet’s interior. The walls of these depressions are characterized by layers and terraces, their bottoms are mostly flat.
Earlier, similar structures had been discovered on the comets 9P/Tempel 1 and 81P/Wild 2, that have been visited by NASA’s space probes Deep Impact and Stardust in the past. “Because of their unusual morphology, these pits can be clearly distinguished from impact craters”, says OSIRIS-scientist Jean-Baptiste Vincent. “They seem to be a typical characteristic of comets”, he adds.
Some of the pits are also active: fine jets of dust are emitted from the inside walls. The scientists reached this conclusion by studying images showing the same jet from different perspectives. “In this way we obtain information on the jet’s three dimensional structure and can determine their origin on the surface”, says Vincent.
However, the emission of dust alone cannot have created these structures. Frozen gases evaporating from the comet’s surface under the influence of the Sun cannot carry enough dust with them to create holes of this size. In some cases, thousands of years of evaporation would be necessary. However, Rosetta’s comet has been advancing into the inner solar system and therewith into the Sun’s vicinity only since 1959. And even a sudden outburst of activity like the one Rosetta witnessed during the approach phase in April 2014 is unable to move enough material.
Instead, it is most likely that the pits are collapsed cavities. “Apparently, these underground voids grow larger with time until the top layer becomes instable and caves in," says Holger Sierks from the MPS, co-author of the new paper and OSIRIS Principal Investigator. As a result, fresh material is exposed at the edges of the depression. From there gases can vaporise thus charging the observed jets.
But how did the cavities come to be? The researchers currently see several possibilities. For example, the voids could date from the comet’s birth. When smaller chunks, called planetesimals, collide at low speeds such gaps may remain.
It is also conceivable, that frozen carbon dioxide and monoxide evaporating from deep within the cometary nucleus produce such subsurface structures. Frozen water evaporates at much higher temperatures. It is difficult to achieve these temperatures beneath the comet's highly insulating, superficial layer of dust by solar radiation alone. Instead, the researchers have a different heat source in view. When amorphous ice beneath the comet's surface consisting of irregularly packed molecules transforms into crystallized ice, heat is released. This might suffice to evaporate water in sufficient quantities.
"At this point, we do not favour any of these three options. Maybe even all effects work together”, says Sierks. "But we hope that the mission will brings clarity in its further course."
Already, the active pits prove useful for estimating the age of cometary surfaces. "Since the pits are active, they change with time," says Vincent. By and by the pits expand: the edges retreat forming extensive terraces. A cometary surface exhibiting deep holes is therefore rather young. Older areas present themselves as smooth plateaus.
BK / HOR