PROVIDENCE, R.I. [Brown University] — The scorching hot surface of Mercury seems like an unlikely place to find ice, but research over the past three decades has suggested that water is frozen on the first rock from the sun, hidden away on crater floors that are permanently shadowed from the sun’s blistering rays.  Now, a new study led by Brown University researchers suggests that there could be much more ice on Mercury’s surface than previously thought.

The study, published in Geophysical Research Letters, adds three new members to the list of craters near Mercury’s north pole that appear to harbor large surface ice deposits. But in addition to those large deposits, the research also shows evidence that smaller-scale deposits scattered around Mercury’s north pole, both inside craters and in shadowed terrain between craters. Those deposits may be small, but they could add up to a lot more previously unaccounted-for ice.

“The assumption has been that surface ice on Mercury exists predominantly in large craters, but we show evidence for these smaller-scale deposits as well,” said Ariel Deutsch, the study’s lead author and a Ph.D. candidate at Brown. “Adding these small-scale deposits to the large deposits within craters adds significantly to the surface ice inventory on Mercury.”

The idea that Mercury might have frozen water emerged in the 1990s, when Earth-based radar telescopes detected highly reflective regions inside several craters near Mercury’s poles. The planet’s axis doesn’t have much tilt, so its poles get little direct sunlight, and the floors of some craters get no direct sunlight at all. Without an atmosphere to hold in any heat from surrounding surfaces, temperatures in those eternal shadows have been calculated to be low enough for water ice to be stable. That raised the possibility these “radar-bright” regions could be ice.

That idea got a boost after NASA’s MESSENGER probe entered Mercury’s orbit in 2011. The spacecraft detected neutron signals from the planet’s north pole that were consistent with water ice.  

For this new study, Deutsch worked with Gregory Neumann from NASA’s Goddard Space Flight Center to take a deep dive into the data returned from MESSENGER. They looked specifically at readings from the spacecraft’s laser altimeter. The device is mostly used to map elevation, but it can also be used to track surface reflectance.

Neumann, an instrument specialist for the MESSENGER mission, helped to calibrate the altimeter’s reflectance signal, which can vary depending upon whether the measurement is taken from directly overhead or at an oblique angle (known as “off-nadir”).  That calibration enabled the researchers to detect high reflectance deposits consistent with surface ice in three large craters for which only off-nadir detections were available.

The addition of those craters to Mercury’s ice inventory is significant. Deutsch estimates the total area of the three sheets to be about 3,400 square kilometers—slightly larger than the state of Rhode Island.

But another major aspect of the work is that the researchers also looked at reflectance data for the terrain surrounding those three large craters. That terrain isn’t as bright as the ice sheets inside the craters, but it’s significantly brighter than the average Mercury surface.

“We suggest that this enhanced reflectance signature is driven by small-scale patches of ice that are spread throughout this terrain,” Deutsch said. “Most of these patches are too small to resolve individually with the altimeter instrument, but collectively they contribute to the overall enhanced reflectance.”

To seek further evidence that such smaller-scale deposits exist, the researchers looked though the altimeter data in search of patches that were smaller than the big crater-based deposits, but still large enough to resolve with the altimeter. They found four, each with diameters of less than about 5 kilometers.

“These four were just the ones we could resolve with the MESSENGER instruments,” Deutsch said. “We think there are probably many, many more of these, ranging in sizes from a kilometer down to a few centimeters.”

Knowing that these small-scale deposits exist, and that they’re likely the source of the slightly brighter surface outside craters, could dramatically increase the ice inventory on Mercury.  Similar small-scale ice deposits are thought to exist on the poles of the Moon. Research models have suggested that accounting for these small-scale deposits roughly doubles the amount of lunar real estate that could harbor ice. The same could be true on Mercury, the researchers say.

How this polar ice may have found its way to Mercury in the first place remains an open question, Deutsch says. The leading hypothesis is that it was delivered by water-rich comet or asteroid impacts. Another idea is that hydrogen may have been implanted in the surface by solar wind, later combining with an oxygen source to form water.

Jim Head, Deutsch’s Ph.D. advisor and co-author of the research, said the work adds a new perspective on a critical question in planetary science.

“One of the major things we want to understand is how water and other volatiles are distributed through the inner solar system—including Earth, the Moon and our planetary neighbors,” Head said. “This study opens our eyes to new places to look for evidence of water, and suggests there’s a whole lot more of it on Mercury than we thought.”

The study was supported by NASA through the Harriet G. Jenkins Graduate Fellowship (NNX16AT19H) and the Solar System Exploration Research Virtual Institute. 

Quelle: Brown University