Researchers establish new timeline for ancient magnetic field on Mars

Mars had a global magnetic field much earlier and much later in the planet's history than scientists have previously known.

A planet’s global magnetic field arises from what scientists call a dynamo: a flow of molten metal within the planet’s core that produces an electrical current. On Earth, the dynamo is what makes compass needles point north. But Mars’ dynamo has been extinct for billions of years.

New findings from canadian researchers working with colleagues in the U.S. and France, published today in Science Advances, bring us closer to knowing the precise timing and duration of Mars’ dynamo.

"We find that the Martian dynamo operated at 4.5 billion and 3.7 billion years ago. Dynamo timing is a big part of a planet’s evolution, and what we find is very different from what we have thought so far," said Anna Mittelholz, postdoctoral fellow in UBC's department of earth, ocean and atmospheric sciences, and first author of the study. “The dynamo tells us something about the planet's thermal history, its evolution, and how it got to where it is today, and it is unique for each of the terrestrial planets Earth, Mars, Venus and Mercury”.

Clues about a planet's magnetic history lie in magnetized rocks on and beneath its surface. Rock is like a tape recorder, especially volcanic rocks. They begin as lava, but as they cool and solidify in the presence of a magnetic field, minerals within the rocks align themselves with the global magnetic field. By dating these rocks, scientists can estimate if a dynamo was active at the time the rock was emplaced.

fig CP Timing of martian dynamo LANGLAIS2020 500px

Lucus Planum observations. (A to C) Magnetic field over AP and LP below 200 km altitude. (A) |B| from MAVEN nighttime tracks. (B) |B| and (C) Br along four tracks close to the fresh LP crater. AP and LP indicated by arrows and dashed black lines, respectively. The magnetic field is shown by the colors along the tracks. The white wiggles show |B| and Br as a function of distance along the track, and the scale bar in (B) denotes the amplitude. (D) Geological map (22) with track for topographic profile shown in (E). (F) A Mars Reconnaissance Orbiter Context Camera (CTX, 6 m/pixel resolution) image of the fresh crater highlighted by the red box in (D) and (E). Unit abbreviations are as follows: eNh, Early Noachian highland; HNt, Hesperian Noachian transition; eHt, Early Hesperian transition; mNh, Middle Noachian highland; Nve, Noachian volcanic effusive; Hve, Hesperian volcanic effusive.


Magnetism in certain rocks on Mars' surface indicate that the Martian dynamo was active between 4.3 and 4.2 billion years ago, but the absence of magnetism over three large basins that formed 3.9 billion years ago has led most scientists to believe the dynamo was inactive by that time.

The researchers analyzed new satellite data and found clear evidence of a magnetic field coming from the Lucus Planum lava flow that formed less than 3.7 billion years ago much later than the aforementioned basins.

The researchers also detected low-intensity magnetic fields over the Borealis Basin in the planet's northern hemisphere, which formed 4.5 billion years ago and is believed to be one of the oldest features on Mars.

"We have these two observations that point to a dynamo at the earliest known time in Mars' history, and a dynamo that was present half a billion years after many people thought it had already switched off," said Catherine Johnson, a professor in the department of earth, ocean and atmospheric sciences and senior scientist at the Planetary Science Institute in Tucson, Ariz., who also contributed to the study.

The researchers offer two possible explanations for the absence of magnetic fields over the basins: the dynamo may have stopped before the basins formed and then re-started before Lucus Planum formed, or the impacts that created the basins simply displaced the portion of crust containing minerals that can carry strong magnetism.

The new data for this study come from MAVEN, the Mars Atmosphere and Volatile Evolution satellite. Earlier data about magnetism on Mars had been gathered by the Mars Global Surveyor satellite which orbited the planet between 1999 and 2006, mostly at 400 kilometres above the surface. MAVEN, launched in 2013, operates as close as ~135 kilometres from the surface and picks up weaker signals that MGS could not detect.

MAVEN's ability to pick up signals from smaller features on and near the surface helps researchers distinguish whether the magnetism is coming from those, or from older rocks buried more deeply in the planet's crust. "These new data make it possible to predict the field on the surface of Mars, even if the contributions of any small spatial scale are still inaccessible from orbit," said Benoit Langlais, CNRS Research Director at the Laboratoire de Planetologie et Geodynamique (University of Nantes and University of Angers).

These new insights have researchers wondering what could be revealed if they get even closer. Mittelholz noted that this study focused on two particular features, but craters remain all over Mars with stories to tell. In the future, exploration could progress from satellites to drones or balloons, providing even more detailed data.


> Référence :

Timing of the martian dynamo: New constraints for a core fied at 4.5 and 3.7 Ga, Mittelholz1, C.L. Johnson1,2, J.M. Feinberg3, B. Langlais4, R.J. Phillips5, Science Advances, vol. 6, n°18

1- Department of Earth and Atmospheric Sciences, The University of British Columbia, Vancouver, Canada
2- Planetary Science Institute, Tucson, AZ, USA
3- Institute for Roc Magnetism, Department of Earth and Environmental Sciences, University of Minnesota, Minneapolis, MN55455, USA
4- Laboratoire de Planétologie et Géodynamique, UMR6112, Université de Nantes, Université d’Angers, CNRS, Nantes, France
5- Department of Earth and Planetary Sciences and Mc Donnell Center for the Space Sciences, Washington University in St. Louis, St. Louis, MO USA


> Contacts :
- Benoit Langlais, Senior Researcher CNRS
Email :
Phone : + 33 (0)2 76 64 51 57 / +33 (0)6 76 82 60 11