An enhanced-color image of Deimos (MRO, 21 February 2009).
Image: NASA/JPL-Caltech/University of Arizona
|Discovered by||Asaph Hall|
|Discovery date||12 August 1877|
Average orbital speed
|Inclination||0.93° (to Mars's equator)
1.791° (to the local Laplace plane)
27.58° (to the ecliptic)
|Dimensions||15 × 12.2 × 11 km|
|6.2 ± 0.18 km
|Albedo||0.068 ± 0.007|
|Temperature||≈ 233 K|
|12.45 ± 0.05 |
Deimos (systematic designation: Mars II) is the smaller and outermore of the two natural satellites of the planet Mars with a mean radius of 6.2 km, the other being Phobos. Deimos takes 30.3 hours to orbit Mars. The name "Deimos" is pronounced // DY-məs, or sometimes // DEE-məs or like the Greek Δείμος. In Greek mythology, Deimos was the twin brother of Phobos and personified Terror.
Deimos was discovered by Asaph Hall, Sr. at the United States Naval Observatory in Washington, D.C on 12 August 1877, at about 07:48 UTC (given in contemporary sources as "11 August 14:40" Washington mean time, using an astronomical convention of beginning a day at noon, so 12 hours must be added to get the actual local mean time). Hall also discovered Phobos on 18 August 1877, at about 09:14 GMT, after deliberately searching for Martian moons.
It is named after Deimos, a figure representing dread in Greek Mythology. The names, at first spelled Phobus and Deimus, were suggested by Henry Madan (1838–1901), Science Master of Eton, from Book XV of the Iliad, where Ares (the Roman god Mars) summons Dread (Deimos) and Fear (Phobos).
Deimos, like Mars's other moon, Phobos, has spectra, albedos and densities similar to those of a C- or D-type asteroid. Like most bodies of its size, Deimos is highly non-spherical with triaxial dimensions of 15 × 12.2 × 11 km making it 0.56 times the size of Phobos. Deimos is composed of rock rich in carbonaceous material, much like C-type asteroids and carbonaceous chondrite meteorites. It is cratered, but the surface is noticeably smoother than that of Phobos, caused by the partial filling of craters with regolith. The regolith is highly porous and has a radar-estimated density of only 1.471 g/cm3. The two largest craters, Swift and Voltaire, each measure about 3 km (1.9 mi) across.
Named geological features
Only two geological features on Deimos have been given names. The craters Swift and Voltaire are named after writers who speculated on the existence of two Martian moons before Phobos and Deimos were discovered.
|Crater||Named after||Coordinates||Diameter (m)|
Deimos's orbit is nearly circular and is close to Mars's equatorial plane. Deimos, Mars's outer moon, is possibly an asteroid that was perturbed by Jupiter into an orbit that allowed it to be captured by Mars, though this hypothesis is still controversial and disputed. Both Deimos and Phobos have very circular orbits which lie almost exactly in Mars's equatorial plane, and hence a capture origin requires a mechanism for circularizing the initially highly eccentric orbit, and adjusting its inclination into the equatorial plane, most likely by a combination of atmospheric drag and tidal forces, although it is not clear that sufficient time was available for this to have occurred for Deimos.
As seen from Mars, Deimos would have an angular diameter of no more than 2.5 minutes (sixty minutes make one degree), one twelfth of the width of the Moon as seen from Earth, and would therefore appear almost star-like to the naked eye. At its brightest ("full moon") it would be about as bright as Venus is from Earth; at the first- or third-quarter phase it would be about as bright as Vega. With a small telescope, a Martian observer could see Deimos's phases, which take 1.2648 days (Deimos's synodic period) to run their course.
Unlike Phobos, which orbits so fast that it actually rises in the west and sets in the east, Deimos rises in the east and sets in the west. However, the Sun-synodic orbital period of Deimos of about 30.4 hours exceeds the Martian solar day ("sol") of about 24.7 hours by such a small amount that 2.7 days elapse between its rising and setting for an equatorial observer.
Because Deimos's orbit is relatively close to Mars and has only a very small inclination to Mars's equator, it cannot be seen from Martian latitudes greater than 82.7°.
Deimos regularly passes in front of the Sun as seen from Mars. It is too small to cause a total eclipse, appearing only as a small black dot moving across the Sun. Its angular diameter is only about 2.5 times the angular diameter of Venus during a transit of Venus from Earth. On 4 March 2004 a transit of Deimos was photographed by Mars Rover Opportunity, and on 13 March 2004 a transit was photographed by Mars Rover Spirit.
The origin of the Martian moons is still controversial. The main hypotheses are that they formed either by capture or by accretion. Because of the similarity to the composition of C- or D-type asteroids, one hypothesis is that the moons may be objects captured into Martian orbit from the asteroid belt, with orbits that have been circularized either by atmospheric drag or tidal forces, as capture requires dissipation of energy. The current Martian atmosphere is too thin to capture a Phobos-sized object by atmospheric braking. Geoffrey Landis has pointed out that the capture could have occurred if the original body was a binary asteroid that separated due to tidal forces. The main alternative hypothesis is that the moons accreted in the present position. Another hypothesis is that Mars was once surrounded by many Phobos- and Deimos-sized bodies, perhaps ejected into orbit around it by a collision with a planetesimal.
Overall, its exploration history is similar to Mars and Phobos. However, no landing or sample returns have been attempted.
A sample return mission called Gulliver has been conceptualized, in which 1 kilogram (2.2 pounds) of material from Deimos would be returned to Earth. Another design is OSIRIS-REx 2, which would use heritage from the first OSIRIS-REx.
- List of natural satellites
- List of missions to the moons of Mars
- Moons of Mars
- Phobos and Deimos in fiction
- Transit of Deimos from Mars
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- Deimos - Viking 2 Orbiter
- Busch, M. W. et al. (2007). "Arecibo Radar Observations of Phobos and Deimos". Icarus 186 (2): 581–584. Bibcode:2007Icar..186..581B. doi:10.1016/j.icarus.2006.11.003.
- of Planetary Nomenclature, USGS Astrogeology Research Program
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- Nomenclature: Crater, craters
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accumulated ejecta from asteroid impacts on the Martian surface
- Mars Phobos and Deimos Survey (M-PADS)–A Martian Moons Orbiter and Phobos Lander (Ball, Andrew J.; Price, Michael E.; Walker, Roger J.; Dando, Glyn C.; Wells, Nigel S. and Zarnecki, John C. (2009). Mars Phobos and Deimos Survey (M-PADS)–A Martian Moons Orbiter and Phobos Lander. Advances in Space Research, 43(1), pp. 120–127.)
- Dr. Britt - The Gulliver Mission: Sample Return from Deimos
- Elifritz, T. L. - OSIRIS-REx II to Mars
- Lee, Pascal; Bicay, Michael; Colapre, Anthony; Elphic, Richard (March 17–21, 2014). "Phobos And Deimos & Mars Environment (PADME): A LADEE-Derived Mission to Explore Mars's Moons and the Martian Orbital Environment." (PDF). 45th Lunar and Planetary Science Conference (2014).
- Reyes, Tim (1 October 2014). "Making the Case for a Mission to the Martian Moon Phobos". Universe Today. Retrieved 2014-10-05.
|Wikimedia Commons has media related to Deimos (moon).|
- Deimos Profile by NASA's Solar System Exploration
- Deimos rotation movie
- Animation of Deimos
- USGS Deimos nomenclature