Phobos (moon)

"Mars I" redirects here. For the Soviet Mars probe, see Mars 1. For other uses, see Mars 1 (disambiguation).
Phobos

Enhanced-color image of Phobos with Stickney crater on the right
Discovery
Discovered by Asaph Hall
Discovery date 18 August 1877
Designations
Mars I
Adjectives Phobian
Orbital characteristics
Epoch J2000
Periapsis 9234.42 km[1]
Apoapsis 9517.58 km[1]
9376 km[1] (2.76 Mars radii)
Eccentricity 0.0151[1]
0.31891023 d
(7 h 39.2 min)
2.138 km/s[1]
Inclination 1.093° (to Mars's equator)
0.046° (to local Laplace plane)
26.04° (to the ecliptic)
Satellite of Mars
Physical characteristics
Dimensions 27 × 22 × 18 km[1]
Mean radius
 11.2667 km
(1.76941 mEarths)
1548.3 km2[1]
(3.03545 µEarths)
Volume 5783.61 km3
(5.33933 nEarths)
Mass 1.0659×1016 kg[1]
(1.78477 nEarths)
Mean density
 1.876 g/cm3[1]
0.0057 m/s2[1]
(581.4 µ g)
11.39 m/s
(41 km/h)[1]
Synchronous
Equatorial rotation velocity
 11.0 km/h (6.8 mph) (at longest axis)
0°
Albedo 0.071[2]
Temperature ≈ 233 K
11.3[3]

    Phobos (systematic designation: Mars I) is the larger and inner of the two natural satellites of Mars, the other being Deimos. Both moons were discovered in 1877.

    Phobos is a small, irregularly shaped object with a mean radius of 11 km,[1] and is seven times more massive than Deimos, Mars's outer moon. Phobos is named after the Greek god Phobos, a son of Ares (Mars) and Aphrodite (Venus) which was the personification of Horror. The name "Phobos" is pronounced /ˈfoʊbəs/ FOH-bəs, or like the Greek Φόβος.

    Phobos orbits 6,000 km (3,700 mi) from the Martian surface, closer to its primary than any other known planetary moon. It is so close that it orbits Mars faster than Mars rotates, and completes an orbit in just 7 hours and 39 minutes. As a result, from the surface of Mars it appears to rise in the west, move across the sky in 4 hours 15 min or less, and set in the east, twice each Martian day. Due to tidal interactions, Phobos is drawing closer to Mars by one meter every century, and it is predicted that in 50 million years it will collide with the planet or break up into a planetary ring.[4]

    Phobos is one of the least reflective bodies in the Solar System, and features a large impact crater, Stickney. The temperatures range from about −4 °C (25 °F) to −112 °C (−170 °F), on the sunlit and shadowed sides respectively.[4]

    Discovery

    Phobos was discovered by astronomer Asaph Hall on 18 August 1877, at the United States Naval Observatory in Washington, D.C., at about 09:14 Greenwich Mean Time (contemporary sources, using the pre-1925 astronomical convention that began the day at noon, give the time of discovery as 17 August at 16:06 Washington mean time).[5][6][7] Hall also discovered Deimos, Mars's other moon, on 12 August 1877 at about 07:48 UTC. The names, originally spelled Phobus and Deimus respectively, were suggested by Henry Madan (1838–1901), Science Master of Eton, based on Greek mythology, in which Phobos is a companion to the god Ares.[8][9]

    Physical characteristics

    Phobos has dimensions of 27 × 22 × 18 km,[1] and is too small to be rounded under its own gravity. Phobos does not have an atmosphere due to low mass and low gravity.[10] It is one of the least reflective bodies in the Solar System. Spectroscopically it appears to be similar to the D-type asteroids,[11] and is apparently of composition similar to carbonaceous chondrite material.[12] Phobos's density is too low to be solid rock, and it is known to have significant porosity.[13][14][15] These results led to the suggestion that Phobos might contain a substantial reservoir of ice. Spectral observations indicate that the surface regolith layer lacks hydration,[16][17] but ice below the regolith is not ruled out.[18][19]

    Phobos is heavily cratered.[20] The most prominent surface feature is the crater Stickney, named after Asaph Hall's wife, Angeline Stickney Hall, Stickney being her maiden name. As with Mimas's crater Herschel, the impact that created Stickney must have nearly shattered Phobos.[21] Many grooves and streaks also cover the oddly shaped surface. The grooves are typically less than 30 meters (98 ft) deep, 100 to 200 meters (330 to 660 ft) wide, and up to 20 kilometers (12 mi) in length, and were originally assumed to have been the result of the same impact that created Stickney. Analysis of results from the Mars Express spacecraft, however, revealed that the grooves are not in fact radial to Stickney, but are centered on the leading apex of Phobos in its orbit (which is not far from Stickney). Researchers suspect that they have been excavated by material ejected into space by impacts on the surface of Mars. The grooves thus formed as crater chains, and all of them fade away as the trailing apex of Phobos is approached. They have been grouped into 12 or more families of varying age, presumably representing at least 12 Martian impact events.[22]

    Faint dust rings produced by Phobos and Deimos have long been predicted but attempts to observe these rings have, to date, failed.[23] Recent images from Mars Global Surveyor indicate that Phobos is covered with a layer of fine-grained regolith at least 100 meters thick; it is hypothesized to have been created by impacts from other bodies, but it is not known how the material stuck to an object with almost no gravity.[24]

    The unique Kaidun meteorite that fell on a Soviet military base in Yemen in 1980, has been hypothesized to be a piece of Phobos, but this has been difficult to verify because little is known about the exact composition of Phobos.[25][26]

    Named geological features

    Geological features on Phobos are named after astronomers who studied Phobos and people and places from Jonathan Swift's Gulliver's Travels.[27] There is one named regio, Laputa Regio, and one named planitia, Lagado Planitia; both are named after places in Gulliver's Travels (the fictional Laputa, a flying island, and Lagado, imaginary capital of the fictional nation Balnibarbi).[28] The only named ridge on Phobos is Kepler Dorsum, named after the astronomer Johannes Kepler. Several craters have been named.[29]

    PHOBOS[30]


    Labeled Map of Phobos – Moon of Mars (USGS).[30]


    Crater Named after Coordinates
    Clustril Character in Gulliver's Travels 60°N 91°W / 60°N 91°W
    D'Arrest Heinrich Louis d'Arrest, astronomer 39°S 179°W / 39°S 179°W
    Drunlo Character in Gulliver's Travels 36°30′N 92°00′W / 36.5°N 92°W
    Flimnap Character in Gulliver's Travels 60°N 350°W / 60°N 350°W
    Grildrig Character in Gulliver's Travels 81°N 195°W / 81°N 195°W
    Gulliver Main character of Gulliver's Travels 62°N 163°W / 62°N 163°W
    Hall Asaph Hall, discoverer of Phobos 80°S 210°W / 80°S 210°W
    Limtoc Character in Gulliver's Travels 11°S 54°W / 11°S 54°W
    Öpik Ernst J. Öpik, astronomer 7°S 297°W / 7°S 297°W
    Reldresal Character in Gulliver's Travels 41°N 39°W / 41°N 39°W
    Roche Édouard Roche, astronomer 53°N 183°W / 53°N 183°W
    Sharpless Bevan Sharpless, astronomer 27°30′S 154°00′W / 27.5°S 154°W
    Shklovsky Iosif Shklovsky, astronomer 24°N 248°W / 24°N 248°W
    Skyresh Character in Gulliver's Travels 52°30′N 320°00′W / 52.5°N 320°W
    Stickney Angeline Stickney, wife of Asaph Hall 1°N 49°W / 1°N 49°W
    Todd David Peck Todd, astronomer 9°S 153°W / 9°S 153°W
    Wendell Oliver Wendell, astronomer 1°S 132°W / 1°S 132°W
    Enhanced-color view of the crater Stickney
    Stickney crater (MRO, 23 March 2008).
    Viking 1 image of Phobos, with Stickney to the right
    Phobos, with Stickney crater to the right (Viking 1, 2003).

    Orbital characteristics

    Orbits of Phobos and Deimos. Phobos is orbiting Mars 4 times faster than Deimos.

    Phobos has been described as "the best studied natural satellite in the Solar System",[31] and its close orbit around its parent planet produces some unusual effects. With an altitude of 5,989 kilometers (3,721 mi), Phobos orbits Mars below the synchronous orbit radius, meaning that it moves around Mars faster than Mars itself rotates.[14] Therefore from the point of view of an observer on the surface of Mars, it rises in the west, moves comparatively rapidly across the sky (in 4 h 15 min or less) and sets in the east, approximately twice each Martian day (every 11 h 6 min). Because it is close to the surface and in an equatorial orbit, it cannot be seen above the horizon from latitudes greater than 70.4°. Its orbit is so low that its angular diameter, as seen by an observer on Mars, varies visibly with its position in the sky. Seen at the horizon, Phobos is about 0.14° wide; at zenith it is 0.20°, one-third as wide as the full Moon as seen from Earth. By comparison, the Sun has an apparent size of about 0.35° in the Martian sky. Phobos's phases, inasmuch as they can be observed from Mars, take 0.3191 days (Phobos's synodic period) to run their course, a mere 13 seconds longer than Phobos's sidereal period. As seen from Phobos, Mars would appear 6,400 times larger and 2,500 times brighter than the full Moon appears from Earth, taking up a quarter of the width of a celestial hemisphere. The Mars–Phobos Lagrangian L1 is 2.5 kilometers (1.6 mi) above Stickney, which is unusually close to the surface.

    Solar transits

    Annular eclipse of the Sun by Phobos as viewed by the Mars Curiosity rover (20 August 2013).

    An observer situated on the Martian surface, in a position to observe Phobos, would see regular transits of Phobos across the Sun. Several of these transits have been photographed by the Mars Rover Opportunity. During the transits, Phobos's shadow is cast on the surface of Mars; an event which has been photographed by several spacecraft. Phobos is not large enough to cover the Sun's disk, and so cannot cause a total eclipse.

    Predicted destruction

    Tidal deceleration is gradually decreasing the orbital radius of Phobos. Bills and colleagues surveyed the literature and observations of Phobos's orbit and concluded that Phobos will be destroyed in less than 30–50 million years,[31] with one study's estimate being about 43 million years.[32] Given Phobos's irregular shape and assuming that it is a pile of rubble (specifically a Mohr–Coulomb body), it will eventually break up when it reaches approximately 2.1 Mars radii.[33]

    Origin

    Video (01:30/real-time): Eclipse of the Sun by Phobos, largest of the two Moons of Mars (Curiosity rover, 20 August 2013).

    The origin of the Martian moons is still controversial.[34] Phobos and Deimos both have much in common with carbonaceous C-type asteroids, with spectra, albedo, and density very similar to those of C- or D-type asteroids.[11] Based on their similarity, one hypothesis is that both moons may be captured main-belt asteroids.[35][36] Both moons 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 probably by a combination of atmospheric drag and tidal forces,[37] although it is not clear that sufficient time is available for this to occur for Deimos.[34] Capture also requires dissipation of energy. The current Martian atmosphere is too thin to capture a Phobos-sized object by atmospheric braking.[34] Geoffrey Landis has pointed out that the capture could have occurred if the original body was a binary asteroid that separated under tidal forces.[36]

    Curiosity's view of the Mars moons: Phobos passing in front of Deimos – in real-time (video-gif, 1 August 2013).

    Phobos could be a second-generation Solar System object that coalesced in orbit after Mars formed, rather than forming concurrently out of the same birth cloud as Mars.[38]

    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 large planetesimal.[39] The high porosity of the interior of Phobos (based on the density of 1.88 g/cm3, voids are estimated to comprise 25 to 35 percent of Phobos's volume) is inconsistent with an asteroidal origin.[40] Observations of Phobos in the thermal infrared suggest a composition containing mainly phyllosilicates, which are well known from the surface of Mars. The spectra are distinct from those of all classes of chondrite meteorites, again pointing away from an asteroidal origin.[41] Both sets of findings support an origin of Phobos from material ejected by an impact on Mars that reaccreted in Martian orbit,[42] similar to the prevailing theory for the origin of Earth's moon.

    Shklovsky's "Hollow Phobos" hypothesis

    In the late 1950s and 1960s, the unusual orbital characteristics of Phobos led to speculations that it might be hollow.

    Around 1958, Russian astrophysicist Iosif Samuilovich Shklovsky, studying the secular acceleration of Phobos's orbital motion, suggested a "thin sheet metal" structure for Phobos, a suggestion which led to speculations that Phobos was of artificial origin.[43] Shklovsky based his analysis on estimates of the upper Martian atmosphere's density, and deduced that for the weak braking effect to be able to account for the secular acceleration, Phobos had to be very light—one calculation yielded a hollow iron sphere 16 kilometers (9.9 mi) across but less than 6 cm thick.[43][44] In a February 1960 letter to the journal Astronautics,[45] Fred Singer, then science advisor to U.S. President Dwight D. Eisenhower, said of Shklovsky's theory:

    Globe of Phobos at the Memorial Museum of Astronautics in Moscow (19 May 2012).
    If the satellite is indeed spiraling inward as deduced from astronomical observation, then there is little alternative to the hypothesis that it is hollow and therefore Martian made. The big 'if' lies in the astronomical observations; they may well be in error. Since they are based on several independent sets of measurements taken decades apart by different observers with different instruments, systematic errors may have influenced them.[45]

    Subsequently, the systemic data errors that Singer predicted were found to exist, and the claim was called into doubt,[46] and accurate measurements of the orbit available by 1969 showed that the discrepancy did not exist.[47] Singer's critique was justified when earlier studies were discovered to have used an overestimated value of 5 cm/yr for the rate of altitude loss, which was later revised to 1.8 cm/yr.[48] The secular acceleration is now attributed to tidal effects,[46] which had not been considered in the earlier studies.

    The density of Phobos has now been directly measured by spacecraft to be 1.887 g/cm3.[49] Current observations are consistent with Phobos being a rubble pile.[49] In addition, images obtained by the Viking probes in the 1970s clearly showed a natural object, not an artificial one. Nevertheless, mapping by the Mars Express probe and subsequent volume calculations do suggest the presence of voids and indicate that it is not a solid chunk of rock but a porous body.[50] The porosity of Phobos was calculated to be 30% ± 5%, or a quarter to a third being empty. This void space is mostly on small scales (millimeters to ~1-m), between individual grains and boulders.[40]

    Exploration

    Launched missions

    Phobos slowly came into view over the decades as it was imaged at progressively higher resolutions. This image compares images from the Mars Spirit rover and an orbiter (2005).
    Illustration of the Phobos probe

    Phobos has been photographed in close-up by several spacecraft whose primary mission has been to photograph Mars. The first was Mariner 7 in 1969, followed by Viking 1 in 1977, Mars Global Surveyor in 1998 and 2003, Mars Express in 2004, 2008, and 2010,[51] and Mars Reconnaissance Orbiter in 2007 and 2008. On August 25, 2005, the Spirit Rover, with an excess of energy due to wind blowing dust off of its solar panels, took several short-exposure photographs of the night sky from the surface of Mars.[52] Phobos and Deimos are both clearly visible in the photograph.

    Dedicated Phobos probes were the Soviet Phobos 1 and Phobos 2, both launched in July 1988. The first was lost en route to Mars, whereas the second returned some data and images but failed shortly before beginning its detailed examination of Phobos's surface, including a lander. Other Mars missions collected more data, but the next dedicated mission attempt would be a sample return mission.

    The Russian Space Agency launched a sample return mission to Phobos in November 2011, called Fobos-Grunt. The return capsule also included a life science experiment of The Planetary Society, called Living Interplanetary Flight Experiment, or LIFE.[53] A second contributor to this mission was the China National Space Administration, which supplied a surveying satellite called "Yinghuo-1", which would have been released in the orbit of Mars, and a soil-grinding and sieving system for the scientific payload of the Phobos lander.[54][55][56] However, after achieving Earth orbit, the Fobos-Grunt probe failed to initiate subsequent burns that would have sent it off to Mars. Attempts to recover the probe were unsuccessful and it crashed back to Earth in January 2012.[57]

    Missions considered

    Fuel is mined from Phobos with the help of a nuclear reactor. (P. Rawlings, 1986)[58]

    In 1997 and 1998, the Aladdin mission was selected as a finalist in the NASA Discovery Program. The plan was to visit both Phobos and Deimos, and launch projectiles at the satellites. The probe would collect the ejecta as it performed a slow flyby (~1 km/s).[59] These samples would be returned to Earth for study three years later.[60][61] The Principal Investigator was Dr. Carle Pieters of Brown University. The total mission cost, including launch vehicle and operations was $247.7 million.[62] Ultimately, the mission chosen to fly was MESSENGER, a probe to Mercury.[63]

    In 2007, the European aerospace subsidiary EADS Astrium was reported to have been developing a mission to Phobos as a technology demonstrator. Astrium was involved in developing a European Space Agency plan for a sample return mission to Mars, as part of the ESA's Aurora programme, and sending a mission to Phobos with its low gravity was seen as a good opportunity for testing and proving the technologies required for an eventual sample return mission to Mars. The mission was envisioned to start in 2016, was to last for three years. The company planned to use a "mothership", which would be propelled by an ion engine, releasing a lander to the surface of Phobos. The lander would perform some tests and experiments, gather samples in a capsule, then return to the mothership and head back to Earth where the samples would be jettisoned for recovery on the surface.[64]

    Proposed missions

    The Phobos monolith (right of center) as taken by the Mars Global Surveyor (MOC Image 55103, 1998).

    In 2007, the Canadian Space Agency funded a study by Optech and the Mars Institute for an unmanned mission to Phobos known as PRIME (Phobos Reconnaissance and International Mars Exploration). A proposed landing site for the PRIME spacecraft is at the "Phobos monolith", a bright object near Stickney which casts a prominent shadow.[65][66][67] Astronaut Buzz Aldrin referred to this "monolith" in a July 22, 2009 interview with C-SPAN: "We should go boldly where man has not gone before. Fly by the comets, visit asteroids, visit the moon of Mars. There’s a monolith there. A very unusual structure on this potato shaped object that goes around Mars once in seven hours. When people find out about that they’re going to say ‘Who put that there? Who put that there?’ The universe put it there. If you choose, God put it there..."[68] The PRIME mission would be composed of an orbiter and lander, and each would carry 4 instruments designed to study various aspects of Phobos's geology.[69] As of 30 April 2009, PRIME does not have a projected launch date.

    In 2008, NASA Glenn Research Center began studying a Phobos and Deimos sample return mission that would use solar electric propulsion. The study gave rise to the "Hall" mission concept, a New Frontiers-class mission currently under further study.[70]

    As of January 2013, a new Phobos Surveyor mission is currently under development by a collaboration of Stanford University, NASA's Jet Propulsion Laboratory, and the Massachusetts Institute of Technology.[71] The mission is currently in the testing phases, and the team at Stanford plans to launch the mission between 2023 and 2033.[71]

    In March 2014, a Discovery class mission was proposed to place an orbiter on Mars orbit by 2021 and study Phobos and Deimos. It is called Phobos And Deimos & Mars Environment (PADME).[72][73]

    As part of a manned mission to Mars

    Phobos in 1998[74]

    Phobos has been proposed as an early target for a manned mission to Mars. The tele-operation of robotic scouts on Mars by humans on Phobos could be conducted without significant time delay, and planetary protection concerns in early Mars exploration might be addressed by such an approach.[75]

    Phobos has also been proposed as an early target for a manned mission to Mars because a landing on Phobos would be considerably less difficult and expensive than a landing on the surface of Mars itself. A lander bound for Mars would need to be capable of atmospheric entry and subsequent return to orbit, without any support facilities (a capacity that has never been attempted in a manned spacecraft), or would require the creation of support facilities in-situ (a "colony or bust" mission); a lander intended for Phobos could be based on equipment designed for lunar and asteroid landings.[76] Additionally, the delta-v to land on Phobos and return is only 80% of that for a trip to and from the surface of the Moon, partly due to Phobos's very weak gravity.[77]

    The human exploration of Phobos could serve as a catalyst for the human exploration of Mars and be exciting and scientifically valuable in its own right.[78]

    See also

    References

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    2. ↑ "Planetary Satellite Physical Parameters". JPL (Solar System Dynamics). 13 July 2006. Retrieved 29 January 2008.
    3. ↑ "Classic Satellites of the Solar System". Observatorio ARVAL. Retrieved 28 September 2007.
    4. ↑ 4.0 4.1 "NASA – Phobos". Solarsystem.nasa.gov. Retrieved 2014-08-04.
    5. ↑ "Notes: The Satellites of Mars". The Observatory 1 (6): 181–185. 20 September 1877. Bibcode:1877Obs.....1..181. Retrieved 4 February 2009.
    6. ↑ Hall, A. (17 October 1877). "Observations of the Satellites of Mars". Astronomische Nachrichten (Signed 21 September 1877) 91 (2161): 11/12–13/14. Bibcode:1877AN.....91...11H. doi:10.1002/asna.18780910103.
    7. ↑ Morley, T. A. (February 1989). "A Catalogue of Ground-Based Astrometric Observations of the Martian Satellites, 1877–1982". Astronomy and Astrophysics Supplement Series 77 (2): 209–226. Bibcode:1989A&AS...77..209M. (Table II, p. 220: first observation of Phobos on 18 August 1877.38498)
    8. ↑ Madan, H. G. (4 October 1877). "Letters to the Editor: The Satellites of Mars". Nature (Signed 29 September 1877) 16 (414): 475. Bibcode:1877Natur..16R.475M. doi:10.1038/016475b0.
    9. ↑ Hall, A. (14 March 1878). "Names of the Satellites of Mars". Astronomische Nachrichten (Signed 7 February 1878) 92 (2187): 47–48. Bibcode:1878AN.....92...47H. doi:10.1002/asna.18780920304.
    10. ↑ "Solar System Exploration: Planets: Mars: Moons: Phobos: Overview". Solarsystem.nasa.gov. Retrieved 19 August 2013.
    11. ↑ 11.0 11.1 "New Views of Martian Moons".
    12. ↑ Lewis, J. S. (2004). Physics and Chemistry of the Solar System. Elsevier Academic Press. p. 425. ISBN 0-12-446744-X.
    13. ↑ "Porosity of Small Bodies and a Reassesment of Ida's Density". When the error bars are taken into account, only one of these, Phobos, has a porosity below 0.2...
    14. ↑ 14.0 14.1 "Close Inspection for Phobos". It is light, with a density less than twice that of water, and orbits just 5,989 kilometers (3,721 mi) above the Martian surface.
    15. ↑ 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.
    16. ↑ Murchie, S. L.; Erard, S.; Langevin, Y.; Britt, D. T. et al. (1991). "Disk-resolved Spectral Reflectance Properties of Phobos from 0.3–3.2 microns: Preliminary Integrated Results from PhobosH 2". Abstracts of the Lunar and Planetary Science Conference 22: 943. Bibcode:1991pggp.rept..249M.
    17. ↑ Rivkin, A. S. et al. (March 2002). "Near-Infrared Spectrophotometry of Phobos and Deimos". Icarus 156 (1): 64. Bibcode:2002Icar..156...64R. doi:10.1006/icar.2001.6767.
    18. ↑ Fanale, F. P.; Salvail, J. R. (1989). "Loss of water from Phobos". Geophys. Res. Lett. 16 (4): 287–290. Bibcode:1989GeoRL..16..287F. doi:10.1029/GL016i004p00287.
    19. ↑ Fanale, Fraser P.; Salvail, James R. (Dec 1990). "Evolution of the water regime of Phobos". Icarus 88: 380–395. Bibcode:1990Icar...88..380F. doi:10.1016/0019-1035(90)90089-R.
    20. ↑ "Phobos".
    21. ↑ "Stickney Crater-Phobos". One of the most striking features of Phobos, aside from its irregular shape, is its giant crater Stickney. Because Phobos is only 28 by 20 kilometers (17 by 12 mi), it must have been nearly shattered from the force of the impact that caused the giant crater. Grooves that extend across the surface from Stickney appear to be surface fractures caused by the impact.
    22. ↑ Murray, J. B. et al. "New Evidence on the Origin of Phobos' Parallel Grooves from HRSC Mars Express" (PDF). 37th Annual Lunar and Planetary Science Conference, March 2006.
    23. ↑ Showalter, M. R.; Hamilton, D. P.; Nicholson, P. D. (2006). "A Deep Search for Martian Dust Rings and Inner Moons Using the Hubble Space Telescope" (PDF). Planetary and Space Science 54 (9–10): 844–854. Bibcode:2006P&SS...54..844S. doi:10.1016/j.pss.2006.05.009.
    24. ↑ Britt, Robert Roy (13 March 2001). "Forgotten Moons: Phobos and Deimos Eat Mars' Dust". space.com. Retrieved 12 May 2010.
    25. ↑ Ivanov, Andrei V. (March 2004). "Is the Kaidun Meteorite a Sample from Phobos?". Solar System Research 38 (2): 97–107. Bibcode:2004SoSyR..38...97I. doi:10.1023/B:SOLS.0000022821.22821.84.
    26. ↑ Ivanov, Andrei; Michael Zolensky (2003). "The Kaidun Meteorite: Where Did It Come From?" (PDF). Lunar and Planetary Science 34. The currently available data on the lithologic composition of the Kaidun meteorite– primarily the composition of the main portion of the meteorite, corresponding to CR2 carbonaceous chondrites and the presence of clasts of deeply differentiated rock – provide weighty support for considering the meteorite’s parent body to be a carbonaceous chondrite satellite of a large differentiated planet. The only possible candidates in the modern Solar System are Phobos and Deimos, the moons of Mars.
    27. ↑ Gazetteer of Planetary Nomenclature USGS Astrogeology Research Program, Categories
    28. ↑ Gazetteer of Planetary Nomenclature USGS Astrogeology Research Program, Phobos
    29. ↑ Gazetteer of Planetary Nomenclature USGS Astrogeology Research Program, Craters
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    32. ↑ Efroimsky, M.; Lainey, V. (2007). "Physics of bodily tides in terrestrial planets and the appropriate scales of dynamical evolution.". Journal of Geophysical Research 112 (E12): E12003. arXiv:0709.1995. Bibcode:2007JGRE..11212003E. doi:10.1029/2007JE002908.
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    34. ↑ 34.0 34.1 34.2 Burns, J. A. "Contradictory Clues as to the Origin of the Martian Moons," in Mars, H. H. Kieffer et al., eds., U. Arizona Press, Tucson, 1992
    35. ↑ "Close Inspection for Phobos". One idea is that Phobos and Deimos, Mars's other moon, are captured asteroids.
    36. ↑ 36.0 36.1 Landis, G. A. "Origin of Martian Moons from Binary Asteroid Dissociation," American Association for the Advancement of Science Annual Meeting; Boston, MA, 2001; abstract.
    37. ↑ Cazenave, A.; Dobrovolskis, A.; Lago, B. (1980). "Orbital history of the Martian satellites with inferences on their origin". Icarus 44 (3): 730–744. Bibcode:1980Icar...44..730C. doi:10.1016/0019-1035(80)90140-2.
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