Rings of mars
Pro Research Analysisby 
Searched over 200M research papers
Formation and Existence of Mars' Rings: Phobos and Deimos Dust Rings
Mars is theorized to have faint rings made of dust, primarily generated by its two small moons, Phobos and Deimos. These moons are constantly bombarded by micrometeoroids, which knock dust off their surfaces and into orbit around Mars. This process is similar to how faint rings are formed around the giant planets in our solar system, such as Jupiter and Saturn 125. The dust from these impacts is distributed by Mars' gravity, its slightly flattened shape (oblateness), and solar radiation, creating rings or toroidal (doughnut-shaped) clouds of dust around the planet 12.
Structure and Dynamics of Martian Dust Rings
Theoretical models predict that the dust from Deimos forms a wide, thick torus, while the dust from Phobos creates a much thinner ring. The Deimos torus is estimated to be about 7,000 km high and 50,000 km wide, while the Phobos ring is about 400 km thick and extends up to 30,000 km from Mars . These rings are not perfectly symmetrical; they are offset and shaped by the combined effects of Mars' gravity, its oblateness, and solar radiation. For example, the Deimos ring is displaced away from the Sun, while the Phobos ring is offset toward the Sun. The rings are also time-variable and vertically asymmetric, with their shapes changing as the dust grains interact with Mars and the Sun 12.
Observational Evidence and Detection Efforts
Despite strong theoretical support, direct detection of Mars' rings has proven difficult. Multiple attempts using spacecraft imaging and plasma instruments have not conclusively identified these rings 14. Observations from the Viking Orbiter and other missions have failed to find clear evidence of rings, though some controversial data from the Phobos-2 spacecraft have been interpreted as possible signs of ring material 14. Proposals have been made to use more sensitive instruments, such as the Spitzer Space Telescope, to search for these elusive dust rings .
Cyclic Ring-Satellite Evolution and Martian History
Recent research suggests that Mars may have experienced several cycles of ring and satellite formation throughout its history. As Phobos' orbit decays due to tidal forces, it is predicted to eventually break apart and form a new ring around Mars. This ring would gradually spread out, with most of the material falling onto Mars and some forming new moons. This cycle may have occurred multiple times, explaining the current orbits and characteristics of Phobos and Deimos 368. The process of ring formation and deposition could also be linked to unusual sedimentary deposits observed on Mars' surface .
Future of Phobos and Martian Ring Formation
Phobos is slowly spiraling inward toward Mars and is expected to break apart due to tidal stresses in 20 to 70 million years. When this happens, a dense ring will form, similar in mass density to Saturn's rings, but it will only last for a few million to a hundred million years before the material either falls onto Mars or forms new satellites 36. This ongoing process highlights the dynamic nature of Mars' satellite and ring system.
Conclusion
While no rings have been directly observed around Mars, strong theoretical and indirect evidence supports their existence. The dust rings are thought to be continually replenished by impacts on Phobos and Deimos, shaped by complex gravitational and solar forces, and may play a key role in the long-term evolution of Mars' moons. Future observations and missions may finally confirm the presence of these faint, elusive rings.
Sources and full results
Most relevant research papers on this topic