Jump to content

Galilean moons

This is a good article. Click here for more information.
From Wikipedia, the free encyclopedia
(Redirected from Galilean satellites)
Montage of Jupiter's four Galilean moons, in a composite image depicting part of Jupiter and their relative sizes (positions are illustrative, not actual). From top to bottom: Io, Europa, Ganymede, Callisto.
"Family portrait" of Jupiter and the Galilean moons captured by Juno

The Galilean moons (/ˌɡælɪˈleɪ.ən/),[1] or Galilean satellites, are the four largest moons of Jupiter: Io, Europa, Ganymede, and Callisto. They are the most readily visible Solar System objects after Saturn, the dimmest of the classical planets; though their closeness to bright Jupiter makes naked-eye observation very difficult, they are readily seen with common binoculars, even under night sky conditions of high light pollution. The invention of the telescope enabled the discovery of the moons in 1610. Through this, they became the first Solar System objects discovered since humans have started tracking the classical planets, and the first objects to be found to orbit any planet beyond Earth.

They are planetary-mass moons and among the largest objects in the Solar System. All four, along with Titan, Triton, and Earth's Moon, are larger than any of the Solar System's dwarf planets. The largest, Ganymede, is the largest moon in the Solar System and surpasses the planet Mercury in size (though not mass). Callisto is only slightly smaller than Mercury in size; the smaller ones, Io and Europa, are about the size of the Moon. The three inner moons — Io, Europa, and Ganymede — are in a 4:2:1 orbital resonance with each other. While the Galilean moons are spherical, all of Jupiter's remaining moons have irregular forms because they are too small for their self-gravitation to pull them into spheres.

The Galilean moons are named after Galileo Galilei, who observed them in either December 1609 or January 1610, and recognized them as satellites of Jupiter in March 1610;[2] they remained the only known moons of Jupiter until the discovery of the fifth largest moon of Jupiter Amalthea in 1892.[3] Galileo initially named his discovery the Cosmica Sidera ("Cosimo's stars") or Medicean Stars, but the names that eventually prevailed were chosen by Simon Marius. Marius discovered the moons independently at nearly the same time as Galileo, 8 January 1610, and gave them their present individual names, after mythological characters that Zeus seduced or abducted, which were suggested by Johannes Kepler in his Mundus Jovialis, published in 1614.[4] Their discovery showed the importance of the telescope as a tool for astronomers by proving that there were objects in space that cannot be seen by the naked eye. The discovery of celestial bodies orbiting something other than Earth dealt a serious blow to the then-accepted (among educated Europeans) Ptolemaic world system, a geocentric theory in which everything orbits around Earth.

History

[edit]

Discovery

[edit]
Galileo Galilei, the discoverer of the four moons

As a result of improvements that Galileo Galilei made to the telescope, with a magnifying capability of 20×,[5] he was able to see celestial bodies more distinctly than was previously possible. This allowed Galileo to observe in either December 1609 or January 1610 what came to be known as the Galilean moons.[6][7]

On 7 January 1610, Galileo wrote a letter containing the first mention of Jupiter's moons. At the time, he saw only three of them, and he believed them to be fixed stars near Jupiter. He continued to observe these celestial orbs from 8 January to 2 March 1610. In these observations, he discovered a fourth body, and also observed that the four were not fixed stars, but rather were orbiting Jupiter.[6]

Galileo's discovery proved the importance of the telescope as a tool for astronomers by showing that there were objects in space to be discovered that until then had remained unseen by the naked eye. More importantly, the discovery of celestial bodies orbiting something other than Earth dealt a blow to the then-accepted Ptolemaic world system, which held that Earth was at the center of the universe and all other celestial bodies revolved around it.[8] Galileo's 13 March 1610, Sidereus Nuncius (Starry Messenger), which announced celestial observations through his telescope, does not explicitly mention Copernican heliocentrism, a theory that placed the Sun at the center of the universe. Nevertheless, Galileo accepted the Copernican theory.[6]

A Chinese historian of astronomy, Xi Zezong, has claimed that a "small reddish star" observed near Jupiter in 364 BCE by Chinese astronomer Gan De may have been Ganymede. If true, this might predate Galileo's discovery by around two millennia.[9]

The observations of Simon Marius are another noted example of observation, and he later reported observing the moons in 1609.[10] However, because he did not publish these findings until after Galileo, there is a degree of uncertainty around his records.[10]

Names

[edit]
The Medician stars in the Sidereus Nuncius (the 'starry messenger'), 1610. The moons are drawn in changing positions.
A Jovilabe:[11] an apparatus from the mid-18th century for demonstrating the orbits of Jupiter's satellites

In 1605, Galileo had been employed as a mathematics tutor for Cosimo de' Medici. In 1609, Cosimo became Grand Duke Cosimo II of Tuscany. Galileo, seeking patronage from his now-wealthy former student and his powerful family, used the discovery of Jupiter's moons to gain it.[6] On 13 February 1610, Galileo wrote to the Grand Duke's secretary:

"God graced me with being able, through such a singular sign, to reveal to my Lord my devotion and the desire I have that his glorious name live as equal among the stars, and since it is up to me, the first discoverer, to name these new planets, I wish, in imitation of the great sages who placed the most excellent heroes of that age among the stars, to inscribe these with the name of the Most Serene Grand Duke."[6]

Galileo initially called his discovery the Cosmica Sidera ("Cosimo's stars"), in honour of Cosimo alone. [a] Cosimo's secretary suggested to change the name to Medicea Sidera ("the Medician stars"), honouring all four Medici brothers (Cosimo, Francesco, Carlo, and Lorenzo).[6] The discovery was announced in the Sidereus Nuncius ("Starry Messenger"), published in Venice in March 1610, less than two months after the first observations.

On 12 March 1610, Galileo wrote his dedicatory letter to the Duke of Tuscany, and the next day sent a copy to the Grand Duke, hoping to obtain the Grand Duke's support as quickly as possible. On 19 March, he sent the telescope he had used to first view Jupiter's moons to the Grand Duke, along with an official copy of Sidereus Nuncius (The Starry Messenger) that, following the secretary's advice, named the four moons the Medician Stars.[6] In his dedicatory introduction, Galileo wrote:

Scarcely have the immortal graces of your soul begun to shine forth on earth than bright stars offer themselves in the heavens which, like tongues, will speak of and celebrate your most excellent virtues for all time. Behold, therefore, four stars reserved for your illustrious name ... which ... make their journeys and orbits with a marvelous speed around the star of Jupiter ... like children of the same family ... Indeed, it appears the Maker of the Stars himself, by clear arguments, admonished me to call these new planets by the illustrious name of Your Highness before all others.[6]

Other names put forward include:

The names that eventually prevailed were chosen by Simon Marius, who discovered the moons independently at the same time as Galileo: he named them at the suggestion of Johannes Kepler after lovers of the god Zeus (the Greek equivalent of Jupiter), in his Mundus Jovialis, published in 1614:[13]

Jupiter is much blamed by the poets on account of his irregular loves. Three maidens are especially mentioned as having been clandestinely courted by Jupiter with success. Io, daughter of the River Inachus, Callisto of Lycaon, Europa of Agenor. 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... I think, therefore, that I shall not have done amiss if the First is called by me Io, the Second Europa, the Third, on account of its majesty of light, Ganymede, the Fourth Callisto... This fancy, and the particular names given, were suggested to me by Kepler, Imperial Astronomer, when we met at Ratisbon fair in October 1613. So if, as a jest, and in memory of our friendship then begun, I hail him as joint father of these four stars, again I shall not be doing wrong.

Galileo steadfastly refused to use Marius' names and invented as a result the numbering scheme that is still used nowadays, in parallel with proper moon names. The numbers run from Jupiter outward, thus I, II, III and IV for Io, Europa, Ganymede, and Callisto respectively.[14] Galileo used this system in his notebooks but never actually published it.[13] The numbered names (Jupiter x) were used until the mid-20th century when other inner moons were discovered, and Marius' names became widely used.[14]

  • The Galilean moons' namesakes
  • Io (left) watched by Argus Panoptes (right) on Hera's orders
    Io (left) watched by Argus Panoptes (right) on Hera's orders
  • Europa on the back of Zeus turned into a bull
    Europa on the back of Zeus turned into a bull
  • Ganymede (left) abducted by Zeus (right)
    Ganymede (left) abducted by Zeus (right)
  • Callisto (leftmost) with Eros and other nymphs, with Artemis seated
    Callisto (leftmost) with Eros and other nymphs, with Artemis seated

Determination of longitude

[edit]
Main article: History of longitude
Map of France presented in 1684, showing the outline of a previous map (Sanson, light outline) compared to the new survey by Cassini and Picard using the moons of Jupiter as timing reference (heavier, shaded outline). The King of France reportedly quipped that the astronomers had taken more territory from him than his enemies.[15]

Galileo's discovery had practical applications. Safe navigation required accurately determining a ship's position at sea. While latitude could be measured well enough by local astronomical observations, determining longitude required knowledge of the time of each observation synchronized to the time at a reference longitude. The longitude problem was so important that large prizes were offered for its solution at various times by Spain, Holland, and Britain.

Galileo proposed determining longitude based on the timing of the orbits of the Galilean moons.[16] The times of the eclipses of the moons could be precisely calculated in advance and compared with local observations on land or on ship to determine the local time and hence longitude. Galileo applied in 1616 for the Spanish prize of 6,000 gold ducats with a lifetime pension of 2,000 a year, and almost two decades later for the Dutch prize, but by then he was under house arrest for possible heresy.[17]: 15–16 

The main problem with the Jovian moon technique was that it was difficult to observe the Galilean moons through a telescope on a moving ship, a problem that Galileo tried to solve with the invention of the celatone. Others suggested improvements, but without success.[15]

Land mapping surveys had the same problem determining longitude, though with less severe observational conditions. The method proved practical and was used by Giovanni Domenico Cassini and Jean Picard to re-map France.[18]

Members

[edit]
Further information: Moons of Jupiter

Some models predict that there may have been several generations of Galilean satellites in Jupiter's early history. Each generation of moons to have formed would have spiraled into Jupiter and been destroyed, due to tidal interactions with Jupiter's proto-satellite disk, with new moons forming from the remaining debris. By the time the present generation formed, the gas in the proto-satellite disk had thinned out to the point that it no longer greatly interfered with the moons' orbits.[19][20]

Other models suggest that Galilean satellites formed in a proto-satellite disk, in which formation timescales were comparable to or shorter than orbital migration timescales.[21] Io is anhydrous and likely has an interior of rock and metal.[19] Europa is thought to contain 8% ice and water by mass with the remainder rock.[19] These moons are, in increasing order of distance from Jupiter:

Name
 Image Model of interior Diameter
(km) 		Mass
(kg) 		Density
(g/cm3) 		Semi-major axis
(km)[22] 		Orbital period (days)[23] (relative to Io) Inclination
(°)[24] 		Eccentricity
Io
Jupiter I 		3660.0
× 3637.4
× 3630.6 		8.93×1022 3.528 421800 1.769
(1) 		0.050 0.0041
Europa
Jupiter II 		3121.6 4.8×1022 3.014 671100 3.551
(2.0) 		0.471 0.0094
Ganymede
Jupiter III 		5268.2 1.48×1023 1.942 1070400 7.155
(4.0) 		0.204 0.0011
Callisto
Jupiter IV 		4820.6 1.08×1023 1.834 1882700 16.689
(9.4) 		0.205 0.0074

Io

[edit]
Main article: Io (moon)
Tupan Patera on Io

Io (Jupiter I) is the innermost of the four Galilean moons of Jupiter; with a diameter of 3642 kilometers, it is the fourth-largest moon in the Solar System, and is only marginally larger than Earth's moon. It was named after Io, a priestess of Hera who became one of the lovers of Zeus. It was referred to as "Jupiter I", or "The first satellite of Jupiter" until the mid-20th century.[14]

With over 400 active volcanos, Io is the most geologically active object in the Solar System.[25] Its surface is dotted with more than 100 mountains, some of which are taller than Earth's Mount Everest.[26] Unlike most satellites in the outer Solar System (which have a thick coating of ice), Io is primarily composed of silicate rock surrounding a molten iron or iron sulfide core.[27]

Although not proven, data from the Galileo orbiter indicates that Io might have its own magnetic field.[28] Io has an extremely thin atmosphere made up mostly of sulfur dioxide (SO2).[29] If a surface data or collection vessel were to land on Io in the future, it would have to be extremely tough (similar to the tank-like bodies of the Soviet Venera landers) to survive the radiation and magnetic fields that originate from Jupiter.[30]

Europa

[edit]
Main article: Europa (moon)
Closeup of Europan lineae

Europa (Jupiter II), the second of the four Galilean moons, is the second closest to Jupiter and the smallest at 3121.6 kilometers in diameter, which is slightly smaller than Earth's Moon. The name comes from a mythical Phoenician noblewoman, Europa, who was courted by Zeus and became the queen of Crete, though the name did not become widely used until the mid-20th century.[14]

It has a smooth and bright surface,[31] with a layer of water surrounding the mantle of the planet, thought to be 100 kilometers thick.[32] The smooth surface includes a layer of ice, while the bottom of the ice is theorized to be liquid water.[33] The apparent youth and smoothness of the surface have led to the hypothesis that a water ocean exists beneath it, which could conceivably serve as an abode for extraterrestrial life.[34] Heat energy from tidal flexing ensures that the ocean remains liquid and drives geological activity.[35] Life may exist in Europa's under-ice ocean. So far, there is no evidence that life exists on Europa, but the likely presence of liquid water has spurred calls to send a probe there.[36]

Recurring plume erupting from Europa.[37]

The prominent markings that criss-cross the moon seem to be mainly albedo features, which emphasize low topography. There are few craters on Europa because its surface is tectonically active and young.[38] Some theories suggest that Jupiter's gravity is causing these markings, as one side of Europa is constantly facing Jupiter. Volcanic water eruptions splitting the surface of Europa and even geysers have also been considered as causes. The reddish-brown color of the markings is theorized to be caused by sulfur, but because no data collection devices have been sent to Europa, scientists cannot yet confirm this.[39] Europa is primarily made of silicate rock and likely has an iron core. It has a tenuous atmosphere composed primarily of oxygen.[40]

Ganymede

[edit]
Main article: Ganymede (moon)
Ancient tectonic features on Ganymede

Ganymede (Jupiter III), the third Galilean moon, is named after the mythological Ganymede, cupbearer of the Greek gods and Zeus's beloved.[41] Ganymede is the largest natural satellite in the Solar System at 5262.4 kilometers in diameter, which makes it larger than the planet Mercury – although only at about half of its mass[42] since Ganymede is an icy world. It is the only satellite in the Solar System known to possess a magnetosphere, likely created through convection within the liquid iron core.[43]

Ganymede is composed primarily of silicate rock and water ice, and a salt-water ocean is believed to exist nearly 200 km below Ganymede's surface, sandwiched between layers of ice.[44] The metallic core of Ganymede suggests a greater heat at some time in its past than had previously been proposed. The surface is a mix of two types of terrain—highly cratered dark regions and younger, but still ancient, regions with a large array of grooves and ridges. Ganymede has a high number of craters, but many are gone or barely visible due to its icy crust forming over them. The satellite has a thin oxygen atmosphere that includes O, O2, and possibly O3 (ozone), and some atomic hydrogen.[45][46]

Callisto

[edit]
Main article: Callisto (moon)
Callisto's Valhalla impact crater in enhanced color as seen by Voyager

Callisto (Jupiter IV) is the fourth and last Galilean moon, and is the second-largest of the four, and at 4820.6 kilometers in diameter, it is the third largest moon in the Solar System, and barely smaller than Mercury, though only a third of the latter's mass. It is named after the Greek mythological nymph Callisto, a lover of Zeus who was a daughter of the Arkadian King Lykaon and a hunting companion of the goddess Artemis. The moon does not form part of the orbital resonance that affects three inner Galilean satellites and thus does not experience appreciable tidal heating.[47] Callisto is composed of approximately equal amounts of rock and ices, which makes it the least dense of the Galilean moons. It is one of the most heavily cratered satellites in the Solar System, and one major feature is a basin around 3000 km wide called Valhalla.[48]

Callisto is surrounded by an extremely thin atmosphere composed of carbon dioxide[49] and probably molecular oxygen.[50] Investigation revealed that Callisto may possibly have a subsurface ocean of liquid water at depths less than 300 kilometres.[51] The likely presence of an ocean within Callisto indicates that it can or could harbour life. However, this is less likely than on nearby Europa.[52] Callisto has long been considered the most suitable place for a human base for future exploration of the Jupiter system since it is furthest from the intense radiation of Jupiter's magnetic field.[53]

Comparative structure

[edit]
Surface features of the four members at different levels of zoom in each row
Jovian radiation
Moon rem/day
Io 3600[54]
Europa 540[54]
Ganymede 8[54]
Callisto 0.01[54]
Earth (Max) 0.07
Earth (Avg) 0.0007

Fluctuations in the orbits of the moons indicate that their mean density decreases with distance from Jupiter. Callisto, the outermost and least dense of the four, has a density intermediate between ice and rock whereas Io, the innermost and densest moon, has a density intermediate between rock and iron. Callisto has an ancient, heavily cratered and unaltered ice surface and the way it rotates indicates that its density is equally distributed, suggesting that it has no rocky or metallic core but consists of a homogeneous mix of rock and ice. This may well have been the original structure of all the moons. The rotation of the three inner moons, in contrast, indicates differentiation of their interiors with denser matter at the core and lighter matter above. They also reveal significant alteration of the surface. Ganymede reveals past tectonic movement of the ice surface which required partial melting of subsurface layers. Europa reveals more dynamic and recent movement of this nature, suggesting a thinner ice crust. Finally, Io, the innermost moon, has a sulfur surface, active volcanism and no sign of ice. All this evidence suggests that the nearer a moon is to Jupiter the hotter its interior. The current model is that the moons experience tidal heating as a result of the gravitational field of Jupiter in inverse proportion to the square of their distance from the giant planet. In all but Callisto this will have melted the interior ice, allowing rock and iron to sink to the interior and water to cover the surface. In Ganymede a thick and solid ice crust then formed. In warmer Europa a thinner more easily broken crust formed. In Io the heating is so extreme that all the rock has melted and water has long ago boiled out into space.

Size

[edit]
Galilean moons compared with moons of other planets (and with Earth; the scale is changed to 1 pixel = 94 km at this resolution).

Latest flyby

[edit]
Jupiter and Io
Io
Europa
Ganymede
Callisto
Jupiter and Galilean moons circa 2007, imaged by New Horizons during flyby. (greyscale colour)

Origin and evolution

[edit]
The relative masses of the Jovian moons. Those smaller than Europa are not visible at this scale, and combined would only be visible at 100× magnification.

Jupiter's regular satellites are believed to have formed from a circumplanetary disk, a ring of accreting gas and solid debris analogous to a protoplanetary disk.[55][56] They may be the remnants of a score of Galilean-mass satellites that formed early in Jupiter's history.[20][55]

Simulations suggest that, while the disk had a relatively high mass at any given moment, over time a substantial fraction (several tenths of a percent) of the mass of Jupiter captured from the Solar nebula was processed through it. However, the disk mass of only 2% that of Jupiter is required to explain the existing satellites.[55] Thus there may have been several generations of Galilean-mass satellites in Jupiter's early history. Each generation of moons would have spiraled into Jupiter, due to drag from the disk, with new moons then forming from the new debris captured from the Solar nebula.[55] By the time the present (possibly fifth) generation formed, the disk had thinned out to the point that it no longer greatly interfered with the moons' orbits.[20] The current Galilean moons were still affected, falling into and being partially protected by an orbital resonance which still exists for Io, Europa, and Ganymede. Ganymede's larger mass means that it would have migrated inward at a faster rate than Europa or Io.[55] Tidal dissipation in the Jovian system is still ongoing and Callisto will likely be captured into the resonance in about 1.5 billion years, creating a 1:2:4:8 chain.[57]

Visibility

[edit]

All four Galilean moons are bright enough to be viewed from Earth without a telescope, if only they could appear farther away from Jupiter. (They are, however, easily distinguished with even low-powered binoculars.) They have apparent magnitudes between 4.6 and 5.6 when Jupiter is in opposition with the Sun,[58] and are about one unit of magnitude dimmer when Jupiter is in conjunction. The main difficulty in observing the moons from Earth is their proximity to Jupiter, since they are obscured by its brightness.[59] The maximum angular separations of the moons are between 2 and 10 arcminutes from Jupiter,[60] which is close to the limit of human visual acuity. Ganymede and Callisto, at their maximum separation, are the likeliest targets for potential naked-eye observation.[61]

  • Jupiter and all of the Galilean moons as seen through a 25 cm (10 in) amateur telescope (Meade LX200).
    Jupiter and all of the Galilean moons as seen through a 25 cm (10 in) amateur telescope (Meade LX200).
  • Jupiter with the Galilean moons and the full Moon as seen around conjunction on 10 April 2017
    Jupiter with the Galilean moons and the full Moon as seen around conjunction on 10 April 2017
  • Small satellites visible against the vastness of the largest planet in the solar system
    Two Hubble Space Telescope views of a rare triple transit of Jupiter by Europa, Callisto and Io (24 January 2015)

Orbit animations

[edit]

GIF animations depicting the Galilean moon orbits and the resonance of Io, Europa, and Ganymede

The Laplace resonance of Io, Europa and Ganymede (conjunctions are highlighted by color changes)
The Galilean moons orbiting Jupiter
  Jupiter ·   Io ·   Europa ·   Ganymede ·   Callisto

See also

[edit]

Notes

[edit]
  1. ^ Cosimo is the Italian form of the Greek name Cosmas itself deriving from cosmos (whence the neuter plural adjective cosmica). Sidera is the plural form of the Latin noun sidus "star, constellation".

References

[edit]
  1. ^ "Galilean". Oxford English Dictionary (Online ed.). Oxford University Press. (Subscription or participating institution membership required.)
  2. ^ Drake, Stillman (1978). Galileo at Work: His Scientific Biography. Chicago: University of Chicago Press. ISBN 978-0-226-16226-3.
  3. ^ "In Depth | Amalthea". NASA Solar System Exploration. Archived from the original on 2019-08-25. Retrieved 2019-11-17.
  4. ^ Pasachoff, Jay M. (2015). "Simon Marius's Mundus Iovialis: 400th Anniversary in Galileo's Shadow". Journal for the History of Astronomy. 46 (2): 218–234. Bibcode:2015AAS...22521505P. doi:10.1177/0021828615585493. S2CID 120470649.
  5. ^ Van Helden, Albert (March 1974). "The Telescope in the Seventeenth Century". Isis. 65 (1): 38–58. doi:10.1086/351216. JSTOR 228880. S2CID 224838258.
  6. ^ a b c d e f g h Galilei, Galileo; Van Helden, Albert (1989). Sidereus Nuncius, or The Sidereal Messenger (in englat). Chicago: University of Chicago Press. pp. 14–16. ISBN 978-0-226-27902-2.{{cite book}}: CS1 maint: unrecognized language (link)
  7. ^ Galilei, Galileo (1610). The Starry Messenger. Venice. ISBN 978-0-374-37191-3. On the seventh day of January in this present date 1610....
  8. ^ "Satellites of Jupiter". The Galileo Project. Rice University. 1995. Archived from the original on 11 February 2012. Retrieved 9 August 2007.
  9. ^ Ze-zong, Xi (June 1981). "The sighting of Jupiter's satellite by Gan De 2000 years before Galileo". Chinese Astronomy and Astrophysics. 5 (2): 242–243. Bibcode:1981ChA&A...5..242X. doi:10.1016/0275-1062(81)90039-4.
  10. ^ a b "The Discovery of the Galilean Satellites". solarviews.com. Archived from the original on 2019-11-19. Retrieved 2019-11-17.
  11. ^ "Jovilabe". Museo Galileo. Archived from the original on 16 April 2015. Retrieved 15 April 2015.
  12. ^ Annuaire de l'Observatoire royal de Bruxelles. L'Académie royale des sciences, des lettres et des beaux-arts de Belgique. 1879. p. 263. Archived from the original on 2016-04-29. Retrieved 2016-03-03.
  13. ^ a b Van Helden, Albert (August 1994). "Naming the Satellites of Jupiter and Saturn" (PDF). The Newsletter of the Historical Astronomy Division of the American Astronomical Society (32). Retrieved 10 March 2023.
  14. ^ a b c d Marazzini, C. (2005). "The names of the satellites of Jupiter: from Galileo to Simon Marius". Lettere Italiana. 57 (3): 391–407.
  15. ^ a b "Solving Longitude: Jupiter's Moons". Royal Museums Greenwich. 16 October 2014.
  16. ^ Howse, Derek (1980). Greenwich time and the discovery of the longitude. Oxford ; New York: Oxford University Press. p. 12. ISBN 978-0-19-215948-9.
  17. ^ Danson, Edwin (2006). Weighing the World: The Quest to Measure the Earth. Oxford ; New York, N.Y: Oxford University Press. ISBN 978-0-19-518169-2.
  18. ^ Howse, Derek (1997). Greenwich Time and the Longitude. Philip Wilson. pp. 26, 31.
  19. ^ a b c Canup, Robin M.; Ward, William R. (2008-12-30). Origin of Europa and the Galilean Satellites. University of Arizona Press. p. 59. arXiv:0812.4995. Bibcode:2009euro.book...59C. ISBN 978-0-8165-2844-8.
  20. ^ a b c Chown, Marcus (7 March 2009). "Cannibalistic Jupiter ate its early moons". New Scientist. Archived from the original on 23 March 2009. Retrieved 18 March 2009.
  21. ^ d'Angelo, Gennaro; Podolak, Morris (2015). "Capture and Evolution of Planetesimals in Circumjovian Disks". The Astrophysical Journal. 806 (2): 203. arXiv:1504.04364. Bibcode:2015ApJ...806..203D. doi:10.1088/0004-637X/806/2/203. S2CID 119216797.
  22. ^ Computed using the IAU-MPC Satellites Ephemeris Service μ value
  23. ^ "Galilean Moons of Jupiter" (PDF). NASA.gov. Archived (PDF) from the original on 8 June 2017.
  24. ^ Computed from IAG Travaux 2001 Archived 2011-08-07 at the Wayback Machine.
  25. ^ Lopes, Rosaly M.C; Kamp, Lucas W; Smythe, William D; Mouginis-Mark, Peter; Kargel, Jeff; Radebaugh, Jani; Turtle, Elizabeth P; Perry, Jason; Williams, David A; Carlson, R.W; Douté, S.; the Galileo NIMS; SSI Teams (2004). "Lava lakes on Io: Observations of Io's volcanic activity from Galileo NIMS during the 2001 fly-bys". Icarus. 169 (1): 140–74. Bibcode:2004Icar..169..140L. doi:10.1016/j.icarus.2003.11.013.
  26. ^ Schenk, Paul; Hargitai, Henrik; Wilson, Ronda; McEwen, Alfred; Thomas, Peter (2001). "The mountains of Io: Global and geological perspectives from Voyager and Galileo". Journal of Geophysical Research: Planets. 106 (E12): 33201–22. Bibcode:2001JGR...10633201S. doi:10.1029/2000JE001408.
  27. ^ Anderson, J. D.; et al. (1996). "Galileo Gravity Results and the Internal Structure of Io". Science. 272 (5262): 709–712. Bibcode:1996Sci...272..709A. doi:10.1126/science.272.5262.709. PMID 8662566. S2CID 24373080.
  28. ^ Porco, C. C.; West, Robert A.; McEwen, Alfred; Del Genio, Anthony D.; Ingersoll, Andrew P.; Thomas, Peter; Squyres, Steve; Dones, Luke; Murray, Carl D.; Johnson, Torrence V.; Burns, Joseph A.; Brahic, Andre; Neukum, Gerhard; Veverka, Joseph; Barbara, John M.; Denk, Tilmann; Evans, Michael; Ferrier, Joseph J.; Geissler, Paul; Helfenstein, Paul; Roatsch, Thomas; Throop, Henry; Tiscareno, Matthew; Vasavada, Ashwin R. (2003). "Cassini Imaging of Jupiter's Atmosphere, Satellites, and Rings" (PDF). Science. 299 (5612): 1541–7. Bibcode:2003Sci...299.1541P. doi:10.1126/science.1079462. PMID 12624258. S2CID 20150275. Archived (PDF) from the original on 2017-09-22.
  29. ^ McEwen, A. S.; Keszthelyi, L.; Spencer, J. R.; Schubert, G.; Matson, D. L.; Lopes-Gautier, R.; Klaasen, K. P.; Johnson, T. V.; Head, J. W.; Geissler, P.; Fagents, S.; Davies, A. G.; Carr, M. H.; Breneman, H. H.; Belton, M. J. S. (1998). "High-Temperature Silicate Volcanism on Jupiter's Moon Io" (PDF). Science. 281 (5373): 87–90. Bibcode:1998Sci...281...87M. doi:10.1126/science.281.5373.87. PMID 9651251. S2CID 28222050. Archived from the original (PDF) on 2020-09-23.
  30. ^ Fanale, F. P.; Johnson, T. V.; Matson, D. L. (1974). "Io: A Surface Evaporite Deposit?". Science. 186 (4167): 922–5. Bibcode:1974Sci...186..922F. doi:10.1126/science.186.4167.922. PMID 17730914. S2CID 205532.
  31. ^ Hefler, Michael (2001). "Europa: In Depth". NASA, Solar system Exploration. NASA, Jet Propulsion Laboratory. Archived from the original on 14 November 2015. Retrieved 9 August 2007.
  32. ^ Schenk, Paul M.; Chapman, Clark R.; Zahnle, Kevin; Moore, Jeffrey M. (2004). "Ages and Interiors: the Cratering Record of the Galilean Satellites". In Bagenal, Fran; Dowling, Timothy E.; McKinnon, William B. (eds.). Jupiter: the planet, satellites, and magnetosphere (PDF). Cambridge planetary science. Cambridge, UK ; New York: Cambridge University Press. Bibcode:2004jpsm.book..427S. ISBN 978-0-521-81808-7.
  33. ^ Hamilton, C. J. "Jupiter's Moon Europa". Archived from the original on 2012-01-24.
  34. ^ Tritt, Charles S. (2002). "Possibility of Life on Europa". Milwaukee School of Engineering. Archived from the original on 9 June 2007. Retrieved 10 August 2007.
  35. ^ "Tidal Heating". geology.asu.edu. Archived from the original on 2006-03-29. Retrieved 2007-10-20.
  36. ^ Phillips, Cynthia (28 September 2006). "Time for Europa". Space.com. Archived from the original on 11 December 2011. Retrieved 5 January 2014.
  37. ^ "Hubble sees recurring plume erupting from Europa". www.spacetelescope.org. Archived from the original on 25 April 2017. Retrieved 24 April 2017.
  38. ^ Greenberg, Richard; Geissler, Paul; Hoppa, Gregory; Tufts, B.Randall; Durda, Daniel D.; Pappalardo, Robert; Head, James W.; Greeley, Ronald; Sullivan, Robert; Carr, Michael H. (1998). "Tectonic Processes on Europa: Tidal Stresses, Mechanical Response, and Visible Features" (PDF). Icarus. 135 (1): 64–78. Bibcode:1998Icar..135...64G. doi:10.1006/icar.1998.5986. S2CID 7444898. Archived from the original (PDF) on 2020-04-12.
  39. ^ Carlson, R.W.; M.S. Anderson (2005). "Distribution of hydrate on Europa: Further evidence for sulfuric acid hydrate". Icarus. 177 (2): 461–471. Bibcode:2005Icar..177..461C. doi:10.1016/j.icarus.2005.03.026.
  40. ^ "The moons of Jupiter". Archived from the original on 2020-02-26. Retrieved 2020-02-26.
  41. ^ "Satellites of Jupiter". The Galileo Project. Archived from the original on 2012-02-11. Retrieved 2007-11-24.
  42. ^ "Ganymede". nineplanets.org. October 31, 1997. Archived from the original on February 8, 2012. Retrieved 2008-02-27.
  43. ^ Kivelson, M.G.; Khurana, K.K.; Volwerk, M. (2002). "The Permanent and Inductive Magnetic Moments of Ganymede" (PDF). Icarus. 157 (2): 507–22. Bibcode:2002Icar..157..507K. doi:10.1006/icar.2002.6834. hdl:2060/20020044825. S2CID 7482644. Archived from the original (PDF) on 2020-04-12.
  44. ^ "Solar System's largest moon likely has a hidden ocean". Jet Propulsion Laboratory. NASA. 2000-12-16. Archived from the original on 2012-01-17. Retrieved 2008-01-11.
  45. ^ Hall, D. T.; Feldman, P. D.; McGrath, M. A.; Strobel, D. F. (1998). "The Far-Ultraviolet Oxygen Airglow of Europa and Ganymede". The Astrophysical Journal. 499 (1): 475–481. Bibcode:1998ApJ...499..475H. doi:10.1086/305604.
  46. ^ Eviatar, Aharon; m. Vasyliūnas, Vytenis; a. Gurnett, Donald (2001). "The ionosphere of Ganymede". Planetary and Space Science. 49 (3–4): 327–36. Bibcode:2001P&SS...49..327E. doi:10.1016/S0032-0633(00)00154-9.
  47. ^ Musotto, S; Varadi, Ferenc; Moore, William; Schubert, Gerald (2002). "Numerical Simulations of the Orbits of the Galilean Satellites". Icarus. 159 (2): 500–4. Bibcode:2002Icar..159..500M. doi:10.1006/icar.2002.6939.
  48. ^ "Galilean Satellites". Archived from the original on 2021-12-20. Retrieved 2022-02-20.
  49. ^ Carlson, R. W. (1999). "A Tenuous Carbon Dioxide Atmosphere on Jupiter's Moon Callisto" (PDF). Science. 283 (5403): 820–1. Bibcode:1999Sci...283..820C. CiteSeerX 10.1.1.620.9273. doi:10.1126/science.283.5403.820. hdl:2014/16785. PMID 9933159. Archived from the original (PDF) on 2008-10-03.
  50. ^ Liang, Mao-Chang; Lane, Benjamin F.; Pappalardo, Robert T.; Allen, Mark; Yung, Yuk L. (2005). "Atmosphere of Callisto" (PDF). Journal of Geophysical Research. 110 (E2): E02003. Bibcode:2005JGRE..110.2003L. doi:10.1029/2004JE002322. S2CID 8162816.
  51. ^ Zimmer, C; Khurana, Krishan K.; Kivelson, Margaret G. (2000). "Subsurface Oceans on Europa and Callisto: Constraints from Galileo Magnetometer Observations" (PDF). Icarus. 147 (2): 329–47. Bibcode:2000Icar..147..329Z. CiteSeerX 10.1.1.366.7700. doi:10.1006/icar.2000.6456. Archived (PDF) from the original on 2009-03-27.
  52. ^ Lipps, Jere H.; Delory, Gregory; Pitman, Joseph T.; Rieboldt, Sarah; et al. (Society of Photo-optical Instrumentation Engineers ; Geological Society of America) (November 2004). Hoover, Richard B.; Levin, Gilbert V.; Rozanov, A. I︠U︡ (eds.). Astrobiology of Jupiter's icy moons. SPIE proceedings series. Vol. 5555. Bellingham, Wash: SPIE. pp. 78–92. Bibcode:2004SPIE.5555...78L. doi:10.1117/12.560356. ISBN 978-0-8194-5493-5. OCLC 57077468. S2CID 140590649. {{cite book}}: |journal= ignored (help)
  53. ^ Trautman, Pat; Bethke, Kristen (2003). "Revolutionary Concepts for Human Outer Planet Exploration(HOPE)" (PDF). NASA. Archived from the original (PDF) on 2012-01-19.
  54. ^ a b c d Ringwald, Frederick A. (29 February 2000). "SPS 1020 (Introduction to Space Sciences)". California State University, Fresno. Archived from the original on 25 July 2008. Retrieved 5 January 2014.
  55. ^ a b c d e Canup, Robert M.; Ward, William R. (2009). "Origin of Europa and the Galilean Satellites". Europa. University of Arizona Press. pp. 59–83. ISBN 978-0-8165-2844-8.
  56. ^ Alibert, Y.; Mousis, O.; Benz, W. (2005). "Modeling the Jovian subnebula I. Thermodynamic conditions and migration of proto-satellites". Astronomy & Astrophysics. 439 (3): 1205–13. arXiv:astro-ph/0505367. Bibcode:2005A&A...439.1205A. doi:10.1051/0004-6361:20052841. S2CID 2260100.
  57. ^ Lari, Giacomo; Saillenfest, Melaine; Fenucci, Marco (2020). "Long-term evolution of the Galilean satellites: the capture of Callisto into resonance". Astronomy & Astrophysics. 639: A40. arXiv:2001.01106. Bibcode:2020A&A...639A..40L. doi:10.1051/0004-6361/202037445. S2CID 209862163. Retrieved 1 August 2022.
  58. ^ Yeomans, Donald K. (2006-07-13). "Planetary Satellite Physical Parameters". JPL Solar System Dynamics. Archived from the original on 2010-05-27. Retrieved 2008-08-23.
  59. ^ Jupiter is about 750 times brighter than Ganymede and about 2000 times brighter than Callisto.
    Ganymede: (5th root of 100)^(4.4 Ganymede APmag − (−2.8 Jup APmag)) = 758
    Callisto: (5th root of 100)^(5.5 Callisto APmag − (−2.8 Jup APmag)) = 2089
  60. ^ Jupiter near perihelion 2010-Sep-19: 656.7 (Callisto angular separation arcsec) − 24.9 (jup angular radius arcsec) = 631 arcsec = 10 arcmin
  61. ^ Dutton, Denis (December 1976). "Naked-Eye Observations of Jupiter's Moons". Sky & Telescope: 482–4. Archived from the original on 12 November 2020. Retrieved 1 August 2022.
[edit]
Wikimedia Commons has media related to Galilean moons.

Retrieved from "https://en.wikipedia.org/w/index.php?title=Galilean_moons&oldid=1258239589"