Icy Impacts: Gauging The Thickness Of Ice On Europa
Sometimes planetary physics is like being in a snowball fight. Most people, if handed an already-formed snowball, can use their experience and the feel of the ball to guess what kind of snow it is comprised of: packable and fluffy, or wet and icy.
Using nearly the same principles, planetary scientists have been able to study the structure of Europa, Jupiter’s icy moon.
Europa is a rocky moon, home to saltwater oceans twice the volume of Earth’s, encased in a shell of ice. Scientists have long thought that Europa may be one of the best places in our solar system to look for nonterrestrial life. The likelihood and nature of that life, though, heavily depend on the thickness of its icy shell, something astronomers have not yet been able to ascertain.
A team of planetary science experts including Brandon Johnson, an associate professor, and Shigeru Wakita, a research scientist, in the Department of Earth, Atmospheric, and Planetary Sciences in Purdue University’s College of Science, announced in a new paper published in Science Advances [ES1] that Europa’s ice shell is at least 20 kilometers thick.
To reach their conclusion, the scientists studied large craters on Europa, running a variety of models to determine what combination of physical characteristics could have created such a surface structure.
“This is the first work that has been done on this large crater on Europa,” Wakita said. “Previous estimates showed a very thin ice layer over a thick ocean. But our research showed that there needs to be a thick layer — so thick that convection in the ice, which has previously been debated, is likely.”
Using data and images from the spacecraft Galileo, which studied Europa in 1998, Johnson analyzed the impact craters to decode truths about Europa’s structure. An expert in planetary physics and colossal collisions, Johnson has studied almost every major planetary body in the solar system. Scientists have long debated the thickness of Europa’s ice shell; no one has visited to measure it directly, so scientists are creatively using the evidence at hand: the craters on Europa’s icy surface (video of impact simulation).
“Impact cratering is the most ubiquitous surface process shaping planetary bodies,” Johnson said. “Craters are found on almost every solid body we’ve ever seen. They are a major driver of change in planetary bodies. When an impact crater forms, it is essentially probing the subsurface structure of a planetary body. By understanding the sizes and shapes of craters on Europa and reproducing their formation with numerical simulations, we’re able to infer information about how thick its ice shell is.”
Europa is a frozen world, but the ice shelters a rocky core. The icy surface, though, is not stagnant. Plate tectonics and convection currents in the oceans and the ice itself refresh the surface fairly frequently. This means the surface itself is only 50 million to 100 million years old — which sounds old to short-lived organisms like humans, but is young as far as geological periods go.
That smooth, young surface means that craters are clearly defined, easier to analyze and not very deep. Their impacts tell scientists more about the icy shell of the moon and the water ocean below, rather than conveying much information about its rocky heart.
“Understanding the thickness of the ice is vital to theorizing about possible life on Europa,” Johnson said. “How thick the ice shell is controls what kind of processes are happening within it, and that is really important for understanding the exchange of material between the surface and the ocean. That is what will help us understand how all kinds of processes happen on Europa — and help us understand the possibility of life.”
Time series of our fiducial model of the formation of an icy multiring basin. Simulation is of a 1.5-km-radius impactor striking a 20-km-thick ice shell with a 6-km-thick conductive lid. Material is colored according to total plastic strain. White dashed curves indicate the material boundaries (i.e., ice shell and ocean). The insets are a magnified view of the upper 6 km of the conductive ice lid and outer portions of the basin where graben would form. Figure S1 shows the total plastic strain in log scale, and fig. S4 outlines the location of graben at 600 s. Movie S1 is an animation of this figure. (A) shows the formation of the transient crater, (B) shows the formation of the central uplift, (C) shows the formation of faults, and (D) represents the enhancement of faults during a secondary phase of collapse (see the main text for details).
Multiring basin formation constrains Europa’s ice shell thickness, Science Advances (open access)
Astrobiology
