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Ganymede (moon)

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This article is about the natural satellite of Jupiter. For the asteroid, see 1036 Ganymed.
Ganymede
True-color image taken by the Galileo probe
True-color image taken by the Galileo probe
Discovery
Discovered byG. Galilei
S. Marius
Discovery dateJanuary 11, 1610
Designations
Jupiter III
AdjectivesGanymedian, Ganymedean
Orbital characteristics
Periapsis1 069 200 km[b]
Apoapsis1 071 600 km[a]
Mean orbit radius
1 070 400 km[1]
Eccentricity0.001 3[1]
7.154 552 96 d[1]
10.880 km/s
Inclination0.20° (to Jupiter's equator)[1]
Satellite ofJupiter
Physical characteristics
2634.1 ± 0.3 km (0.413 Earths)[2]
87.0 million km2 (0.171 Earths)[c]
Volume7.6 km3 (0.0704 Earths)[d]
Mass1.4819 kg (0.025 Earths)[2]
Mean density
1.936 g/cm3[2]
1.428 m/s2 (0.146 g)[e]
2.741 km/s[f]
synchronous
0–0.33°[3]
Albedo0.43 ± 0.02[4]
Surface temp. min mean max
K 70[5] 110[5] 152[6]
4.61 (opposition) [4]
Atmosphere
Surface pressure
trace
Composition by volumeoxygen[7]

Ganymede (Template:PronEng GAN-ə-meed, or as Greek Γανυμήδης) is a natural satellite of Jupiter and the largest natural satellite in the Solar System. Completing an orbit in a little more than seven days, it is the seventh satellite and third Galilean satellite from Jupiter.[8] Ganymede participates in a 1:2:4 orbital resonance with the satellites Europa and Io, respectively. It is larger in diameter than the planet Mercury but has only about half its mass.[9]

Ganymede is composed primarily of silicate rock and water ice. It is a fully differentiated body with an iron-rich, liquid core. A saltwater ocean is believed to exist nearly 200 km below Ganymede's surface, sandwiched between layers of ice.[10] Its surface comprises two main types of terrain. Dark regions, saturated with impact craters and dated to four billion years ago, cover about a third of the satellite. Lighter regions, crosscut by extensive grooves and ridges and only slightly less ancient, cover the remainder. The cause of the light terrain's disrupted geology is not fully known, but was likely the result of tectonic activity brought about by tidal heating.[2]

Ganymede is the only satellite in the Solar System known to possess a magnetosphere, likely created through convection within the liquid iron core.[11] The meager magnetosphere is buried within Jupiter's much larger magnetic field and connected to it through open field lines. The satellite has a thin oxygen atmosphere that includes O, O2, and possibly O3 (ozone).[7] Atomic hydrogen is a minor atmospheric constituent. Whether the satellite has an ionosphere to correspond to its atmosphere is unresolved.[12]

Ganymede's discovery is credited to Galileo Galilei, who observed it in 1610.[13] The satellite's name was soon suggested by astronomer Simon Marius, for the mythological Ganymede, cupbearer of the Greek gods and Zeus's beloved.[14] Beginning with Pioneer 10, spacecraft have been able to examine Ganymede closely.[15] The Voyager probes refined measurements of its size, while the Galileo craft discovered its underground ocean and magnetic field. The Jupiter Icy Moons Orbiter was meant to orbit Ganymede, but the NASA project was cancelled in 2005.[16]

Discovery and naming

On January 11, 1610, Galileo Galilei observed what he believed were three stars near Jupiter; the next night he noticed that they had moved. He found a fourth supposed star, which would turn out to be Ganymede, on January 11. By January 15, Galileo came to the conclusion that the stars were actually bodies orbiting Jupiter.[17] He claimed the right to name the moons; he considered "Cosmian Stars" and settled on "Medicean Stars".[14]

The French astronomer Nicolas-Claude Fabri de Peiresc suggested individual names from the Medici family for the moons, but his proposal was not taken up.[14] Simon Marius, who had originally claimed to have found the Galilean satellites,[18] tried to name the moons the "Saturn of Jupiter", the "Jupiter of Jupiter" (this was Ganymede), the "Venus of Jupiter", and the "Mercury of Jupiter", another nomenclature that never caught on. From a suggestion by Johannes Kepler, Marius once again tried to name the moons:[14]

…Then there was Ganymede, the handsome son of King Tros, whom Jupiter, having taken the form of an eagle, transported to heaven on his back, as poets fabulously tell … the Third, on account of its majesty of light, Ganymede …[17]

This name and those of the other Galilean satellites fell into disfavor for a considerable time, and were not in common use until the mid-20th century. In much of the earlier astronomical literature, Ganymede is referred to instead by its Roman numeral designation (a system introduced by Galileo) as Jupiter III or as the "third satellite of Jupiter". Following the discovery of moons of Saturn, a naming system based on that of Kepler and Marius was used for Jupiter’s moons.[14] Ganymede is the only Galilean moon of Jupiter named after a male figure.

Orbit and rotation

Ganymede orbits Jupiter at a distance of 1 070 400 km, third among the Galilean satellites,[8] and completes a revolution every seven days and three hours. Like most known moons, Ganymede is tidally locked, with one face always pointing toward the planet.[19] Its orbit is very slightly eccentric and inclined to the Jovian equator, with the eccentricity and inclination changing quasi-periodically due to solar and planetary gravitational perturbations on a timescale of centuries. The ranges of change are 0.0009–0.0022 and 0.05–0.32°, respectively.[20] These orbital variations cause the axial tilt (the angle between rotational and orbital axes) to vary between 0 and 0.33°.[3]

The Laplace resonances of Ganymede, Europa, and Io

Ganymede participates in orbital resonances with Europa and Io: for every orbit of Ganymede, Europa orbits twice and Io orbits four times.[20][21] The superior conjunction between Io and Europa always occurs when Io is at periapsis and Europa at apoapsis. The superior conjunction between Europa and Ganymede occurs when Europa is at periapsis.[20] The longitudes of the Io–Europa and Europa–Ganymede conjunctions change with the same rate, making the triple conjunctions possible. Such a complicated resonance is called the Laplace resonance.[22]

The current Laplace resonance is unable to pump the orbital eccentricity of Ganymede to a higher value.[22] The value of about 0.0013 is probably a remnant from a previous epoch, when such pumping was possible.[21] The ganymedian orbital eccentricity is somewhat puzzling; if it is not pumped now it should have decayed long ago due to the tidal dissipation in the interior of Ganymede.[22] This means that the last episode of the eccentricity excitation happened only several hundred million years ago.[22] Because the orbital eccentricity of Ganymede is relatively low—0.0015 on average[21]—the tidal heating of this moon is negligible now.[22] However, in the past Ganymede may have passed through one or more Laplace-like resonances[j] which were able to pump the orbital eccentricity to a value as high as 0.01–0.02.[2][22] This probably caused a significant tidal heating of the interior of Ganymede; the formation of the grooved terrain may be a result of one or more heating episodes.[2][22]

The origin of the Laplace resonance among Io, Europa, and Ganymede is not known. Two hypotheses exist: that it is primordial and has existed from the beginning of the Solar System;[23] or that it developed after the formation of the Solar System. A possible sequence of the events is as follows: Io raised tides on Jupiter, causing its orbit to expand until it encountered 2:1 resonance with Europa; after that the expansion continued, but some of the angular moment was transferred to Europa as the resonance caused its orbit to expand as well; the process continued until Europa encountered 2:1 resonance with Ganymede.[22] Eventually the drift rates of conjunctions between all three moons were synchronized and locked in the Laplace resonance.[22]

Physical characteristics

Composition

Interior of Ganymede

The average density of Ganymede, 1.936 g/cm3, suggests a composition of approximately equal parts rocky material and water, which is mainly in the form of ice.[2] The mass fraction of ices is between 46–50%, slightly lower than that in Callisto.[24] Some additional volatile ices such as ammonia may also be present.[24][25] The exact composition of Ganymede's rock is not known, but is probably close to the composition of L/LL type ordinary chondrites, which are characterized by less total iron, less metallic iron and more iron oxide than H chondrites. The weight ratio of iron to silicon is 1.05:1.27 in Ganymede, whereas the solar ratio is around 1.8.[24]

Ganymede's surface has an albedo of about 43%.[26] Water ice seems to be ubiquitous on the surface, with a mass fraction of 50–90%,[2] significantly more than in Ganymede as a whole. Near-infrared spectroscopy has revealed the presence of strong water ice absorption bands at wavelengths of 1.04, 1.25, 1.5, 2.0 and 3.0 μm.[26] The grooved terrain is brighter and has more icy composition than the dark terrain.[27] The analysis of high-resolution, near-infrared and UV spectra obtained by the Galileo spacecraft and from the ground has revealed various non-water materials: carbon dioxide, sulfur dioxide and, possibly, cyanogen, hydrogen sulfate and various organic compounds.[2][28] Galileo results have also shown magnesium sulfate (MgSO4) and, possibly, sodium sulfate (Na2SO4) on Ganymede's surface.[19][29] These salts may originate from the subsurface ocean.[29]

The ganymedian surface is asymmetric; the leading hemisphere—that facing the direction of the orbital motion[g]—is brighter than the trailing one.[26] This is similar to Europa, but the reverse is true on Callisto.[26] The trailing hemisphere of Ganymede appears to be enriched in sulfur dioxide.[30][31] The distribution of carbon dioxide does not demonstrate any hemispheric asymmetry, although it is not observed near the poles.[28][32] Impact craters on Ganymede (except one) do not show any enrichment in carbon dioxide, which also distinguishes it from Callisto. Ganymede's carbon dioxide levels were probably depleted in the past.[32]

Internal structure

A sharp boundary divides the dark Nicholson Regio from the bright Harpagia Sulcus.

Ganymede appears to be fully differentiated, consisting of an iron sulfide–iron core, silicate mantle and an outer ice mantle.[33][2] This model is supported by the low value of its dimensionless[h] moment of inertia—0.3105 ± 0.0028—which was measured during Galileo flybys.[33][2] In fact, Ganymede has the lowest moment of inertia among the solid solar system bodies. The existence of a liquid, iron-rich core provides a natural explanation for the intrinsic magnetic field of Ganymede detected by Galileo.[34] The convection in the liquid iron, which has high electrical conductivity, is the most reasonable model of magnetic field generation.[11]

The precise thicknesses of the different layers in the interior of Ganymede depend on the assumed composition of silicates (fraction of olivine and pyroxene) and amount of sulfur in the core.[24][33] The most probable values are 700–900 km for the core radius and 800–1000 km for the thickness of the outer ice mantle, with the remainder being made by the silicate mantle.[34][33][35][36] The density of the core is 5.5–6 g/cm3 and the silicate mantle is 3.4–3.6 g/cm3.[34][33][35][24] Some models of the magnetic field generation require the existence of a solid core made of pure iron inside the liquid Fe–FeS core—similar to the structure of the Earth's core. The radius of this core may be up to 500 km.[34] The temperature in the core of Ganymede is probably 1500–1700 K and pressure up to 100 kBar (10 Gpa).[33][34]

Surface features

See also: List of geological features on Ganymede
Voyager 2 image mosaic of Ganymede's anti-Jovian hemisphere. The ancient dark area of Galileo Regio lies at the upper right. It is separated from the smaller dark region of Marius Regio to its left by the brighter and younger band of Uruk Sulcus. Fresh ice ejected from the relatively recent Osiris Crater created the bright rays at the bottom.

The Ganymedian surface is a mix of two types of terrain: very old, highly cratered, dark regions and somewhat younger (but still ancient), lighter regions marked with an extensive array of grooves and ridges. The dark terrain, which comprises about one-third of the surface,[37] contains clays and organic materials that could indicate the composition of the impactors from which Jovian satellites accreted.[38]

The heating mechanism required for the formation of the grooved terrain on Ganymede is an unsolved problem in the planetary sciences. The modern view is that the grooved terrain is mainly tectonic in nature.[2] Cryovulcanism is thought to have played only a minor role, if any.[2] The forces that caused the strong stresses in the ganymedian ice lithosphere necessary to initiate the tectonic activity may be connected to the tidal heating events in the past, possibly caused when the satellite passed through unstable orbital resonances.[2][39] The tidal flexing of the ice may have heated the interior and strained the lithosphere, leading to the development of cracks and horst and graben faulting, which erased the old, dark terrain on 70% of the surface.[40][2] The formation of the grooved terrain may also be connected with the early core formation. During subsequent evolution deep, hot water plumes may have risen from the core to the surface, leading to the tectonic deformation of the lithosphere.[41] Radiogenic heating within the satellite is the most relevant current heat source, contributing, for instance, to thickness of the ocean. Research models have found that if the orbital eccentricity were an order of magnitude greater than current (as it may have been in the past), tidal heating would be a more substantial heat source than radiogenic heating.[42]

Fresh impact craters on the grooved terrain of Ganymede

Cratering is seen on both types of terrain, but is especially extensive on the dark terrain: it appears to be saturated with impact craters and has evolved largely through impact events.[2] The brighter, grooved terrain contains much fewer impact features, which have been only of a minor importance to its tectonic evolution.[2] The density of cratering indicates an age of 4 billion years for the dark terrain, similar to the highlands of the Moon, and a somewhat younger age for the grooved terrain (but how much younger is uncertain).[43] Ganymede may have experienced a period of heavy cratering 3.5 to 4 billion years ago similar to that of the Moon.[43] If true, the vast majority of impacts happened in that epoch, while the cratering rate has been much smaller since.[9] Craters both overlay and are crosscut by the groove systems, indicating that some of the grooves are quite ancient. Relatively young craters with rays of ejecta are also visible.[44][9] Ganymedian craters are flatter than those on the Moon and Mercury. This is probably due to the relatively weak nature of Ganymede's icy crust, which can (or could) flow and thereby soften the relief. Ancient craters whose relief has disappeared leave only a "ghost" of a crater known as a palimpsest.[9]

One significant feature on Ganymede is a dark plain named Galileo Regio, which contains a series of concentric grooves, or furrows, likely created during a period of geologic activity.[45] Another prominent feature on Ganymede are polar caps, likely composed of water frost. The frost extends to 40° latitude.[19] These polar caps were first seen by the Voyager spacecraft. Theories on the caps' formation include the migration of water to higher latitudes and bombardment by plasma of the ice. Data from Galileo suggests the latter is correct.[46]

Atmosphere and ionosphere

In 1972, a team of Indian, British and American astronomers working at Indonesia's Bosscha Observatory claimed that they had detected a thin atmosphere around the satellite during an occultation, when it and Jupiter passed in front of a star.[47] They estimated that the surface pressure was around 1 μBar (0.1 Pa).[47] However, in 1979 Voyager 1 observed an occultation of a star (κ Centauri) during its flyby of the planet, with differing results.[48] The occultation measurements were conducted in the far-ultraviolet spectrum with wavelength shorter than 200 nm; they were much more sensitive to the presence of gases than measurements in the visible spectrum in 1972. No atmosphere was revealed by the Voyager data. The upper limit on the surface particle number density was found to be 1.5 cm−3, which corresponds to a surface pressure of less than 2.5 μBar.[48] The latter value is almost five orders of magnitude less than that measured in 1972, indicating that the earlier interpretation was too optimistic.[48]

Despite the Voyager data, evidence for a tenuous oxygen atmosphere on Ganymede, very similar to the one found on Europa, was found by the Hubble Space Telescope (HST) in 1995.[7][49] HST actually observed airglow of atomic oxygen in the far-ultraviolet at the wavelengths 130.4 nm and 135.6 nm. Such an airglow is excited when molecular oxygen is dissociated by electron impacts,[7] evidence of a significant neutral atmosphere composed predominantly of O2 molecules. The surface number density probably lies in the 1.2–7 cm−3 range, corresponding to the surface pressure of 0.2–1.2 μBar.[7][i] These values are in agreement with the Voyager's upper limit set in 1981. The oxygen is not evidence of life; it is thought to be produced when water ice on Ganymede's surface is split into hydrogen and oxygen by radiation, with the hydrogen then being more rapidly lost due to its low atomic mass.[49] The airglow observed over Ganymede is not spatially homogeneous like that over Europa. HST observed two bright spots located in the northern and southern hemispheres, near ± 50° latitude, which is exactly the boundary between the open and closed field lines of the ganymedian magnetosphere (see below).[50] The bright spots are probably polar auroras, caused by plasma precipitation along the open field lines.[51]

False color temperature map of Ganymede

The existence of a neutral atmosphere implies that an ionosphere should exist, because oxygen molecules are ionized by the impacts of the energetic electrons coming from the magnetosphere[52] and by solar EUV radiation.[12] However, the nature of the ganymedian ionosphere is as controversial as the nature of the atmosphere. Some Galileo measurements found an elevated electron density near the moon, suggesting an ionosphere, while others failed to detect anything.[12] The electron density near the surface is estimated by different sources to lie in the range 400–2,500 cm−3.[12] As of 2008, the parameters of the ionosphere of Ganymede are not well constrained.

Additional evidence of the oxygen atmosphere comes from spectral detection of gases trapped in the ice at the surface of Ganymede. The detection of ozone (O3) bands was announced in 1996.[53] In 1997 spectroscopic analysis revealed the dimer (or diatomic) absorption features of the molecular oxygen. Such an absorption can arise only if the oxygen is in a dense phase. The best candidate is the molecular oxygen trapped in ice. The depth of the dimer absorption bands depends on latitude and longitude, rather than on surface albedo—they tend to decrease with increasing latitude on Ganymede, while the O3 shows an opposite effect.[54] Laboratory work has found that O2 would not cluster and bubble but dissolve in ice at Ganymede's relatively warm surface temperature of 100 K.[55]

A search for sodium in the atmosphere, just after such a finding on Europa, turned up nothing in 1997. Sodium is at least 13 times less abundant around Ganymede than around Europa, possibly because of a relative deficiency at the surface or because the magnetosphere fends off energetic particles.[56] Another minor constituent of the ganymedian atmosphere is atomic hydrogen. Hydrogen atoms were observed as far as 3,000 km from the surface of the moon. Their density on the surface is about 1.5 cm−3.[57]

Magnetosphere

Enhanced-color Galileo spacecraft image of Ganymede's trailing hemisphere[58]

The Galileo craft made six close flybys of Ganymede from 1995–2000 (G1, G2, G7, G8, G28 and G29)[11] and discovered that Ganymede has a permanent (intrinsic) magnetic moment independent of the Jovian magnetic field.[59] The value of the moment is about 1.3 T·m3,[11] which is three times larger than the magnetic moment of Mercury. The magnetic dipole is tilted with respect to the rotational axis of Ganymede by 176°, which means that it is directed against the Jovian magnetic moment.[11] Its north pole lies below the orbital plane. The dipole magnetic field created by this permanent moment has a strength of 719 ± 2 nT at the equator of the moon,[11] which should be compared with the Jovian magnetic field at the distance of Ganymede—about 120 nT.[59] The equatorial field of Ganymede is directed against the Jovian field, meaning reconnection is possible. The intrinsic field strength at the poles is two times that at the equator—1440 nT.[11]

The permanent magnetic moment carves a part of space around Ganymede, creating a tiny magnetosphere embedded inside that of Jupiter; it is the only moon in the Solar System known to possess the feature.[59] Its diameter is 4–5 RG (RG = 2,631.2 km).[60] The ganymedian magnetosphere has a region of closed field lines located below 30° latitude, where charged particles (electrons and ions) are trapped, creating a kind of radiation belt.[60] The main ion species in the magnetosphere is single ionized oxygen—O+[12]—which fits well with the tenuous oxygen atmosphere of the moon. In the polar cap regions, at latitudes higher than 30°, magnetic field lines are open, connecting Ganymede with Jupiter's ionosphere.[60] In these areas, the energetic (tens and hundreds of keV) electrons and ions have been detected,[52] which may be responsible for the auroras observed around the ganymedian poles.[50] In addition, heavy ions continuously precipitate on the polar surface of the moon, sputtering and darkening the ice.[52]

Magnetic field of the Jovian satellite Ganymede, which is embedded into the magnetosphere of Jupiter. Closed field lines are marked with green color.

The interaction between the ganymedian magnetosphere and Jovian plasma is in many respects similar to that of the solar wind and Earth's magnetosphere.[60][61] The plasma co-rotating with Jupiter impinges on the trailing side of the ganymedian magnetosphere much like the solar wind impinges on the Earth's magnetosphere. The main difference is the speed of plasma flow—supersonic in the case of Earth and subsonic in the case of Ganymede. Because of the subsonic flow, there is no bow shock off the trailing hemisphere of Ganymede.[61]

In addition to the intrinsic magnetic moment, Ganymede has an induced dipole magnetic field.[11] Its existence is connected with the variation of the Jovian magnetic field near the moon. The induced moment is directed radially to or from Jupiter following the direction of the varying part of the planetary magnetic field. The induced magnetic moment is an order of magnitude weaker than the intrinsic one. The field strength of the induced field at the magnetic equator is about 60 nT—half of that of the ambient Jovian field.[11] The induced magnetic field of Ganymede is similar to those of Callisto and Europa, indicating that this moon also has a subsurface water ocean with a high electrical conductivity.[11]

Given that Ganymede is completely differentiated and has a metallic core,[2][34] its intrinsic magnetic field is probably generated in a similar fashion to the Earth's: as a result of conducting material moving in the interior.[11][34] The magnetic field detected around Ganymede is likely to be caused by compositional convection in the core,[34] if the magnetic field is the product of dynamo action, or magnetoconvection.[11][62]

Despite the presence of an iron core, Ganymede's magnetosphere remains enigmatic, particularly given that similar bodies lack the feature.[2] Some research has suggested that, given its relatively small size, the core ought to have sufficiently cooled to the point where fluid motions and a magnetic field would not be sustained. One explanation is that the same orbital resonances proposed to have disrupted the surface also allowed the magnetic field to persist: with Ganymede's eccentricity pumped and tidal heating increased during such resonances, the mantle may have insulated the core, preventing it from cooling.[40] Another explanation is a remnant magnetization of silicate rocks in the mantle, which is possible if the satellite had a more significant dynamo-generated field in the past.[2]

Origin and evolution

Ganymede likely formed by an accretion in Jupiter’s subnebula, a disk of gas and dust surrounding Jupiter after its formation.[63] The accretion of Ganymede probably took about 10 000 years,[64] much shorter than the 100 000 years estimated for Callisto. The Jovian subnebula may have been relatively "gas-starved" when the Galilean satellites formed; this would have allowed for the lengthy accretion times required for Callisto.[63] In contrast Ganymede formed closer to Jupiter, where the subnebular was denser, which explains its shorter formation timescale.[64] This relatively fast formation prevented the escape of accretional heat, which led to ice melt and differentiation: the separation of the rocks and ice. The rocks settled to the center, forming the core. In this respect, Ganymede is different from Callisto, which failed to melt and differentiate early due to loss of the accretional heat during its slower formation.[65] This hypothesis explains why the two Jovian moons look so dissimilar, despite their similar mass and composition.[36][65]

After formation, the ganymedian core largely retained the heat accumulated during accretion and differentiation, only slowly releasing it to the ice mantle like a kind thermal battery.[65] The mantle, in turn, transported it to the surface by convection.[36] Soon the decay of radioactive elements within rocks further heated the core, causing increased differentiation: an inner, iron–iron sulfide core and a silicate mantle formed.[34][65] With this, Ganymede became a fully differentiated body. By comparison, the radioactive heating of undifferentiated Callisto caused convection in its icy interior, which effectively cooled it and prevented large-scale melting of ice and rapid differentiation.[66] The convective motions in Callisto have caused only a partial separation of rock and ice.[66] Today, Ganymede continues to cool slowly.[34] The heat being released from its core and silicate mantle enables the subsurface ocean to exist,[25] while the slow cooling of the liquid Fe–FeS core causes convection and supports magnetic field generation.[34] The current heat flux out of Ganymede is probably higher than that out of Callisto.[65]

Exploration

The Voyager spacecraft.

Several probes flying by or orbiting Jupiter have explored Ganymede in detail. The first probes to explore were Pioneer 10 and Pioneer 11,[15] neither of which returned much information about the satellite.[67] Voyager 1 and Voyager 2 were next, passing by Ganymede in 1979. They refined its size, revealing it was larger than Saturn's moon Titan, which was previously thought to have been bigger.[68] The grooved terrain was also seen.[69]

In 1995, the Galileo spacecraft entered orbit around Jupiter and between 1996 and 2000 made six close flybys to explore Ganymede.[19] These flybys are G1, G2, G7, G8, G28 and G29.[11] During the closest flyby—G2—Galileo passed just 264 km from the surface of Ganymede.[11] During a G1 flyby in 1996, the ganymedian magnetic field was discovered,[70] while the discovery of the ocean was announced in 2001.[19][11] Galileo transmitted a large number of spectral images and discovered several non-ice compounds on the surface of Ganymede.[28] The most recent spacecraft to explore Ganymede up close was New Horizons, which passed by in 2007 on its way to Pluto. New Horizons made topography and composition maps of Ganymede as it sped by.[71][72]

One proposal to orbit Ganymede was the Jupiter Icy Moons Orbiter. Nuclear fission would have been used to power the craft, which would have been able to study Ganymede in detail.[73] However, the mission was cancelled in 2005 because of budget cuts.[16] There is a proposal to send a dedicated mission to orbit Ganymede, tentatively called The Grandeur of Ganymede. If flown, the orbiter will stay in a low-altitude polar orbit around the moon for at least a year.[38]

See also

Notes

  1. ^ Apoapsis is derived from semimajor axis a and eccentricity e: .
  2. ^ Periapsis is derived from semimajor axis a and eccentricity e: .
  3. ^ Surface area derived from the radius r: .
  4. ^ Volume v derived from the radius r: .
  5. ^ Surface gravity derived from the mass m, the gravitational constant G and the radius r: .
  6. ^ Escape velocity derived from the mass m, the gravitational constant G and the radius r: .
  7. ^ Leading hemisphere is a hemisphere looking in the direction of the orbital motion, the trailing hemisphere looks in the reverse direction.
  8. ^ The dimensionless moment of inertia referred to is I/(mr²), where I is the Moment of Inertia, m the mass, and r the maximal radius. It is 0.4 for a homogenous spherical body, but less than 0.4 if density increases with depth.
  9. ^ The surface number density and pressure were calculated from the column densities reported in Hall, et al. 1998, assuming a scale height of 20 km and temperature 120 K.
  10. ^ Laplace-like resonance is similar to the current Laplace resonance among Galilean moons with the only difference that longitudes of the Io–Europa and Europa–Ganymede conjunctions change with rates, whose ratio is a rational number—not unity as in the case of the Laplace resonance

References

  1. ^ a b c d "Planetary Satellite Mean Orbital Parameters". Jet Propulsion Laboratory, California Institute of Technology.
  2. ^ a b c d e f g h i j k l m n o p q r s t Showman, Adam P. (1999). "The Galilean Satellites" (pdf). Science. 286: 77–84. doi:10.1126/science.286.5437.77. PMID 10506564. {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help)
  3. ^ a b Bills, Bruce G. (2005). "Free and forced obliquities of the Galilean satellites of Jupiter". Icarus. 175: 233–247. doi:10.1016/j.icarus.2004.10.028.
  4. ^ a b Yeomans, Donald K. (2006-07-13). "Planetary Satellite Physical Parameters". JPL Solar System Dynamics. Retrieved 2007-11-05.
  5. ^ a b Delitsky, Mona L. (1998). "Ice chemistry of Galilean satellites" (pdf). J.of Geophys. Res. 103 (E13): 31, 391–31, 403. doi:10.1029/1998JE900020. {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help)
  6. ^ Orton, G.S. (1996). "Galileo Photopolarimeter-radiometer observations of Jupiter and the Galilean Satellites". Science. 274: 389–391. doi:10.1126/science.274.5286.389. {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help)
  7. ^ a b c d e Hall, D.T. (1998). "The Far-Ultraviolet Oxygen Airglow of Europa and Ganymede". The Astrophysical Journal. 499: 475–481. doi:10.1086/305604. {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help)
  8. ^ a b "Jupiter's Moons". The Planetary Society. Retrieved 2007-12-07.
  9. ^ a b c d "Ganymede". nineplanets.org. October 31, 1997. Retrieved 2008-02-27.
  10. ^ "Solar System's largest moon likely has a hidden ocean". Jet Propulsion Laboratory. NASA. 2000-12-16. Retrieved 2008-01-11.
  11. ^ a b c d e f g h i j k l m n o Kivelson, M.G. (2002). "The Permanent and Inductive Magnetic Moments of Ganymede" (pdf). Icarus. 157: 507–522. doi:10.1006/icar.2002.6834. {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help)
  12. ^ a b c d e Eviatar, Aharon (2001). "The ionosphere of Ganymede" (ps). Plan.Space Sci. 49: 327–336. doi:10.1016/S0032-0633(00)00154-9. {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help) Cite error: The named reference "Eviatar2001" was defined multiple times with different content (see the help page).
  13. ^ "Sidereus Nuncius". Eastern Michigan University. Retrieved 2008-01-11.
  14. ^ a b c d e "Satellites of Jupiter". The Galileo Project. Retrieved 2007-11-24.
  15. ^ a b "Pioneer 11". Solar System Exploration. Retrieved 2008-01-06.
  16. ^ a b "Jupiter Icy Moons Orbiter Victim of Budget Cut". Planet Surveyor. Retrieved 2008-01-06.
  17. ^ a b "The Discovery of the Galilean Satellites". Views of the Solar System. Space Research Institute, Russian Academy of Sciences. Retrieved 2007-11-24.
  18. ^ "DISCOVERY". Cascadia Community College. Retrieved 2007-11-24.
  19. ^ a b c d e Miller, Ron (2005). The Grand Tour: A Traveler's Guide to the Solar System (3rd edition ed.). Thailand: Workman Publishing. pp. 108–114. ISBN 0-7611-3547-2. {{cite book}}: |edition= has extra text (help); Unknown parameter |coauthors= ignored (|author= suggested) (help); Unknown parameter |month= ignored (help)
  20. ^ a b c Musotto, Susanna (2002). "Numerical Simulations of the Orbits of the Galilean Satellites". Icarus. 159: 500–504. doi:10.1006/icar.2002.6939. {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help)
  21. ^ a b c "High Tide on Europa". SPACE.com. Retrieved 2007-12-07.
  22. ^ a b c d e f g h i Showman, Adam P. (1997). "Tidal Evolution into the Laplace Resonance and the Resurfacing of Ganymede" (pdf). Icarus. 127: 93–111. doi:10.1006/icar.1996.5669. {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help)
  23. ^ Peale, S.J. (2002). "A Primordial Origin of the Laplace Relation Among the Galilean Satellites". Science. 298: 593–597. doi:10.1126/science.1076557. PMID 12386333. {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help)
  24. ^ a b c d e Kuskov, O.L. (2005). "Internal structure of Europa and Callisto". Icarus. 177: 550–369. doi:10.1016/j.icarus.2005.04.014. {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help)
  25. ^ a b Spohn, T. (2003). "Oceans in the icy Galilean satellites of Jupiter?" (pdf). Icarus. 161: 456–467. doi:10.1016/S0019-1035(02)00048-9. {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help)
  26. ^ a b c d Calvin, Wendy M. (1995). "Spectra of the ice Galilean satellites from 0.2 to 5 µm: A compilation, new observations, and a recent summary". J.of Geophys. Res. 100: 19, 041–19, 048. doi:10.1029/94JE03349. {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help)
  27. ^ "Ganymede: the Giant Moon". Wayne RESA. Retrieved 2007-12-31.
  28. ^ a b c McCord, T.B. (1998). "Non-water-ice constituents in the surface material of the icy Galilelean satellites from Galileo near-infrared mapping spectrometer investigation". J. of Geophys. Res. 103 (E4): 8, 603–8, 626. doi:10.1029/98JE00788. {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help)
  29. ^ a b McCord, Thomas B. (2001). "Hydrated Salt Minerals on Ganymede's Surface: Evidence of an Ocean Below". Science. 292: 1523–1525. doi:10.1126/science.1059916. PMID 11375486. {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help)
  30. ^ Domingue, Deborah (1996). "Evidence from IUE for Spatial and Temporal Variations in the Surface Composition of the Icy Galilean Satellites". Bulletin of the American Astronomical Society. 28: 1070. {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help)
  31. ^ Domingue, Deborah L. (1998). "IEU's detection of tenuous SO2 frost on Ganymede and its rapid time variability". Geophys. Res. Lett. 25 (16): 3, 117–3, 120. doi:10.1029/98GL02386. {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help)
  32. ^ a b Hibbitts, C.A. (2003). "Carbon dioxide on Ganymede". J.of Geophys. Res. 108 (E5): 5, 036. doi:10.1029/2002JE001956. {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help)
  33. ^ a b c d e f Sohl, F. (2002). "Implications from Galileo Observations on the Interior Structure and Chemistry of the Galilean Satellites". Icarus. 157: 104–119. doi:10.1006/icar.2002.6828. {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help)
  34. ^ a b c d e f g h i j k Hauk, Steven A. (2006). "Sulfur's impact on core evolution and magnetic field generation on Ganymede" (pdf). J. of Geophys. Res. 111: E09008. doi:10.1029/2005JE002557. {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help)
  35. ^ a b Kuskov, O.L. (2005). "Internal Structure of Icy Satellites of Jupiter" (pdf). Geophysical Research Abstracts. 7. European Geosciences Union: 01892. {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help)
  36. ^ a b c Freeman, J. (2006). "Non-Newtonian stagnant lid convection and the thermal evolution of Ganymede and Callisto" (pdf). Planetary and Space Science. 54: 2–14. doi:10.1016/j.pss.2005.10.003.
  37. ^ Petterson, Wesley (2007). "A Global Geologic Map of Ganymede" (pdf). Lunar and Planetary Science. XXXVIII: 1098. {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help)
  38. ^ a b Pappalardo, R.T. (2001). "The Grandeur of Ganymede: Suggested Goals for an Orbiter Mission" (pdf). Lunar and Planetary Science. XXXII: 4062. {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help)
  39. ^ Showman, Adam P. (1997). "Coupled Orbital and Thermal Evolution of Ganymede" (pdf). Icarus. 129: 367–383. doi:10.1006/icar.1997.5778. {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help)
  40. ^ a b Bland (2007). "Ganymede's orbital and thermal evolution and its effect on magnetic field generation" (pdf). Lunar and Planetary Society Conference. 38: 2020. {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help); Unknown parameter |month= ignored (help)
  41. ^ Barr, A.C. (2001). "Rise of Deep Melt into Ganymede's Ocean and Implications for Astrobiology" (pdf). Lunar and Planetary Science Conference. 32: 1781. {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help)
  42. ^ Huffmann, H. (2004). "Internal Structure and Tidal Heating of Ganymede" (PDF). European Geosciences Union, Geophysical Research Abstracts. 6. {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help)
  43. ^ a b Zahnle, K. (1998). "Cratering Rates on the Galilean Satellites" (pdf). Icarus. 136: 202–222. doi:10.1006/icar.1998.6015. {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help)
  44. ^ "Ganymede". Lunar and Planetary Institute. 1997.
  45. ^ Casacchia, R. (1984). "Geologic evolution of Galileo Regio". Journal of Geophysical Research. 89: B419–B428. Bibcode:1984LPSC...14..419C. doi:10.1029/JB089iS02p0B419. {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help)
  46. ^ Khurana, Krishan K. (2007). "The origin of Ganymede's polar caps". Icarus. 191 (1): 193–202. doi:10.1016/j.icarus.2007.04.022. {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help)
  47. ^ a b Carlson, R.W. (1973). "Atmosphere of Ganymede from its occultation of SAO 186800 on 7 June 1972". Science. 53: 182. {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help)
  48. ^ a b c Broadfoot, A.L. (1981). "Overview of the Voyager Ultraviolet Spectrometry Results through Jupiter Encounter" (pdf). Science. 86: 8259–8284. {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help)
  49. ^ a b "Hubble Finds Thin Oxygen Atmosphere on Ganymede". Jet Propulsion Laboratory. NASA. 1996. Retrieved 2008-01-15. {{cite web}}: Unknown parameter |month= ignored (help)
  50. ^ a b Feldman, Paul D. (2000). "HST/STIS Ultraviolet Imaging of Polar Aurora on Ganymede". The Astrophysical Journal. 535: 1085–1090. doi:10.1086/308889. {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help)
  51. ^ Johnson, R.E. (1997). "Polar "Caps" on Ganymede and Io Revisited". Icarus. 128 (2): 469–471. doi:10.1006/icar.1997.5746.
  52. ^ a b c Paranicas, C. (1999). "Energetic particles observations near Ganymede". J.of Geophys.Res. 104 (A8): 17, 459–17, 469. doi:10.1029/1999JA900199. {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help)
  53. ^ Noll, Keith S. (1996). "Detection of Ozone on Ganymede". Science. 273 (5273): 341–343. doi:10.1126/science.273.5273.341. PMID 8662517. Retrieved 2008-01-13. {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help); Unknown parameter |month= ignored (help)
  54. ^ Calvin, Wendy M. (1997). "Latitudinal Distribution of O2on Ganymede: Observations with the Hubble Space Telescope". Icarus. 130 (2): 505–516. doi:10.1006/icar.1997.5842. {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help); Unknown parameter |month= ignored (help)
  55. ^ Vidal, R. A. (1997). "Oxygen on Ganymede: Laboratory Studies". Science. 276 (5320): 1839–1842. doi:10.1126/science.276.5320.1839. PMID 9188525. {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help)
  56. ^ Brown, Michael E. (1997). "A Search for a Sodium Atmosphere around Ganymede". Icarus. 126 (1): 236–238. doi:10.1006/icar.1996.5675.
  57. ^ Barth, C.A. (1997). "Galileo ultraviolet spectrometer observations of atomic hydrogen in the atmosphere of Ganymede". Geophys. Res. Lett. 24 (17): 2147–2150. doi:10.1029/97GL01927. {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help)
  58. ^ "Galileo has successful flyby of Ganymede during eclipse". Spaceflight Now. Retrieved 2008-01-19.
  59. ^ a b c Kivelson, M.G. (1997). "The magnetic field and magnetosphere of Ganymede" (pdf). Geophys. Res. Lett. 24 (17): 2155–2158. {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help)
  60. ^ a b c d Kivelson, M.G. (1998). "Ganymede's magnetosphere: magnetometer overview" (pdf). J.of Geophys. Res. 103 (E9): 19, 963–19, 972. doi:10.1029/98JE00227. {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help)
  61. ^ a b Volwerk, M. (1999). "Probing Ganymede's magnetosphere with field line resonances" (pdf). J.of Geophys. Res. 104 (A7): 14, 729–14, 738. doi:10.1029/1999JA900161. {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help)
  62. ^ Hauck, Steven A. (2002). "Internal structure and mechanism of core convection on Ganymede" (pdf). Lunar and Planetary Science. XXXIII: 1380.
  63. ^ a b Canup, Robin M. (2002). "Formation of the Galilean Satellites: Conditions of Accretion" (pdf). The Astronomical Journal. 124: 3404–3423. doi:10.1086/344684. {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help)
  64. ^ a b Mosqueira, Ignacio (2003). "Formation of the regular satellites of giant planets in an extended gaseous nebula I: subnebula model and accretion of satellites". Icarus. 163: 198–231. doi:10.1016/S0019-1035(03)00076-9. {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help)
  65. ^ a b c d e McKinnon, William B. (2006). "On convection in ice I shells of outer Solar System bodies, with detailed application to Callisto". Icarus. 183: 435–450. doi:10.1016/j.icarus.2006.03.004.
  66. ^ a b Nagel, K.A (2004). "A model for the interior structure, evolution, and differentiation of Callisto". Icarus. 169: 402–412. doi:10.1016/j.icarus.2003.12.019. {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help)
  67. ^ "Exploration of Ganymede". Terraformers Society of Canada. Retrieved 2008-01-06.
  68. ^ "Voyager 1 and 2". ThinkQuest. Retrieved 2008-01-06.
  69. ^ "The Voyager Planetary Mission". Views of the Solar System. Retrieved 2008-01-06.
  70. ^ "New Discoveries From Galileo". Jet Propulsion Laboratory. Retrieved 2008-01-06.
  71. ^ "Pluto-Bound New Horizons Spacecraft Gets A Boost From Jupiter". Space Daily. Retrieved 2008-01-06.
  72. ^ Grundy, W.M. (2007). "New Horizons Mapping of Europa and Ganymede". Science. 318: 234–237. doi:10.1126/science.1147623. PMID 17932288. {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help)
  73. ^ "Jupiter Icy Moons Orbiter (JIMO)". The Internet Encyclopedia of Science. Retrieved 2008-01-06.
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