Water Ice In Eternal Polar Night on Ceres
The American Dawn space probe has been orbiting the asteroid Ceres between Mars and Jupiter since March 2015. Thanks to the two identical onboard cameras from the Max Planck Institute for Solar System Research (MPS), the Framing Cameras, the dwarf planet has been almost completely mapped. In a current study, a team headed by scientists from the MPS reports on Ceres’ most northerly regions, where the Göttingen cameras have performed a very special feat: they have succeeded in taking photos of water ice deposits in places ruled by almost eternal darkness.
View of the North Pole: The colours show the varying height of Ceres’ landscape. The numbers refer to ten craters where the Framing Cameras built in Göttingen at the Max Planck Institute for Solar System Research have discovered water ice.
Thomas Platz is the lead author of the study now published in Nature Astronomy, a new specialist journal. “Using our cameras, we looked at the craters in the region near the north pole between 65 and 90 degrees north. Some of these craters are at least partially in eternal darkness which means they are never reached by sunlight. The reason for this is that Ceres’ rotational axis has an angle of inclination of only 4.028 degrees,” explains the member of the Framing Camera team at the MPS.
NASA’s Dawn spacecraft determined the hydrogen content of the upper yard, or meter, of Ceres’ surface. Blue indicates where hydrogen content is higher, near the poles, while red indicates lower content at lower latitudes.
The computer simulation shows a conceivable scenario: An impact such as the one that created the Oxo crater, which measures approx. 10 kilometres across (42 degrees north), would have been able to hurl icy rock as far as the north pole, where it could have survived in the cold traps of the permanently dark crater.
Crater No. 1, whose interior has a large region in permanent darkness (a). In the weak scattered light, the framing cameras can make out bright deposits of ice (b). Crater No. 2 with its dark region is shown in Figures (c) to (e). The ice shown in (d) extends into the region with direct illumination (e).
Scientists have long thought that Ceres’ interior contains large amounts of ice because its density is so low – 2.1621 grammes per cubic centimetre. This is now the second time that water has been found directly on the surface. The current results join measurements from the Herschel telescope operated by the European Space Agency ESA, which measured water vapour close to Ceres in 2014. In December 2015, moreover, Max Planck researchers in Göttingen used the Framing Cameras to record patches of mist over two craters close to the equator, likewise an indication of water in vapour form.
Deposits of ice on parts of Ceres’ surface which experience direct sunlight are found to be unstable over long, geological periods of time. The dwarf plant has no atmosphere and thus the ice sublimates in a relatively short period of time once it reaches the surface. This means it passes directly from ice to the gaseous state. At places which are permanently in darkness, and thus extremely cold, where the temperatures fall below minus 163 degrees Celsius, ice can survive for a very long time.
“We know ice deposits exist in the polar regions of our Moon and the planet Mercury, both of which have no atmosphere either. These ice deposits can be explained as the result of external events such as the impacts of comets,” says Nathues. “The craters near Ceres’ poles, however, contain ice which is probably indigenous to Ceres, i.e. it originates mainly from Ceres itself,” explains Platz. As the co-authors of the study of the Free University of Berlin have been able to show in a simulation, the impact which originally created the Oxo crater, for example, could have blasted away icy rock which exists below the surface and hurled it as far as the polar regions.
Ice is everywhere on Ceres
Ceres’ uppermost surface is rich in hydrogen, with higher concentrations at mid-to-high latitudes — consistent with broad expanses of water ice, according to a new study in the journal Science.
“On Ceres, ice is not just localized to a few craters. It’s everywhere, and nearer to the surface with higher latitudes,” said Thomas Prettyman, principal investigator of Dawn’s gamma ray and neutron detector (GRaND), based at the Planetary Science Institute, Tucson, Arizona.
This movie of images from NASA’s Dawn spacecraft shows a crater on Ceres that is partly in shadow all the time. Such craters are called “cold traps.” Dawn has shown that water ice could potentially be preserved in such place for very long amounts of time.
Credits: NASA/JPL-Caltech/UCLA/MPS/DLR/IDA
Researchers used the GRaND instrument to determine the concentrations of hydrogen, iron and potassium in the uppermost yard (or meter) of Ceres. GRaND measures the number and energy of gamma rays and neutrons emanating from Ceres. Neutrons are produced as galactic cosmic rays interact with Ceres’ surface. Some neutrons get absorbed into the surface, while others escape. Since hydrogen slows down neutrons, it is associated with fewer neutrons escaping. On Ceres, hydrogen is likely to be in the form of frozen water (which is made of two hydrogen atoms and one oxygen atom).
Rather than a solid ice layer, there is likely to be a porous mixture of rocky materials in which ice fills the pores, researchers found. The GRaND data show that the mixture is about 10 percent ice by weight.
“These results confirm predictions made nearly three decades ago that ice can survive for billions of years just beneath the surface of Ceres,” Prettyman said. “The evidence strengthens the case for the presence of near-surface water ice on other main belt asteroids.”
Clues to Ceres’ inner life
Concentrations of iron, hydrogen, potassium and carbon provide further evidence that the top layer of material covering Ceres was altered by liquid water in Ceres’ interior. Scientists theorize that the decay of radioactive elements within Ceres produced heat that drove this alteration process, separating Ceres into a rocky interior and icy outer shell. Separation of ice and rock would lead to differences in the chemical composition of Ceres’ surface and interior.
Because meteorites called carbonaceous chondrites were also altered by water, scientists are interested in comparing them to Ceres. These meteorites probably come from bodies that were smaller than Ceres, but had limited fluid flow, so they may provide clues to Ceres’ interior history. The Science study shows that Ceres has more hydrogen and less iron than these meteorites, perhaps because denser particles sunk while brine-rich materials rose to the surface. Alternatively, Ceres or its components may have formed in a different region of the solar system than the meteorites.
Ice in permanent shadow
A second study, led by Thomas Platz of the Max Planck Institute for Solar System Research, Gottingen, Germany, and published in the journal Nature Astronomy, focused on craters that are persistently in shadow in Ceres’ northern hemisphere. Scientists closely examined hundreds of cold, dark craters called “cold traps” — at less than minus 260 degrees Fahrenheit (110 Kelvin), they are so chilly that very little of the ice turns into vapor in the course of a billion years. Researchers found deposits of bright material in 10 of these craters. In one crater that is partially sunlit, Dawn’s infrared mapping spectrometer confirmed the presence of ice.
This suggests that water ice can be stored in cold, dark craters on Ceres. Ice in cold traps has previously been spotted on Mercury and, in a few cases, on the moon. All of these bodies have small tilts with respect to their axes of rotation, so their poles are extremely cold and peppered with persistently shadowed craters. Scientists believe impacting bodies may have delivered ice to Mercury and the moon. The origins of Ceres’ ice in cold traps are more mysterious, however.
“We are interested in how this ice got there and how it managed to last so long,” said co-author Norbert Schorghofer of the University of Hawaii. “It could have come from Ceres’ ice-rich crust, or it could have been delivered from space.”
Regardless of its origin, water molecules on Ceres have the ability to hop around from warmer regions to the poles. A tenuous water atmosphere has been suggested by previous research, including the Herschel Space Observatory’s observations of water vapor at Ceres in 2012-13. Water molecules that leave the surface would fall back onto Ceres, and could land in cold traps. With every hop there is a chance the molecule is lost to space, but a fraction of them ends up in the cold traps, where they accumulate.
‘Bright spots’ get names
This video shows a flyover of the intriguing crater named Occator on dwarf planet Ceres. Occator is home to Ceres’ brightest area.
Credits: NASA/JPL-Caltech/UCLA/MPS/DLR/IDA
Ceres’ brightest area, in the northern-hemisphere crater Occator, does not shine because of ice, but rather because of highly reflective salts. A new video produced by the German Aerospace Center (DLR) in Berlin simulates the experience of flying around this crater and exploring its topography. Occator’s central bright region, which includes a dome with fractures, has recently been named Cerealia Facula. The crater’s cluster of less reflective spots to the east of center is called Vinalia Faculae.
“The unique interior of Occator may have formed in a combination of processes that we are currently investigating,” said Ralf Jaumann, planetary scientist and Dawn co-investigator at DLR. “The impact that created the crater could have triggered the upwelling of liquid from inside Ceres, which left behind the salts.”
Dawn’s next steps
Dawn began its extended mission phase in July, and is currently flying in an elliptical orbit more than 4,500 miles (7,200 kilometers) from Ceres. During the primary mission, Dawn orbited and accomplished all of its original objectives at Ceres and protoplanet Vesta, which the spacecraft visited from July 2011 to September 2012.
Dr Birgit Krummheuer
Max Planck Institute for Solar System Research, Göttingen
Elizabeth Landau
Jet Propulsion Laboratory,
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