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Phobos (pronounced /ˈfoʊbəs/ FOE-bəs, or as Greek Φόβος) (systematic designation: Mars I) is the larger and closer of the two moons of Mars, the other being Deimos. Both moons were discovered in 1877. With a mean radius of 11.1 km (6.9 mi), Phobos is 7.24 times as massive as Deimos. It is named after the Greek god Phobos (which means "fear"), a son of Ares (Mars).

A small, irregularly shaped object, Phobos orbits about 9,377 km (5,827 mi) from the center of Mars, closer to its primary than any other known planetary moon. Phobos is one of the least-reflective bodies in the solar system, and features a large impact crater, Stickney crater. It orbits so close to the planet that it moves around Mars faster than Mars itself rotates. As a result, from the surface of Mars it appears to rise in the west, move rapidly across the sky (in 4 h 15 min or less) and sets in the east. Phobos's orbital radius is decreasing and it will eventually either impact the surface of Mars or break up into a planetary ring.

The Martian Moon Phobos - Full 360 Degree View | ESA Mars Space Science HD

Main article: History of the moons of Mars

Phobos was discovered by astronomer Asaph Hall on August 18, 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 August 17 16:06 Washington mean time).[8][9][10] Hall also discovered Deimos, Mars' other moon. The names, originally spelled Phobus and Deimus respectively, were suggested by Henry Madan (1838–1901), Science Master of Eton, based on Book XV of the Iliad, in which the god Ares summons Dread (Deimos) and Fear (Phobos).[11][12]

Physical characteristics
A mosaic of three separate images taken by Viking 1 on October 19, 1978. The large crater (mostly in darkness) on the upper left is Stickney.

Phobos is one of the least-reflective bodies in the solar system. Spectroscopically it appears to be similar to the D-type asteroids,[13] and is apparently of composition similar to carbonaceous chondrite material.[14] Phobos' density is too low to be solid rock, and it is known to have significant porosity.[15][16][17] 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,[18][19] but ice below the regolith is not ruled out.[20]

Faint dust rings produced by Phobos and Deimos have long been predicted but attempts to observe these rings have, to date, failed.[21] 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.[22]

Phobos is highly non-spherical, with dimensions of 27 × 22 × 18 km.[2] Because of its shape alone, the gravity on its surface varies by about 210%; the tidal forces raised by Mars more than double this variation (to about 450%) because they compensate for a little more than half of Phobos' gravity at its sub- and anti-Mars poles.[citation needed]

Phobos is heavily cratered.[23] The most prominent surface feature is Stickney crater, 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.[24] 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.[25]

The unique Kaidun meteorite is thought to be a piece of Phobos, but this has been difficult to verify since little is known about the detailed composition of the moon.[26][27]

"Hollow Phobos" suggestions

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' orbital motion, suggested a "thin sheet metal" structure for Phobos, a suggestion which led to speculations that Phobos was of artificial origin.[28] 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 kilometres (9.9 mi) across but less than 6 cm thick.[28][29] In a February 1960 letter to the journal Astronautics,[30] Fred Singer, then science advisor to U.S. President Dwight D. Eisenhower, said of Shklovsky's theory:

[Phobos'] purpose would probably be to sweep up radiation in Mars' atmosphere, so that Martians could safely operate around their planet.
My conclusion there is, and here I back Shklovsky, that 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.[30]

Subsequently, the systemic data errors that Singer predicted were found to exist, and the claim was called into doubt,[31] and accurate measurements of the orbit available by 1969 showed that the discrepancy did not exist.[32] Singer's critique was justified when earlier studies were later 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.[33] The secular acceleration is now attributed to tidal effects, 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,[4] which is inconsistent with a hollow shell. In addition, images obtained by the Viking probes in the 1970s clearly showed a natural object, not an artificial one, and the "hollow Phobos" speculations have been relegated to the status of a historical curiosity.

However, mapping by the Mars Express probe and subsequent volume calculations do suggest the presence of voids within the moon and indicate that it is not a solid chunk of rock but a porous body instead.[34] The porosity of Phobos was calculated to be 30% ± 5%, or a quarter to a third of the moon being hollow. This void space is mostly on small scales (millimeters to ~1-m), between individual grains and boulders [6].

Named geological features
Color view of Stickney Crater by the Mars Reconnaissance Orbiter.
Some of the named craters of Phobos. C = Clustril; D = Drunlo; F = Flimnap; L = Limtoc; R = Reldresal; S = Stickney; Sk = Skyresh. Grildrig is on the horizon below Skyresh and Flimnap.

Geological features on Phobos are named after astronomers who studied Phobos and people and places from Jonathan Swift's Gulliver's Travels.[35] The only named ridge on Phobos is Kepler Dorsum, named after the astronomer Johannes Kepler. Several craters have been named.[36]
Crater Named after Coordinates
Clustril Character in Gulliver's Travels 60°N 91°W / 60°N 91°W / 60; -91 (Clustril)
D'Arrest Heinrich Louis d'Arrest, astronomer 39°S 179°W / 39°S 179°W / -39; -179 (D'Arrest)
Drunlo Character in Gulliver's Travels 36°30′N 92°00′W / 36.5°N 92°W / 36.5; -92 (Drunlo)
Flimnap Character in Gulliver's Travels 60°N 350°W / 60°N 350°W / 60; -350 (Flimnap)
Grildrig Character in Gulliver's Travels 81°N 195°W / 81°N 195°W / 81; -195 (Grildrig)
Gulliver Main character of Gulliver's Travels 62°N 163°W / 62°N 163°W / 62; -163 (Gulliver)
Hall Asaph Hall, discoverer of Phobos 80°S 210°W / 80°S 210°W / -80; -210 (Hall)
Limtoc Character in Gulliver's Travels 11°S 54°W / 11°S 54°W / -11; -54 (Limtoc)
Reldresal Character in Gulliver's Travels 41°N 39°W / 41°N 39°W / 41; -39 (Reldresal)
Roche Édouard Roche, astronomer 53°N 183°W / 53°N 183°W / 53; -183 (Roche)
Sharpless Bevan Sharpless, astronomer 27°30′S 154°00′W / 27.5°S 154°W / -27.5; -154 (Sharpless)
Skyresh Character in Gulliver's Travels 52°30′N 320°00′W / 52.5°N 320°W / 52.5; -320 (Skyresh)
Stickney Angeline Stickney, wife of Asaph Hall 1°N 49°W / 1°N 49°W / 1; -49 (Stickney)
Todd David Peck Todd, astronomer 9°S 153°W / 9°S 153°W / -9; -153 (Todd)
Wendell Oliver Wendell, astronomer 1°S 132°W / 1°S 132°W / -1; -132 (Wendell)

Orbital characteristics
Orbits of Phobos and Deimos (to scale), seen from above Mars' north pole. Phobos is orbiting Mars 3.96 times faster than Deimos.

Phobos' unusually close orbit around its parent planet produces some unusual effects. It orbits Mars below the synchronous orbit radius, meaning that it moves around Mars faster than Mars itself rotates. Therefore 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). Since 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' phases, inasmuch as they can be observed from Mars, take 0.3191 days (Phobos' synodic period) to run their course, a mere 13 seconds longer than Phobos' 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 Lagrange 1 point is 2.5 kilometres (1.6 mi) above Stickney Crater, which is unusually close to the surface.

Phobos transits Sun, as seen by Mars Rover Opportunity

Solar transits
Main article: Transit of Phobos from Mars

An observer situated on the Martian surface, in a position to observe Phobos, would see regular transits of the moon across the Sun. Several of these transits have been photographed by the Mars Rover Opportunity. During the transits, Phobos' 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.

Future destruction

Because Phobos' orbital period is shorter than a Martian day, tidal deceleration is decreasing its orbital radius at the rate of about 20 metres (66 ft) per century. In an estimated 11 million years it will either impact the surface of Mars or, more likely, break up into a planetary ring.[37] Given Phobos' irregular shape and assuming that it is a pile of rubble (specifically a Mohr-Coulomb body), it has been calculated that Phobos is currently stable with respect to tidal forces. But it is estimated that Phobos will pass the Roche Limit for a rubble pile when its orbital radius drops by a little over 2,000 kilometers (1,200 mi) to about 7,100 kilometers (4,400 mi). Newer calculations suggests this will happen in just 7.6 million years from now.[38] At this distance, Phobos will likely begin to break up and form a ring system which will continue to spiral slowly into Mars.[39]

Viking 1 image of Phobos, with Stickney Crater to the right

The origin of the Martian moons is still controversial.[40] 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.[13] Based on their similarity, one hypothesis is that both moons may be captured main belt asteroids.[41][42] 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 likely by a combination of atmospheric drag and tidal forces,[43] although it is not clear that sufficient time is available for this to occur for Deimos.[40] Capture also requires dissipation of energy. The current Mars atmosphere is too thin to capture a Phobos-sized object by atmospheric braking.[40] Geoffrey Landis has pointed out that the capture could have occurred if the original body was a binary asteroid that separated under tidal forces.[42]

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.[44] 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.[45]

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

Phobos has been photographed in close-up by several spacecraft whose primary mission has been to photograph Mars. The first was Mariner 9 in 1971, followed by Viking 1 in 1977, Mars Global Surveyor in 1998 and 2003, Mars Express in 2004, 2008, and 2010,[46] and Mars Reconnaissance Orbiter in 2007 and 2008. In Summer 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. Phobos and Deimos are both clearly visible in the photograph. The only dedicated Phobos probes have been the Soviet Phobos 1 and Phobos 2, both launched in July 1988. The first was lost en route to Mars, while the second returned unusual data and images but failed shortly before beginning its detailed examination of the moon's surface.

Future missions

The Russian Space Agency is planning to launch a sample return mission to Phobos in 2011, called Phobos-Grunt. The return capsule will include a life science experiment of The Planetary Society, called Living Interplanetary Flight Experiment, or LIFE.[47] A second contributor to this mission is the China National Space Administration, which is sending a surveying satellite called "Yinghuo-1", which will be released in the orbit of Mars, and a soil grinding and sieving system for the scientific payload of the Phobos lander.[48][49][50]

In 2007, the European aerospace subsidiary EADS Astrium was reported to have been developing a mission to Phobos as a technology demonstrator. Astrium is 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 the low gravity Phobos is seen as a good opportunity for testing and proving the technologies required for an eventual sample return mission to Mars. The mission is envisioned to start in 2016, and last for three years. The company plans 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.[51]

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.[52][53] 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...”[54] The PRIME mission would be composed of an orbiter and lander, and each would carry 4 instruments designed to study various aspects of Phobos' geology.[55] As of 30 April 2009 (2009 -04-30)[update], PRIME does not have a projected launch date.

Phobos has also been proposed as an early target for a manned mission to Mars, since a landing on Phobos would be considerably less difficult and expensive than a landing on the surface of Mars itself.[56] A lander bound for Mars would need to be capable of atmospheric entry and subsequent return to orbit, without any support facilities (a capacity which 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.

See also


1. ^ NASA Celestia
2. ^ a b "Mars: Moons: Phobos". NASA Solar System Exploration. September 30, 2003. Retrieved August 18, 2008.
3. ^ a b "Planetary Satellite Physical Parameters". JPL (Solar System Dynamics). July 13, 2006. Retrieved January 29, 2008.
4. ^ a b "Mars Express closes in on the origin of Mars' larger moon". DLR. October 16, 2008. Retrieved October 16, 2008.
5. ^ a b use a spherical radius of 11.1 km (6.9 mi); volume of a sphere * density of 1.877 g/cm³ yields a mass (m=d*v) of 1.07 × 1016 kg and an escape velocity (sqrt((2*g*m)/r)) of 11.3 m/s (40 km/h)
6. ^ a b "Precise mass determination and the nature of Phobos". Geophysical Research Letters, Vol. 37. . Retrieved May 31, 2010.
7. ^ "Classic Satellites of the Solar System". Observatorio ARVAL. Retrieved September 28, 2007.
8. ^ "Notes: The Satellites of Mars". The Observatory 1 (6): 181–185. September 20, 1877. Retrieved February 4, 2009.
9. ^ Hall, A. (October 17, 1877, signed September 21, 1877). Observations of the Satellites of Mars. 91. Astronomische Nachrichten. pp. 11/12–13/14. Retrieved February 4, 2009.
10. ^ Morley, T. A. (February 1989). "A Catalogue of Ground-Based Astrometric Observations of the Martian Satellites, 1877-1982". Astronomy and Astrophysics Supplement Series (ISSN 0365-0138) 77 (2): 209–226. (Table II, p. 220: first observation of Phobos on August 18, 1877.38498)
11. ^ Madan, H. G. (October 4, 1877, signed September 29, 1877). "Letters to the Editor: The Satellites of Mars". Nature (Macmillan Journals ltd.) 16 (414): 475. doi:10.1038/016475b0.
12. ^ Hall, A. (March 14, 1878, signed February 7, 1878). "Names of the Satellites of Mars". Astronomische Nachrichten 92 (2187): 47–48. doi:10.1002/asna.18780920304.
13. ^ a b "New Views of Martian Moons".
14. ^ Lewis, J. S. (2004). Physics and Chemistry of the Solar System. Elsevier Academic Press. pp. 425. ISBN 0-12-446744-X.
15. ^ "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..."
16. ^ "Close Inspection for Phobos". "It is light, with a density less than twice that of water, and orbits just 5,989 kilometres (3,721 mi) above the Martian surface."
17. ^ Busch, M. W.; et al. (2007). "Arecibo Radar Observations of Phobos and Deimos". Icarus 186 (2): 581–584. doi:10.1016/j.icarus.2006.11.003.
18. ^ Murchie, S. L.; Erard, S., Langevin, Y., Britt, D. T., Bibring, J. P., and Mustard, J. F. (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.
19. ^ Rivkin, A. S.; et al. (March 2002). "Near-Infrared Spectrophotometry of Phobos and Deimos". Icarus 156 (1): 64. doi:10.1006/icar.2001.6767.
20. ^ Fanale, Fraser P., "Water regime of Phobos" (1991).
21. ^ Showalter, M. R.; Hamilton, D. P. and 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: 844–854.
22. ^ Britt, Robert Roy (March 13, 2001). "Forgotten Moons: Phobos and Deimos Eat Mars' Dust". Retrieved May 12, 2010.
23. ^ "Phobos".
24. ^ "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 kilometres (17 by 12 mi), the moon 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."
25. ^ 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.
26. ^ Ivanov, Andrei V. (March 2004). "Is the Kaidun Meteorite a Sample from Phobos?". Solar System Research 38 (2): 97–107. doi:10.1023/B:SOLS.0000022821.22821.84. Retrieved 20 August 2009.
27. ^ 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.".
28. ^ a b Shklovsky, I. S.; The Universe, Life, and Mind, Academy of Sciences USSR, Moscow, 1962
29. ^ Öpik, E. J. (September 1964). "Is Phobos Artificial?". Irish Astronomical Journal, Vol. 6. pp. 281–283. Retrieved February 4, 2009.
30. ^ a b Singer, S. F.; Astronautics, February 1960
31. ^ Öpik, E. J. (March 1963, signed September 1962). "News and Comments: Phobos, Nature of Acceleration". Irish Astronomical Journal, Vol. 6. pp. 40. Retrieved February 4, 2009.
32. ^ Singer, S. F. (1967). "On the Origin of the Martian Satellites Phobos and Deimos". Seventh International Space Science Symposium held May 10–18, 1966 in Vienna, North-Holland Publishing Company. .
33. ^ "More on the Moons of Mars". Singer, S. F., Astronautics, February 1960. American Astronautical Society. Page 16
34. ^ "Cheap Flights to Phobos" by Stuart Clark, in New Scientist magazine, 30th January 2010.
35. ^ Gazetteer of Planetary Nomenclature USGS Astrogeology Research Program, Categories
36. ^ Gazetteer of Planetary Nomenclature USGS Astrogeology Research Program, Craters
37. ^ Sharma, B. K. (May 10, 2008). "Theoretical Formulation of the Phobos, moon of Mars, rate of altitudinal loss".
38. ^ Phobos Might Only Have 10 Million Years to Live
39. ^ Holsapple, K. A. (December 2001). "Equilibrium Configurations of Solid Cohesionless Bodies". Icarus 154 (2): 432–448. doi:10.1006/icar.2001.6683. Retrieved November 12, 2007.
40. ^ a b c 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
41. ^ "Close Inspection for Phobos". "One idea is that Phobos and Deimos, Mars's other moon, are captured asteroids."
42. ^ a b Landis, G. A. "Origin of Martian Moons from Binary Asteroid Dissociation," American Association for the Advancement of Science Annual Meeting; Boston, MA, 2001; abstract.
43. ^ Cazenave, A.; Dobrovolskis, A.; Lago, B. (1980). "Orbital history of the Martian satellites with inferences on their origin". Icarus 44 (3): 730–744. doi:10.1016/0019-1035(80)90140-2.
44. ^ Martin Pätzold and Olivier Witasse (March 4, 2010). "Phobos Flyby Success". ESA. Retrieved March 4, 2010.
45. ^ Craddock, R. A.; (1994); The Origin of Phobos and Deimos, Abstracts of the 25th Annual Lunar and Planetary Science Conference, held in Houston, TX, March 14–18, 1994, p. 293
46. ^ "Closest Phobos flyby gathers data". London. March 4, 2010. Retrieved March 7, 2010.
47. ^ "Projects LIFE Experiment: Phobos". The Planetary Society. Retrieved May 12, 2010.
48. ^ "Russia, China Could Sign Moon Exploration Pact in 2006". RIA Novosti. September 11, 2006. Retrieved May 12, 2010.
49. ^ "HK triumphs with out of this world invention". Hong Kong Trader. May 1, 2007. Retrieved May 12, 2010.
50. ^ "PolyU-made space tool sets for Mars again". Hong Kong Polytechnic University. 2 April 2007. Retrieved May 12, 2010.
51. ^ Amos, J.; Martian Moon ’Could be Key Test’, BBC News (February 9, 2007)
52. ^ Optech press release, "Canadian Mission Concept to Mysterious Mars moon Phobos to Feature Unique Rock-Dock Maneuver," May 3, 2007.
53. ^ PRIME: Phobos Reconnaissance & International Mars Exploration, Mars Institute website, accessed July 27, 2009.
54. ^ "Buzz Aldrin Reveals Existence of Monolith on Mars Moon". C-Span. July 22, 2009.
55. ^ Mullen, Leslie (April 30, 2009). "New Missions Target Mars Moon Phobos". Astrobiology Magazine ( Retrieved September 5, 2009.
56. ^ Landis, Geoffrey A. "Footsteps to Mars: an Incremental Approach to Mars Exploration," Journal of the British Interplanetary Society, Vol. 48, pp. 367-342 (1995); presented at Case for Mars V, Boulder CO, 26-May 29, 1993; appears in From Imagination to Reality: Mars Exploration Studies, R. Zubrin, ed., AAS Science and Technology Series Volume 91 pp. 339-350 (1997). (text available as Footsteps to Mars (PDF)

External links

* Phobos Profile at NASA's Solar System Exploration site
* HiRISE images of Phobos
* USGS Phobos nomenclature
* Asaph Hall and the Moons of Mars
* Flight around Phobos (movie)
* Animation of Phobos

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