A Crust Like Heavy Armor – New Research Sheds Light on Mars’ Structure

Mars is strikingly dichotomous: lowlands (blue) dominate the northern hemisphere, while there are high plains in the south. Credit: MOLA Science Team

During the final year of NASA’s Mars InSight mission, a large marsquake allowed researchers from ETH Zurich to determine the global thickness and density of the Mars’ crust. The Martian crust turned out to be significantly thicker compared to those of Earth or the Moon and the planet’s main source of heat is radioactive.

The Marsquake Service at ETH Zurich detected the strongest marsquake ever noted on a celestial body other than Earth in May 2022. This event, which had an approximated magnitude of 4.6, was documented on the Martian surface via the seismometer deployed as part of the NASA Mars InSight mission.

“This marsquake sent out strong seismic waves that traveled along the surface of Mars,” says Doyeon Kim, a seismologist at the Institute of Geophysics at ETH Zurich.

Surface waves offer a global perspective

After more than three years of daily monitoring and with the power levels decreasing on InSight’s seismometer, researchers were rewarded with data from a sizeable marsquake. The surface waves observed from this large marsquake not only traveled from the quake’s source to the measuring station, they also continued to travel around the entire planet several times. This data not only provided information about specific areas of Mars but also enabled a global view of the planet.

“From this quake, the largest quake recorded during the entire InSight mission, we observed surface waves that circled Mars up to three times,” says the seismologist and lead author of a study just published in the journal, Geophysical Research Letters.

In order to gain information about the structure that the waves passed through, the researchers measured how fast these waves propagate at different frequencies.

Topographic map of the Martian surface (l.) and representation of the crust thickness (r.). Credit: MOLA Science Team / Doyeon Kim, ETH Zurich

These seismic velocities provide insights into the interior structure at different depths. Previously, observed surface waves from the two large meteorite impacts also allowed regional findings along their specific propagation paths.

“Now, we have seismic observations that represent the global structure,” says Kim.

Comparing data from Mars with that of the Earth and Moon

Combining their newly obtained results with existing data on the gravity and topography of Mars, the researchers were able to determine the thickness of the Martian crust. It averages 42 to 56 kilometers (26 – 35 miles). On average, the crust is thinnest at the Isidis impact basin at ~10 km (6 miles), and thickest at Tharsis province at ~90 km (56 miles).

To put this into perspective, seismic data indicates that the Earth’s crust has an average thickness of 21 to 27 kilometers (13 – 17 miles), while the lunar crust, as determined by the Apollo mission seismometers is between 34 and 43 kilometres (21 – 27 miles) thick.

“This means that the Martian crust is much thicker than that of the Earth or the Moon,” says Kim. Generally, smaller planetary bodies in our solar system have a thicker crust than the larger bodies. Kim explains, “We were fortunate to observe this quake. On Earth, we would have difficulty determining the thickness of the Earth’s crust using the same magnitude of quake that occurred on Mars. While Mars is smaller than the Earth, it transports seismic energy more efficiently.”

One of the most important results of this research concerns the difference between the northern and southern hemispheres of Mars. This contrast has been observed for as long as there have been telescopes; it is particularly visible in images from Mars satellites. The northern hemisphere on Mars consists of flat lowlands, while there are high plateaus in the south. The division between northern lowlands and southern highlands is called a Martian dichotomy.

Similar crust density and radioactive heat

“One might think that this difference could be explained by two different rock compositions,” says Kim: “One rock would be denser than the other.” While the composition may be the same in the north and south, the thickness of the crust varies. If the crust is thicker in the south, there would be less dense Martian mantle material underneath it, whereas a thinner crust in the north would have more of this dense, heavier material.

Precisely what have the researchers been able to prove? “Based on the seismic observations and the gravity data, we show that the density of the crust in the northern lowlands and the southern highlands is similar,” they write. In contrast, the crust in the southern hemisphere extends to a greater depth than in the northern hemisphere. “This finding is very exciting and allows an end to a long-standing scientific discussion on the origin and structure of the Martian crust,” says Kim. After all, analysis of meteorite impacts on Mars last year already provided evidence that the crusts in the north and south are made of the same material.

Further conclusions can also be drawn from the thick Martian crust. “Our study provides how the planet generates its heat and explains Mars’ thermal history,” says Kim. As a single-plate planet, the main source of heat produced in the interior of Mars today is a result of the decay of radioactive elements such as thorium, uranium, and potassium. The study found that 50 to 70 percent of these heat-producing elements are found in the Martian crust. This high accumulation could explain why there are local regions underneath where melting processes may still be taking place today.

Reference: “Global crustal thickness revealed by surface waves orbiting Mars” by Doyeon Kim, Cecilia Duran, Domenico Giardini, Ana-Catalina Plesa, Simon C. Stähler, Christian Boehm, Vedran Lekic, Scott M. McLennan, Savas Ceylan, John Clinton, Paul McEwan Davis, Amir Khan, Brigitte Knapmeyer-Endrun, Mark Paul Panning, Mark A. Wieczorek and Philippe Lognonné, 22 June 2023, Geophysical Research Letters.
DOI: 10.1029/2023GL103482