Wikipedia

Phobos (moon)

This article is about the moon ofMars.For the god, seePhobos (mythology).For other uses, seePhobos.
"Mars I" redirects here. For the Soviet Mars probe, seeMars 1.For other uses, seeMars 1 (disambiguation).

Phobos(/ˈfoʊbəs/;systematic designation:Mars I) is the innermost and larger of the twonatural satellites of Mars,the other beingDeimos.The two moons were discovered in 1877 by American astronomerAsaph Hall.Phobos is named afterthe Greek god of fear and panic,who is the son ofAres(Mars) and twin brother ofDeimos.

Phobos
A false color image of Phobos, as captured by theMars Reconnaissance Orbiterin 2008
Discovery
Discovered byAsaph Hall
Discovery date18 August 1877
Designations
Designation
Mars I
Pronunciation/ˈfoʊbɒs/[1]or/ˈfoʊbəs/[2]
Named after
Φόβος
AdjectivesPhobian[3]/ˈfoʊbiən/[4]
Orbital characteristics
EpochJ2000
Periapsis9234.42 km[5]
Apoapsis9517.58 km[5]
9376 km[5](2.76 Mars radii/1.472 Earth radii)
Eccentricity0.0151[5]
0.31891023d
(7 h 39 m 12 s)[6]
2.138 km/s[5]
Inclination1.093° (to Mars's equator)
0.046° (to localLaplace plane)
26.04° (to theecliptic)
Satellite ofMars
Physical characteristics
Dimensions25.90 km × 22.60 km × 18.32 km
(±0.08 km × 0.08 km × 0.06 km)[7]
11.08±0.04 km[7]
1640±8 km2[7]
Volume5695±32 km3[7]
Mass1.060×1016kg[8]
1.861±0.011 g/cm3[7]
0.0057 m/s2[5]
(581.4μg)
11.39m/s
(41 km/h)[5]
Synchronous
Equatorial rotation velocity
11.0 km/h (6.8 mph) (at longest axis)
0°
Albedo0.071 ± 0.012 at 0.54 μm[9]
Temperature≈ 233K
11.8[10]

Phobos is a small, irregularly shaped object with amean radiusof 11 km (7 mi). It orbits 6,000 km (3,700 mi) from the Martian surface, closer to itsprimary bodythan any other knownnatural satelliteto a planet. It orbitsMarsmuch 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 and 15 minutes or less, and set in the east, twice eachMartian day.Phobos is one of the least reflective bodies in theSolar System,with analbedoof 0.071. Surface temperatures range from about −4 °C (25 °F) on the sunlit side to −112 °C (−170 °F) on the shadowed side. The notable surface feature is the largeimpact crater,Stickney,which takes up a substantial proportion of the moon's surface. The surface is also marked by many grooves, and there are numerous theories as to how these grooves were formed.

Images and models indicate that Phobos may be arubble pileheld together by a thincrustthat is being torn apart bytidalinteractions. Phobos gets closer to Mars by about 2 centimetres (0.79 in) per year.

Discovery

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Main article:History of the moons of Mars

Phobos was discovered by the American astronomerAsaph Hallon 18 August 1877 at theUnited States Naval ObservatoryinWashington, D.C.,at about 09:14Greenwich Mean Time.(Contemporary sources, using the pre-1925astronomical conventionthat began the day at noon,[11]give the time of discovery as 17 August at 16:06Washington mean time,meaning 18 August 04:06 in the modern convention.)[12][13][14]Hall had discoveredDeimos,Mars' other moon, a few days earlier.[15] The discoveries were made using the world's largestrefracting telescope,the 26-inch "Great Equatorial".[16]

The names, originally spelledPhobusandDeimusrespectively, were suggested by the British academicHenry Madan,a science master atEton College,who based them onGreek mythology,in whichPhobosis a companion to the god,Ares.[17][18]

Physical characteristics

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Phobos has dimensions of 26 by 23 by 18 kilometres (16 mi × 14 mi × 11 mi),[7]and retains too little mass to be rounded under its own gravity. Phobos does not have anatmospheredue to its low mass and low gravity.[19]It is one of the least reflective bodies in the Solar System, with an albedo of about 0.071.[20]Infrared spectra show that it has carbon-rich material found incarbonaceous chondrites,and its composition shows similarities to that of Mars' surface.[21]Phobos' density is too low to be solid rock, and it is known to have significantporosity.[22][23][24]These results led to the suggestion that Phobos might contain a substantial reservoir of ice. Spectral observations indicate that the surfaceregolithlayer lacks hydration,[25][26]but ice below the regolith is not ruled out.[27][28]Surface temperatures range from about −4 °C (25 °F) on the sunlit side to −112 °C (−170 °F) on the shadowed side.[29]

Unlike Deimos, Phobos is heavily cratered,[30]with one of the craters near the equator having a central peak despite the moon's small size.[31]The most prominent of these is the craterStickney,a large impact crater some 9 km (5.6 mi) in diameter, which takes up a substantial proportion of the moon's surface area. As withMimas' craterHerschel,the impact that created Stickney must have nearly shattered Phobos.[32]

(top) False color image of the impact craterStickneyimaged by theMars Reconnaissance Orbiterin March 2008; (bottom) Labeled Map of Phobos – Moon of Mars (U.S. Geological Survey)

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 theMars Expressspacecraft, however, revealed that the grooves are not 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 ascrater 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.[33]However, in November 2018, following further computational probability analysis, astronomers concluded that the many grooves on Phobos were caused by boulders, ejected from the asteroid impact that created Stickney crater. These boulders rolled in a predictable pattern on the surface of the moon.[34][35]

Faint dust rings produced by Phobos and Deimos have long been predicted but attempts to observe these rings have, to date, failed.[36]Recent images fromMars Global Surveyorindicate 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.[37]

The uniqueKaidun meteoritethat fell on aSovietmilitary base inYemenin 1980 has been hypothesized to be a piece of Phobos, but this couldn't be verified because little is known about the exact composition of Phobos.[38][39]

Shklovsky's "Hollow Phobos" hypothesis

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In the late 1950s and 1960s, the unusual orbital characteristics of Phobos led to speculations that it might be hollow.[40]Around 1958, Russian astrophysicistIosif Samuilovich Shklovsky,studying thesecularaccelerationof Phobos' orbital motion, suggested a "thin sheet metal" structure for Phobos, a suggestion which led to speculations that Phobos was of artificial origin.[41]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 centimetres (2.4 in) thick.[41][42]In a February 1960 letter to the journalAstronautics,[43]Fred Singer,then science advisor to U.S. PresidentDwight D. Eisenhower,said of Shklovsky's theory:

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.[43]

Subsequently, the systematic data errors that Singer predicted were found to exist, the claim was called into doubt,[44]and accurate measurements of the orbit available by 1969 showed that the discrepancy did not exist.[45]Singer's critique was justified when earlier studies were discovered to have used an overestimated value of 5 centimetres (2.0 in) per year for the rate of altitude loss, which was later revised to 1.8 centimetres (0.71 in) per year.[46]The secular acceleration is now attributed to tidal effects, which create drag on the moon and therefore cause it to spiral inward.[47]

The density of Phobos has now been directly measured by spacecraft to be 1.887 g/cm3(0.0682 lb/cu in).[48]Current observations are consistent with Phobos being arubble pile.[48]In addition, images obtained by theVikingprobesin the 1970s clearly showed a natural object, not an artificial one. Nevertheless, mapping by theMars Expressprobe 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.[49]The porosity of Phobos was calculated to be 30% ± 5%, or a quarter to a third being empty.[50]

Named geological features

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Geological features on Phobos are named afterastronomerswho studied Phobos and people and places fromJonathan Swift'sGulliver's Travels.[51]

Craters on Phobos

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A number of craters have been named, and are listed in the following map and table.[52]

Crater Coordinates Diameter
(km)		 Approval
Year		 Eponym Ref
Clustril 60°N91°W/ 60°N 91°W/60; -91(Clustril) 3.4 2006 Character inLilliputwho informedFlimnapthat his wife had visited Gulliver privately in Jonathan Swift's novelGulliver's Travels WGPSN
D'Arrest 39°S179°W/ 39°S 179°W/-39; -179(D'Arrest) 2.1 1973 Heinrich Louis d'Arrest;German/Danish astronomer (1822–1875) WGPSN
Drunlo 36°30′N92°00′W/ 36.5°N 92°W/36.5; -92(Drunlo) 4.2 2006 Character in Lilliput who informed Flimnap that his wife had visited Gulliver privately inGulliver's Travels WGPSN
Flimnap 60°N10°E/ 60°N 10°E/60; 10(Flimnap) 1.5 2006 Treasurer of Lilliput inGulliver's Travels WGPSN
Grildrig 81°N165°E/ 81°N 165°E/81; 165(Grildrig) 2.6 2006 Name given to Gulliver by the farmer's daughterGlumdalclitchin the giants' countryBrobdingnaginGulliver's Travels WGPSN
Gulliver 62°N163°W/ 62°N 163°W/62; -163(Gulliver) 5.5 2006 Lemuel Gulliver;surgeon captain and voyager inGulliver's Travels WGPSN
Hall 80°S150°E/ 80°S 150°E/-80; 150(Hall) 5.4 1973 Asaph Hall;American astronomer discoverer of Phobos and Deimos (1829–1907) WGPSN
Limtoc 11°S54°W/ 11°S 54°W/-11; -54(Limtoc) 2 2006 General in Lilliput who prepared articles of impeachment against Gulliver inGulliver's Travels WGPSN
Öpik 7°S63°E/ 7°S 63°E/-7; 63(Öpik) 2 2011 Ernst J. Öpik,Estonian astronomer (1893–1985) WGPSN
Reldresal 41°N39°W/ 41°N 39°W/41; -39(Reldresal) 2.9 2006 Secretary for Private Affairs in Lilliput; Gulliver's friend inGulliver's Travels WGPSN
Roche 53°N177°E/ 53°N 177°E/53; 177(Roche) 2.3 1973 Édouard Roche;French astronomer (1820–1883) WGPSN
Sharpless 27°30′S154°00′W/ 27.5°S 154°W/-27.5; -154(Sharpless) 1.8 1973 Bevan Sharpless;American astronomer (1904–1950) WGPSN
Shklovsky 24°N112°E/ 24°N 112°E/24; 112(Shklovsky) 2 2011 Iosif Shklovsky,Soviet astronomer (1916–1985) WGPSN
Skyresh 52°30′N40°00′E/ 52.5°N 40°E/52.5; 40(Skyresh) 1.5 2006 Skyresh Bolgolam; High Admiral of the Lilliput council who opposed Gulliver's plea for freedom and accused him of being a traitor inGulliver's Travels WGPSN
Stickney 1°N49°W/ 1°N 49°W/1; -49(Stickney) 9 1973 Angeline Stickney(1830–1892); wife of American astronomer Asaph Hall (above) WGPSN
Todd 9°S153°W/ 9°S 153°W/-9; -153(Todd) 2.6 1973 David Peck Todd;American astronomer (1855–1939) WGPSN
Wendell 1°S132°W/ 1°S 132°W/-1; -132(Wendell) 1.7 1973 Oliver Wendell;American astronomer (1845–1912) WGPSN

Other named features

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There is one namedregio,Laputa Regio,and one namedplanitia,Lagado Planitia;both are named after places inGulliver's Travels(the fictionalLaputa,a flying island, andLagado,imaginary capital of the fictional nationBalnibarbi).[53]The only named ridge on Phobos isKepler Dorsum,named after the astronomerJohannes Kepler.[54]

Orbital characteristics

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Orbits of Phobos andDeimos

Theorbital motionof Phobos has been intensively studied, making it "the best studiednatural satellitein the Solar System "in terms of orbits completed.[55]Its close orbit around Mars produces some unusual effects. With an altitude of 5,989 km (3,721 mi), Phobos orbits Mars below thesynchronous orbitradius, meaning that it moves around Mars faster than Mars itself rotates.[23]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 anequatorialorbit, it cannot be seen above the horizon fromlatitudesgreater than 70.4°. Its orbit is so low that itsangular 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; atzenith,it is 0.20°, one-third as wide as the fullMoonas seen fromEarth.By comparison, theSunhas 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'synodicperiod) to run their course, a mere 13 seconds longer than Phobos'sidereal period.

Solar transits

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Main article:Transit of Phobos from Mars
PhobostransitstheSun,as viewed by thePerseveranceroveron 2 April 2022

An observer situated on the Martian surface, in a position to observe Phobos, would see regulartransitsof Phobos across the Sun. Several of these transits have been photographed by the Mars RoverOpportunity.During the transits, Phobos casts a shadow on the surface of Mars; this event has been photographed by several spacecraft. Phobos is not large enough to cover the Sun's disk, and so cannot cause atotal eclipse.[56]

Predicted destruction

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Tidal decelerationis gradually decreasing the orbital radius of Phobos by approximately 2 m (6 ft 7 in) every 100 years,[57]and with decreasing orbital radius the likelihood of breakup due totidal forcesincreases, estimated in approximately 30–50 million years,[57][55]or about 43 million years in one study's estimate.[58]

Phobos' grooves were long thought to be fractures caused by the impact that formed the Stickney crater. Other modelling suggested since the 1970s support the idea that the grooves are more like "stretch marks" that occur when Phobos gets deformed by tidal forces, but in 2015 when the tidal forces were calculated and used in a new model, the stresses were too weak to fracture a solid moon of that size, unless Phobos is a rubble pile surrounded by a layer of powdery regolith about 100 m (330 ft) thick. Stress fractures calculated for this model line up with the grooves on Phobos. The model is supported with the discovery that some of the grooves are younger than others, implying that the process that produces the grooves is ongoing.[57][59][inconsistent]

Given Phobos' irregular shape and assuming that it is a pile of rubble (specifically aMohr–Coulomb body), it will eventually break up due to tidal forces when it reaches approximately 2.1 Mars radii.[60]When Phobos is broken up, it will form a planetary ring around Mars.[61]This predicted ring may last from 1 million to 100 million years. The fraction of the mass of Phobos that will form the ring depends on the unknown internal structure of Phobos. Loose, weakly bound material will form the ring. Components of Phobos with strong cohesion will escape tidal breakup and will enter the Martian atmosphere.[62]It is predicted that within 30 to 50 million years it will either collide with the planet or break up into aplanetary ring.[29]

Origin

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An illustration of main-belt asteroid capture hypothesis

The origin of the Martian moons has been disputed.[63]Phobos and Deimos both have much in common with carbonaceousC-type asteroids,withspectra,albedo,anddensityvery similar to those of C- or D-type asteroids.[64]Based on their similarity, one hypothesis is that both moons may be capturedmain-belt asteroids.[65][66]Both moons have very circular orbits which lie almost exactly in Mars'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,[67]although it is not clear that sufficient time is available for this to occur for Deimos.[63]Capture also requires dissipation of energy. The current Martian atmosphere is too thin to capture a Phobos-sized object by atmospheric braking.[63]Geoffrey A. Landishas pointed out that the capture could have occurred if the original body was abinary asteroidthat separated under tidal forces.[66][68]

Phobos could be a second-generation Solar System object thatcoalescedin orbit after Mars formed, rather than forming concurrently out of the same birth cloud as Mars.[69]

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 largeplanetesimal.[70]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' volume) is inconsistent with an asteroidal origin.[50]Observations of Phobos in thethermal infraredsuggest a composition containing mainlyphyllosilicates,which are well known from the surface of Mars. The spectra are distinct from those of all classes ofchondritemeteorites, again pointing away from an asteroidal origin.[71]Both sets of findings support an origin of Phobos from material ejected by an impact on Mars that reaccreted in Martian orbit,[72]similar to theprevailing theoryfor the origin of Earth's moon.

Some areas of the surface are reddish in color, while others are bluish. The hypothesis is that gravity pull from Mars makes the reddish regolith move over the surface, exposing relatively fresh, unweathered and bluish material from the moon, while the regolith covering it over time has been weathered due to exposure of solar radiation. Because the blue rock differs from known Martian rock, it could contradict the theory that the moon is formed from leftover planetary material after the impact of a large object.[73]

In February 2021, Amirhossein Bagheri (ETH Zurich), Amir Khan (ETH Zurich),Michael Efroimsky(US Naval Observatory) and their colleagues proposed a new hypothesis on the origin of the moons. By analyzing the seismic and orbital data fromMars InSight Missionand other missions, they proposed that the moons are born from disruption of a common parent body around 1 to 2.7 billion years ago. The common progenitor of Phobos and Deimos was most probably hit by another object and shattered to form both moons.[74]

Exploration

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Launched missions

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Phobos over Mars (ESAMars Express)

Phobos has been photographed in close-up by several spacecraft whose primary mission has been to photograph Mars. The first wasMariner 7in 1969, followed byMariner 9in 1971,Viking 1in 1977,Phobos 2in 1989[75]Mars Global Surveyorin 1998 and 2003,Mars Expressin 2004, 2008, 2010[76]and 2019, andMars Reconnaissance Orbiterin 2007 and 2008. On 25 August 2005, theSpiritrover,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, and was able to successfully photograph both Phobos and Deimos.[77]

The Soviet Union undertook thePhobos programwith two probes, both launched successfully in July 1988.Phobos 1was accidentally shut down by an erroneous command from ground control issued in September 1988 and lost while the craft was still en route.Phobos 2arrived at the Mars system in January 1989 and, after transmitting a small amount of data and imagery shortly before beginning its detailed examination of Phobos' surface, the probe abruptly ceased transmission due either to failure of the onboard computer or of the radio transmitter, already operating on backup power. Other Mars missions collected more data, but no dedicatedsample return missionhas been successfully performed.

TheRussian Space Agencylaunched a sample return mission to Phobos in November 2011, calledFobos-Grunt.The return capsule also included a life science experiment ofThe Planetary Society,calledLiving Interplanetary Flight Experiment,or LIFE.[78]A second contributor to this mission was theChina 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.[79][80]However, after achievingEarth orbit,theFobos–Gruntprobe failed to initiate subsequent burns that would have sent it to Mars. Attempts to recover the probe were unsuccessful and it crashed back to Earth in January 2012.[81]

On 1 July 2020, theMars orbiterof theIndian Space Research Organisationwas able to capture photos of the body from 4,200 km away.[82]

Missions considered

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In 1997 and 1998, theAladdinmission was selected as a finalist in the NASADiscovery 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).[83]These samples would be returned to Earth for study three years later.[84][85]The Principal Investigator was Dr.Carle PietersofBrown University.The total mission cost, including launch vehicle and operations was $247.7 million.[86]Ultimately, the mission chosen to fly wasMESSENGER,a probe to Mercury.[87]

In 2007, the European aerospace subsidiaryEADS Astriumwas reported to have been developing a mission to Phobos as atechnology demonstrator.Astrium was involved in developing aEuropean Space Agencyplan for a sample return mission to Mars, as part of the ESA'sAurora 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 anion 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.[88]

Proposed missions

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ThePhobos monolith(right of center) as taken by theMars Global Surveyor(MOC Image 55103, 1998)

In 2007, theCanadian Space Agencyfunded a study byOptechand theMars Institutefor an uncrewed mission to Phobos known asPhobos Reconnaissance and International Mars Exploration(PRIME). A proposed landing site for the PRIME spacecraft is at the "Phobos monolith",a prominent object near Stickney crater.[89][90][91]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.[92]

In 2008,NASA Glenn Research Centerbegan studying a Phobos and Deimos sample return mission that would use solar electric propulsion. The study gave rise to the "Hall" mission concept, aNew Frontiers-class mission under further study as of 2010.[93]

Another concept of a sample return mission from Phobos and Deimos isOSIRIS-REx II,which would use heritage technology from the firstOSIRIS-RExmission.[94]

As of January 2013, a newPhobos Surveyormission is currently under development by a collaboration ofStanford University,NASA'sJet Propulsion Laboratory,and theMassachusetts Institute of Technology.[95]The mission is currently in the testing phases, and the team at Stanford plans to launch the mission between 2023 and 2033.[95]

In March 2014, a Discovery class mission was proposed to place an orbiter in Mars orbit by 2021 to study Phobos and Deimos through a series of close flybys. The mission is calledPhobos And Deimos & Mars Environment(PADME).[96][97][98]Two other Phobos missions that were proposed for the Discovery 13 selection included a mission calledMerlin,which would flyby Deimos but actually orbit and land on Phobos, and another one isPandorawhich would orbit both Deimos and Phobos.[99]

TheJapanese Aerospace Exploration Agency(JAXA) unveiled on 9 June 2015 theMartian Moons Exploration(MMX), a sample return mission targeting Phobos.[100]MMX will land and collect samples from Phobos multiple times, along with conducting Deimos flyby observations and monitoring Mars' climate. By using acorersampling mechanism, the spacecraft aims to retrieve a minimum 10 g amount of samples.[101]NASA, ESA, DLR, andCNES[102]are also participating in the project, and will provide scientific instruments.[103][104]The U.S. will contribute the Neutron and Gamma-Ray Spectrometer (NGRS), and France the Near IR Spectrometer (NIRS4/MacrOmega).[101][105]Although the mission has been selected for implementation[106][107]and is now beyond proposal stage, formal project approval by JAXA has been postponed following theHitomimishap.[108]Development and testing of key components, including the sampler, is currently ongoing.[109]As of 2017,MMX is scheduled to be launched in 2026, and will return to Earth five years later.[101]

Russia plans to repeat Fobos-Grunt mission in the late 2020s, and the European Space Agency is assessing a sample-return mission for 2024 calledPhootprint.[110][111]

Human missions

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NASA concept of a human mission to Phobos

Phobos has been proposed as an early target for ahuman mission to Mars.Theteleoperationof robotic scouts on Mars by humans on Phobos could be conducted without significant time delay, andplanetary protectionconcerns in early Mars exploration might be addressed by such an approach.[112]

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 ofatmospheric entryand subsequent return to orbit without any support facilities, or would require the creation ofsupport facilities in-situ.A lander instead bound for Phobos could be based on equipment designed for lunar andasteroidlandings.[113]Furthermore, due to Phobos' very weak gravity, thedelta-vrequired to land on Phobos and return is only 80% of that required for a trip to and from the surface of the Moon.[114]

It has been proposed that the sands of Phobos could serve as a valuable material foraerobrakingduring a Mars landing. A relatively small amount of chemical fuel brought from Earth could be used to lift a large amount of sand from the surface of Phobos to a transfer orbit. This sand could be released in front of a spacecraft during the descent maneuver causing a densification of the atmosphere just in front of the spacecraft.[115][116]

While human exploration of Phobos could serve as a catalyst for the human exploration of Mars, it could be scientifically valuable in its own right.[117]

Space elevator base

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First discussed in fiction in 1956 by Fontenay,[118]Phobos has been proposed as a future site forspace elevatorconstruction. This would involve a pair of space elevators: one extending 6,000 km from the Mars-facing side to the edge of Mars' atmosphere, the other extending 6,000 km (3,700 mi) from the other side and away from Mars. A spacecraft launching from Mars' surface to the lower space elevator would only need a delta-v of 0.52 km/s (0.32 mi/s), as opposed to the over 3.6 km/s (2.2 mi/s) needed to launch to low Mars orbit. The spacecraft could be lifted up using electrical power and then released from the upper space elevator with a hyperbolic velocity of 2.6 km/s (1.6 mi/s), enough to reach Earth and a significant fraction of the velocity needed to reach theasteroid belt.The space elevators could also work in reverse to help spacecraft enter the Martian system. The great mass of Phobos means that any forces from space elevator operation would have minimal effect on its orbit. Additionally, materials from Phobos could be used for space industry.[119]

See also

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References

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