Several sites of cliff collapse on Comet 67P/Churyumov-Gerasimenko were identified during Rosetta’s mission. This image focuses on an example in the Ash region, close to the boundary with Imhotep on the comet’s large lobe. The yellow arrows mark the fractures where the detachment occurred. The images were taken by Rosetta’s OSIRIS camera on Dec. 2, 2014 (left) and March 12, 2016 (right). Credit: ESA/Rosetta/MPS for OSIRIS Team MPS/UPD/LAM/IAA/SSO/INTA/UPM/DASP/IDA A study published March 21, 2017 in the journal Science summarizes the types of surface changes observed during the two years that the European Space Agency’s Rosetta spacecraft spent investigating comet 67P/Churyumov-Gerasimenko. Notable differences are seen before and after the comet’s most active period—perihelion—when it reached its closest point to the Sun along its orbit. ”Monitoring the comet continuously as it traversed the inner solar system gave us an unprecedented insight not only into how comets change when they travel close to the Sun, but also how fast these changes take place,” said Mohamed El-Maarry, a comet researcher at the University of Colorado, Boulder and the lead author of the study.
The changes are linked to different geological processes: weathering and erosion, sublimation of water ice, and mechanical stresses arising from the comet’s spin.
”Comet landscapes are fascinating. They are sculpted by slow erosion and dramatic outbursts,” said Dennis Bodewits, an assistant research scientist in astronomy at the University of Maryland who is a co-author of the study. ”One of the key points of this paper is that the observed changes are small and relatively subtle. Features such as large holes suggest that more violent activity is infrequent on the time scale of an orbital period.”
Weathering occurs all over the comet, where consolidated materials are weakened—such as by heating and cooling cycles on daily or seasonal timescales—causing their fragmentation. Combined with heating of subsurface ices that lead to outflows of gas, this can ultimately result in the sudden collapse of cliff walls, the evidence of which is apparent in several locations on the comet. A 30-meter-wide, 12,800-ton boulder was found to have moved 140 meters in the Khonsu region of Comet 67P/Churyumov-Gerasimenko in the lead up to perihelion in August 2015, when the comet’s activity was at its highest. In both images, an arrow points to the boulder; in the right-hand image, the dotted circle outlines the original location of the boulder for reference. The images were taken by Rosetta’s OSIRIS camera on May 2, 2015 (left) and Feb. 7, 2016 (right). Credit: ESA/Rosetta/MPS for OSIRIS Team MPS/UPD/LAM/IAA/SSO/INTA/UPM/DASP/IDA A completely different process is thought to be responsible for a 500-meter-long fracture spotted in August 2014 that runs through the comet’s neck in the Anuket region. This fracture was found to have extended by about 30 meters by December 2014. This is linked to the comet’s increasing spin rate in the lead up to perihelion. Furthermore, in images taken in June 2016, a new 150 to 300-meter-long fracture was identified parallel to the original fracture.
Close to the fractures, a four-meter-wide boulder moved by about 15 meters, as determined by comparing images taken in March 2015 and June 2016. It is not clear whether the fracture extension and movement of the boulder are related to each other or caused by different processes.
A substantially larger boulder, some 30 meters wide and weighing 12,800 tons, was found to have moved an impressive 140 meters in the Khonsu region, on the larger of the two comet lobes.
It is thought that the boulder moved during the perihelion period, as several outburst events were detected close to its original position. The movement could have been triggered in one of two ways: either a large amount of underlying material eroded away, allowing the boulder to roll downslope, or a forceful outburst could have directly lifted the boulder to the new location.
Erosion caused by the sublimation of material, and deposition of dust falling from outbursts, are also thought to be responsible for sculpting the landscape in different ways. For example, scarps in several smooth plains have been observed to retreat by tens of meters and at a rate of up to a few meters per day around perihelion. Dune-like features that were identified early in Rosetta’s mission in the neck region of Comet 67P/Churyumov–Gerasimenko were seen to evolve over the two years of study (first and last images). In addition, numerous circular scarp-like features were seen to develop and fade over time (central set of images). The circular features reached a diameter of 100 m in less than three months before subsequently fading away again, giving rise to a new set of ripples. The repeated development of these unique features at the same spot is thought to be linked to the curved structure of the neck region directing the flow of sublimating gas in a particular way. The arrows point to the approximately location of the ripple and scarp features to help guide the eye between images when the viewing orientation and resolution changes. The images were taken by Rosetta’s OSIRIS camera on 5 September 2014 (left), 25 April 2015 (centre top left), 10 May 2015 (centre top right), 11 July 2015 (centre bottom left), 20 December 2015 (centre bottom right), and 7 June 2016 (right). The image resolutions are 0.8, 1.6, 2.4, 2.9, 1.7 and 0.5 m/pixel, respectively. Credit: ESA/Rosetta/MPS for OSIRIS Team MPS/UPD/LAM/IAA/SSO/INTA/UPM/DASP/IDA ”Scarp retreats were observed before on Comet Tempel 1, inferred by comparing images taken during flybys of the comet by NASA’s Deep Impact in 2005, and Stardust-NExT in 2011,” said El-Maarry. ”What we were able to do with Rosetta was to monitor similar changes continuously, and at a higher resolution. Our observations additionally tell us that scarp retreat seems to be a common process on comets, specifically in smooth-looking deposits.”
Furthermore, in the smooth plains of the Imhotep region, previously hidden circular features and small boulders have been exposed by the removal of material. In one location, a depth of about three meters had been removed, most likely through the sublimation of underlying ices.
Changes were also noted in the comet’s smooth neck region, near distinctive ripples that were likened to Earth’s sand dunes when they were first identified. Close monitoring of the ripple formations showed this location to also display expanding circular features in the soft material that reached diameters of 100 meters in less than three months. They subsequently faded away to give rise to new sets of ripples.
The researchers speculate that the repeated development of these unique features at the same spot must be linked to the curved structure of the neck region directing the flow of sublimating gas in a particular way.
Another type of change is the development of honeycomb-like features noticed in the dusty terrains of the Ma’at region on the comet’s small lobe in the northern hemisphere, marked by an increase in surface roughness in the six months leading up to perihelion. Showcase of the different types of changes identified in high-resolution images of Comet 67P/Churyumov–Gerasimenko during more than two years of monitoring by ESA’s Rosetta spacecraft. The approximate locations of each feature are marked on the central context images. Dates of when the ‘before’ and ‘after’ images were taken are also indicated. Note that the orientation and resolution between image pairs may vary, therefore in each image set arrows point to the location of the changes, for guidance. Credit: Top centre images: ESA/Rosetta/NAVCAM, CC BY-SA 3.0 IGO; all others: ESA/Rosetta/MPS for OSIRIS Team MPS/UPD/LAM/IAA/SSO/INTA/UPM/DASP/IDA Similar to other seasonal changes, these features faded substantially after perihelion, presumably as a result of resurfacing by the deposition of new particles ejected from the southern hemisphere during this active period.
”This documentation of changes over time was a key goal of Rosetta’s mission, and shows the surface of comets as geologically active, on both seasonal and short transient timescales,” said Matt Taylor, Rosetta project scientist for the European Space Agency.
The scientists also note that although many small-scale localized changes have occurred, there were no major shape-changing events that significantly altered the comet’s overall appearance. Ground-based observations over the last few decades suggest similar levels of activity during each perihelion, so the researchers think that the major landforms seen during Rosetta’s mission were sculpted during a different orbital configuration.
”At UMD, we use telescopes such as Swift and Spitzer to look at the activity of comets as they approach the Sun for the first time,” said Michael A’Hearn, a Distinguished University Professor Emeritus of astronomy at UMD and a co-author on the study. A’Hearn also served as principal investigator on the Deep Impact mission. ”We know that such comets are indeed very active. But Rosetta allowed us to see in great detail what this activity did to the surface of comet 67P/Churyumov-Gerasimenko.”
The research paper, ”Surface changes on comet 67P/Churyumov-Gerasimenko suggest a more active past,” Mohamed El-Maarry et al., was published March 21, 2017 in the journal Science.
A complementary paper, ”The pristine interior of comet 67P revealed by the combined Aswan outburst and cliff collapse,” by M. Pajola et al, is also published today in Nature Astronomy. Read our news story here.
Explore further:Rosetta comet orbiter films deep-space landslide
More information: ”Surface changes on comet 67P/Churyumov-Gerasimenko suggest a more active past,”, Science, DOI: 10.1126/science.aak9384
Journal reference:ScienceNature Astronomy
Provided by:University of Maryland