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No planet stirs human imagination quite like Mars. As non-stop land-based missions continue to probe its past and search for possible traces of life, another intrigue—this time high above its skyline—had long baffled scientists: how did Mars end up with its two small moons, Phobos and Deimos, first spotted in 1877? This riddle may have just been solved by a multidisciplinary study combining French, Belgian and Japanese expertise.1
Capture or Impact?
Scientists have long hesitated between two hypotheses. The first suggests that the moons are asteroids like those found in the belt between Jupiter and Mars; but why they should have been trapped around Mars remains unclear. An alternative theory posits that the moons formed from the debris of a collision between Mars and a protoplanet—a planet in the making; here though, uncertainty has hovered over the mechanism producing two small satellites. “A major difficulty has been to explain why a giant impact on Mars would have left two moons so different from our own Moon, a huge single mass, that also formed from Earth undergoing such an impact,” explains planetary scientist Sébastien Charnoz of the IPG,2 who contributed to the new study.
To shed light on this puzzle, the researchers3 pooled their expertise in astrophysics, planetary science, mathematics and computer science to create complex models running a range of hydrodynamic and numerical simulations able to recreate the sequence of past events. Their findings back up the second hypothesis of an almighty collision while also, for the first time, coherently filling in the gaps to explain how two moons emerged from the crash debris.
According to the simulations, Mars suffered a colossal impact with a body three times smaller some 4 to 4.5 billion years ago. Debris from the collision initially accumulated into a long disk around Mars, resembling one of Saturn’s rings. Within this disk, an enormous moon a thousand times the mass of Phobos gradually formed—similar to the way in which our Moon amassed from debris created by Earth’s impact.
The tide effect
The new study innovates by identifying the crucial factor differentiating moon formation around Mars and Earth: the planets’ differing rotation speeds, prompting “completely different tidal actions,” explains Charnoz. The scientist indicates that at the time of their respective giant impacts, “Earth took less than 4 hours to spin on its axis whereas Mars rotated very slowly over a 24-hour period.” The upshot of this divergence is that Earth kept a single large moon whereas debris from the Mars collision further collected into a dozen smaller moons alongside a larger companion. Eventually, Martian tide action due to the planet’s slow rotation caused most of the moons, including the largest one, to fall back onto the planet’s surface, leaving only the two most distant ones: Phobos and Deimos. Conversely, the Earth’s fast rotation pushed its moon further away.
In future analyses, the team plans to examine the “long-term dynamics of Phobos and Deimos,” says Charnoz. Fellow team member and planetary scientist Ryuki Hyodo, originally from Kobe University, currently also collaborating with the IPG, adds that “high-resolution impact simulations are still needed to understand more about the disk structure.”
Another moon "landing"
Even if concrete evidence is still required to confirm the team’s scenario, parallel findings certainly seem to back it up. A recent French study on the orbital and physical properties of the Martian moons points towards their formation from a colossal impact.4 And further plans are underway to gather more conclusive evidence. The Japan Aerospace Exploration Agency (JAXA) has announced a space mission commencing in 2022, with an expected return to Earth in 2026. “Its objective is to carry out close-up remote sensing and in-situ observations of both Phobos and Deimos, and to bring back samples from Phobos,” says Hyodo. The current study’s Franco-Belgian-Japanese collaboration has an exciting role to look forward to in this mission: JAXA will enlist them to conduct tests on the samples to determine whether this moon is indeed composed of a mixture of Martian mantle and debris from the vanished protoplanet as implied by their simulations.
The team’s input thus marks a crucial step towards deciphering the enigma. “More generally, our findings clarify how giant impacts give birth to satellites and can create a diverse variety of satellite systems,” explains Charnoz. Casting attention to other regions of our universe, the planetary scientist anticipates that the team could apply their method to study “Uranus and Neptune and—why not?—systems of satellites around exoplanets that we may identify in the future.”
- 1. P. Rosenblatt et al., “Accretion of Phobos and Deimos in an extended debris disc stirred by transient moons,” Nature Geoscience, 2016. DOI: 10.1038/NGEO2742.
- 2. Institut de Physique du Globe de Paris (CNRS / Université Paris Diderot).
- 3. From Université Paris Diderot, Royal Observatory of Belgium, Université de Rennes 1, CNRS and Earth Life Science Institute (Tokyo Institute of Technology), with additional support from IPGP, the Labex UnivEarthS and Kobe University.
- 4. T. Ronnet et al., “Reconciling the Orbital and Physical Properties of the Martian Moons,” Astrophysical Journal, forthcoming.
As well as contributing to the CNRSNews, Fui Lee Luk is a freelance translator for various publishing houses and websites. She has a PhD in French literature (Paris III / University of Sydney).