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! Mass<br>(kg)
! Mass<br>(kg)
! Density<br>(g/cm³)
! Density<br>(g/cm³)
! <small>[[Semi-major axis]]<br>(km)<ref>Computed using the [http://www.minorplanetcenter.org/iau/NatSats/NaturalSatellites.html IAU-MPC Satellites Ephemeris Service] µ value</ref></small>
! <small>[[Semi-major axis]]<br>(km)<ref>Computed using the [http://www.minorplanetcenter.org/iau/NatSats/NaturalSatellites.html IAU-MPC Satellites Ephemeris Service]{{dead link|date=January 2017 |bot=InternetArchiveBot |fix-attempted=yes }} µ value</ref></small>
! <small>[[Orbital period]]([[Day|d]])<br><ref>Source: [http://sse.jpl.nasa.gov/planets/profile.cfm?Object=Jupiter&Display=Facts JPL/NASA]</ref> (relative)</small>
! <small>[[Orbital period]]([[Day|d]])<br><ref>Source: [http://sse.jpl.nasa.gov/planets/profile.cfm?Object=Jupiter&Display=Facts JPL/NASA]</ref> (relative)</small>
! [[Inclination]]<br>([[Degree (angle)|°]])<ref>Computed from [http://www.hnsky.org/iau-iag.htm IAG Travaux 2001].</ref>
! [[Inclination]]<br>([[Degree (angle)|°]])<ref>Computed from [http://www.hnsky.org/iau-iag.htm IAG Travaux 2001].</ref>
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Europa, 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 the [[Moon]]. The name comes from a mythical [[Phoenicia]]n noblewoman, [[Europa (mythology)|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.<ref name="marazzini"/>
Europa, 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 the [[Moon]]. The name comes from a mythical [[Phoenicia]]n noblewoman, [[Europa (mythology)|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.<ref name="marazzini"/>


It is one of the smoothest objects in the Solar System,<ref>{{cite web|url=http://www2.jpl.nasa.gov/galileo/moons/europa.html|title=Europa: Another Water World?|date=2001|accessdate=9 August 2007|publisher=[[NASA]], Jet Propulsion Laboratory|work=Project Galileo: Moons and Rings of Jupiter}}</ref> with a layer of water surrounding the mantle of the planet, thought to be 100 kilometers thick.<ref>Schenk, P. M.; Chapman, C. R.; Zahnle, K.; Moore, J. M.; ''Chapter 18: Ages and Interiors: the Cratering Record of the Galilean Satellites'', in ''Jupiter: The Planet, Satellites and Magnetosphere'', Cambridge University Press, 2004</ref> The smooth surface includes a layer of ice, while the bottom of the ice is theorized to be liquid water.<ref name="EuropaAlbedo">{{cite web|url=http://www.solarviews.com/eng/europa.htm|author=Hamilton, C. J.|title=Jupiter's Moon Europa}}</ref> 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]].<ref>{{cite web|url=http://people.msoe.edu/~tritt/sf/europa.life.html|title=Possibility of Life on Europa|last=Tritt|first=Charles S.|accessdate=10 August 2007|publisher=Milwaukee School of Engineering|date=2002}}</ref> Heat energy from [[tidal flexing]] ensures that the ocean remains liquid and drives geological activity.<ref name=geology>{{cite web| url=http://geology.asu.edu/~glg_intro/planetary/p8.htm |title=Tidal Heating|accessdate=2007-10-20|work=geology.asu.edu |archiveurl = https://web.archive.org/web/20060329000051/http://geology.asu.edu/~glg_intro/planetary/p8.htm |archivedate = 2006-03-29}}</ref> Life may exist in Europa's under-ice ocean, perhaps subsisting in an environment similar to Earth's deep-ocean [[hydrothermal vent]]s or the Antarctic [[Lake Vostok]].<ref>''[http://science.nasa.gov/newhome/headlines/ast10dec99_2.htm Exotic Microbes Discovered near Lake Vostok]'', Science@NASA (December 10, 1999)</ref> Life in such an ocean could possibly be similar to [[Microorganism|microbial]] life on Earth in the [[deep ocean]].<ref>Jones, N.; [http://www.newscientist.com/article.ns?id=dn1647 ''Bacterial explanation for Europa's rosy glow''], NewScientist.com (11 December 2001)</ref> 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.<ref>{{cite web|last=Phillips|first=Cynthia|url=http://www.space.com/2954-time-europa.html|title=Time for Europa|publisher=Space.com |date=28 September 2006 |deadurl=no |accessdate=5 January 2014}}</ref>
It is one of the smoothest objects in the Solar System,<ref>{{cite web|url=http://www2.jpl.nasa.gov/galileo/moons/europa.html|title=Europa: Another Water World?|date=2001|accessdate=9 August 2007|publisher=[[NASA]], Jet Propulsion Laboratory|work=Project Galileo: Moons and Rings of Jupiter}}</ref> with a layer of water surrounding the mantle of the planet, thought to be 100 kilometers thick.<ref>Schenk, P. M.; Chapman, C. R.; Zahnle, K.; Moore, J. M.; ''Chapter 18: Ages and Interiors: the Cratering Record of the Galilean Satellites'', in ''Jupiter: The Planet, Satellites and Magnetosphere'', Cambridge University Press, 2004</ref> The smooth surface includes a layer of ice, while the bottom of the ice is theorized to be liquid water.<ref name="EuropaAlbedo">{{cite web|url=http://www.solarviews.com/eng/europa.htm|author=Hamilton, C. J.|title=Jupiter's Moon Europa}}</ref> 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]].<ref>{{cite web|url=http://people.msoe.edu/~tritt/sf/europa.life.html |title=Possibility of Life on Europa |last=Tritt |first=Charles S. |accessdate=10 August 2007 |publisher=Milwaukee School of Engineering |date=2002 |deadurl=yes |archiveurl=https://web.archive.org/web/20070609150109/http://people.msoe.edu/~tritt/sf/europa.life.html |archivedate=9 June 2007 |df= }}</ref> Heat energy from [[tidal flexing]] ensures that the ocean remains liquid and drives geological activity.<ref name=geology>{{cite web| url=http://geology.asu.edu/~glg_intro/planetary/p8.htm |title=Tidal Heating|accessdate=2007-10-20|work=geology.asu.edu |archiveurl = https://web.archive.org/web/20060329000051/http://geology.asu.edu/~glg_intro/planetary/p8.htm |archivedate = 2006-03-29}}</ref> Life may exist in Europa's under-ice ocean, perhaps subsisting in an environment similar to Earth's deep-ocean [[hydrothermal vent]]s or the Antarctic [[Lake Vostok]].<ref>''[http://science.nasa.gov/newhome/headlines/ast10dec99_2.htm Exotic Microbes Discovered near Lake Vostok]'', Science@NASA (December 10, 1999)</ref> Life in such an ocean could possibly be similar to [[Microorganism|microbial]] life on Earth in the [[deep ocean]].<ref>Jones, N.; [http://www.newscientist.com/article.ns?id=dn1647 ''Bacterial explanation for Europa's rosy glow''], NewScientist.com (11 December 2001)</ref> 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.<ref>{{cite web|last=Phillips|first=Cynthia|url=http://www.space.com/2954-time-europa.html|title=Time for Europa|publisher=Space.com |date=28 September 2006 |deadurl=no |accessdate=5 January 2014}}</ref>


The prominent markings that criss-cross the moon seem to be mainly [[albedo feature]]s, which emphasize low topography. There are few [[Impact crater|craters]] on Europa because its surface is tectonically active and young.<ref>Arnett, B.; ''[http://www.astro.auth.gr/ANTIKATOPTRISMOI/nineplanets/nineplanets/europa.html Europa]'' (November 7, 1996)</ref> Some theories suggest that Jupiter's gravity is causing these markings, as one side of Europa is constantly facing Jupiter. Also, volcanic water eruptions splitting the surface of Europa, and even geysers have been considered as a cause. The color of the markings, reddish-brown, is theorized to be caused by sulfur, but scientists cannot confirm that, because no data collection devices have been sent to Europa.<ref>{{cite journal|title=Distribution of hydrate on Europa: Further evidence for sulfuric acid hydrate|doi=10.1016/j.icarus.2005.03.026|first1=R.W.|last1=Carlson|author2=M.S. Anderson |date=2005|bibcode=2005Icar..177..461C|volume=177|journal=Icarus|pages=461–471}}</ref> Europa is primarily made of [[silicate]] rock and likely has an [[iron]] core. It has a tenuous atmosphere composed primarily of [[oxygen]].
The prominent markings that criss-cross the moon seem to be mainly [[albedo feature]]s, which emphasize low topography. There are few [[Impact crater|craters]] on Europa because its surface is tectonically active and young.<ref>Arnett, B.; ''[http://www.astro.auth.gr/ANTIKATOPTRISMOI/nineplanets/nineplanets/europa.html Europa]'' (November 7, 1996)</ref> Some theories suggest that Jupiter's gravity is causing these markings, as one side of Europa is constantly facing Jupiter. Also, volcanic water eruptions splitting the surface of Europa, and even geysers have been considered as a cause. The color of the markings, reddish-brown, is theorized to be caused by sulfur, but scientists cannot confirm that, because no data collection devices have been sent to Europa.<ref>{{cite journal|title=Distribution of hydrate on Europa: Further evidence for sulfuric acid hydrate|doi=10.1016/j.icarus.2005.03.026|first1=R.W.|last1=Carlson|author2=M.S. Anderson |date=2005|bibcode=2005Icar..177..461C|volume=177|journal=Icarus|pages=461–471}}</ref> Europa is primarily made of [[silicate]] rock and likely has an [[iron]] core. It has a tenuous atmosphere composed primarily of [[oxygen]].
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! Moon !! [[Röntgen equivalent man|rem]]/day
! Moon !! [[Röntgen equivalent man|rem]]/day
|-
|-
| Io || 3600<ref name="ringwald">{{cite web |date=29 February 2000 |title=SPS 1020 (Introduction to Space Sciences)|publisher=California State University, Fresno|last=Ringwald|first=Frederick A.|url=http://zimmer.csufresno.edu/~fringwal/w08a.jup.txt |deadurl=no |accessdate=5 January 2014}}</ref>
| Io || 3600<ref name="ringwald">{{cite web|date=29 February 2000 |title=SPS 1020 (Introduction to Space Sciences) |publisher=California State University, Fresno |last=Ringwald |first=Frederick A. |url=http://zimmer.csufresno.edu/~fringwal/w08a.jup.txt |deadurl=yes |accessdate=5 January 2014 |archiveurl=http://www.webcitation.org/5jwBSgPuV?url=http%3A%2F%2Fzimmer.csufresno.edu%2F%7Efringwal%2Fw08a.jup.txt |archivedate=20 September 2009 |df= }}</ref>
|-
|-
| Europa || 540<ref name="ringwald"/>
| Europa || 540<ref name="ringwald"/>

Revision as of 11:05, 7 January 2017

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.

The Galilean moons are the four largest moons of Jupiter—Io, Europa, Ganymede, and Callisto. They were discovered by Galileo Galilei around January 1610 and were the first group of objects found to orbit another planet. Their names derive from the lovers of Zeus. They are among the largest objects in the Solar System with the exception of the Sun and the eight planets, with radii larger than any of the dwarf planets. Ganymede is the largest moon in the Solar System, and is even bigger than the planet Mercury. The three inner moons—Io, Europa, and Ganymede—are in a 4:2:1 orbital resonance with each other.

The Galilean moons were discovered in either 1609 or 1610 when Galileo made improvements to his telescope, which enabled him to observe celestial bodies more distinctly than ever.[1] Galileo's 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. More importantly, the incontrovertible discovery of celestial bodies orbiting something other than Earth dealt a serious blow to the then-accepted Ptolemaic world system, or the geocentric theory in which everything orbits around Earth.

Galileo initially named his discovery the Cosmica Sidera ("Cosimo's stars"), but the names that eventually prevailed were chosen by Simon Marius. Marius discovered the moons independently at the same time as Galileo, and gave them their present names, which were suggested by Johannes Kepler, in his Mundus Jovialis, published in 1614.[2]

History

Discovery

Galileo Galilei, the discoverer of the four moons

As a result of improvements Galileo Galilei made to the telescope, with a magnifying capability of 20×,[3] he was able to see celestial bodies more distinctly than was ever possible before. This allowed Galilei to discover in either December 1609 or January 1610 what came to be known as the Galilean moons.[1][4]

On January 7, 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 January 8 to March 2, 1610. In these observations, he discovered a fourth body, and also observed that the four were not fixed stars, but rather were orbiting Jupiter.[1]

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.[5] Galileo's 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.[1]

A Chinese historian of astronomy, Xi Zezong, has claimed that a "small reddish star" observed near Jupiter in 362 BCE by Chinese astronomer Gan De may have been Ganymede, predating Galileo's discovery by around two millennia.[6]

Dedication to the Medicis

The Medician stars in the Sidereus Nuncius (the 'starry messenger'), 1610. The moons are drawn in changing positions.

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.[1] On February 13, 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."[1]

Galileo asked whether he should name the moons the "Cosmian Stars", after Cosimo alone, or the "Medician Stars", which would honor all four brothers in the Medici clan. The secretary replied that the latter name would be best.[1]

On March 12, 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 March 19, 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.[1] 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.[1]

Name

A Jovilabe:[7] an apparatus from the mid-18th century for demonstrating the orbits of Jupiter's satellites

Galileo initially called his discovery the Cosmica Sidera ("Cosimo's stars"), in honour of Cosimo II de' Medici (1590–1621).[8] At Cosimo's suggestion, Galileo changed the name to Medicea Sidera ("the Medician stars"), honouring all four Medici brothers (Cosimo, Francesco, Carlo, and Lorenzo). The discovery was announced in the Sidereus Nuncius ("Starry Messenger"), published in Venice in March 1610, less than two months after the first observations.

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): Io, Europa, Ganymede and Callisto, in his Mundus Jovialis, published in 1614.[10]

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.[10] Galileo used this system in his notebooks but never actually published it. The numbered names (Jupiter x) were used until the mid-20th century when other inner moons were discovered, and Marius' names became widely used.[10]

Determination of longitude

See also: History of longitude

Galileo was able to develop a method of determining longitude based on the timing of the orbits of the Galilean moons.[11] 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. The main problem with the 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. The method was used by Cassini and Picard to re-map France.[12]

Members

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.[13][14] 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.[15] Io is anhydrous and likely has an interior of rock and metal.[13] Europa is thought to contain 8% ice and water by mass with the remainder rock.[13] These moons are, in increasing order of distance from Jupiter:

Name
 Image Model of interior
I E G C 		Diameter
(km) 		Mass
(kg) 		Density
(g/cm³) 		Semi-major axis
(km)[16] 		Orbital period(d)
[17] (relative) 		Inclination
(°)[18] 		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) 		0.471 0.0094
Ganymede
Jupiter III 		5262.4 1.48×1023 1.942 1070400 7.155

(4) 		0.204 0.0011
Callisto
Jupiter IV 		4820.6 1.08×1023 1.834 1882700 16.69

(9.4) 		0.205 0.0074

Io

Main article: Io (moon)
The three inner Galilean moons revolve in a 1:2:4 resonance.

Io is the innermost of the four Galilean moons of Jupiter and, with a diameter of 3,642 kilometers, the fourth-largest moon in the Solar System. It was named after Io, a priestess of Hera who became one of the lovers of Zeus. Nevertheless, it was simply referred to as "Jupiter I", or "The first satellite of Jupiter", until the mid-20th century.[10]

With over 400 active volcanos, Io is the most geologically active object in the Solar System.[19] Its surface is dotted with more than 100 mountains, some of which are taller than Earth's Mount Everest.[20] 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.

Although not proven, recent data from the Galileo orbiter indicate that Io might have its own magnetic field.[21] Io has an extremely thin atmosphere made up mostly of sulfur dioxide (SO2).[22] 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.[23]

Europa

Main article: Europa (moon)
Two Hubble Space Telescope views of a rare triple transit of Jupiter by Europa, Callisto and Io (24 January 2015).

Europa, 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 the 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.[10]

It is one of the smoothest objects in the Solar System,[24] with a layer of water surrounding the mantle of the planet, thought to be 100 kilometers thick.[25] The smooth surface includes a layer of ice, while the bottom of the ice is theorized to be liquid water.[26] 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.[27] Heat energy from tidal flexing ensures that the ocean remains liquid and drives geological activity.[28] Life may exist in Europa's under-ice ocean, perhaps subsisting in an environment similar to Earth's deep-ocean hydrothermal vents or the Antarctic Lake Vostok.[29] Life in such an ocean could possibly be similar to microbial life on Earth in the deep ocean.[30] 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.[31]

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.[32] Some theories suggest that Jupiter's gravity is causing these markings, as one side of Europa is constantly facing Jupiter. Also, volcanic water eruptions splitting the surface of Europa, and even geysers have been considered as a cause. The color of the markings, reddish-brown, is theorized to be caused by sulfur, but scientists cannot confirm that, because no data collection devices have been sent to Europa.[33] Europa is primarily made of silicate rock and likely has an iron core. It has a tenuous atmosphere composed primarily of oxygen.

Ganymede

Main article: Ganymede (moon)

Ganymede, the third Galilean moon is named after the mythological Ganymede, cupbearer of the Greek gods and Zeus's beloved.[34] 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[35] 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.[36]

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.[37] 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.[38][39]

Relative masses of the Jovian moons. Io and Callisto together are about 50%, as are Europa and Ganymede. The Galileans so dominate the system that all the other Jovian moons put together are not visible at this scale.

Callisto

Main article: Callisto (moon)

Callisto 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. Callisto was a daughter of the Arkadian King Lykaon and a hunting companion of the goddess Artemis. It does not form part of the orbital resonance that affects three inner Galilean satellites and thus does not experience appreciable tidal heating.[40] 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.

Callisto is surrounded by an extremely thin atmosphere composed of carbon dioxide[41] and probably molecular oxygen.[42] Investigation revealed that Callisto may possibly have a subsurface ocean of liquid water at depths greater than 100 kilometers.[43] The likely presence of an ocean within Callisto indicates that it can or could harbor life. However, this is less likely than on nearby Europa.[44] 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.[45]

Comparative structure

Comparison of (a part of) Jupiter and its four largest natural satellites
Jovian Radiation
Moon rem/day
Io 3600[46]
Europa 540[46]
Ganymede 8[46]
Callisto 0.01[46]

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.

Surface features of the four members at different levels of zoom in each row

Size

Galilean moons compared with other Solar System bodies, although pixel scale is not accurate at this resolution.

Latest flyby

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

Origin and evolution

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.[47][48] They may be the remnants of a score of Galilean-mass satellites that formed early in Jupiter's history.[14][47]

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.

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.[47] 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.[47] 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.[14] 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.[47]

Visibility

The Galilean moons seen with an amateur telescope.

All four Galilean moons are bright enough that they could be sighted from Earth without a telescope, if they were farther away from Jupiter. (They are, however, easily visible with even low-powered binoculars.) They have apparent magnitudes between 4.6 and 5.6 when Jupiter is in opposition with the Sun,[49] 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.[50] The maximum angular separations of the moons are between 2 and 10 minutes of arc from Jupiter,[51] 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.

See also

References

  1. ^ a b c d e f g h i Galilei, Galileo, Sidereus Nuncius. Translated and prefaced by Albert Van Helden. Chicago & London: University of Chicago Press 1989, 14–16
  2. ^ 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.
  3. ^ Van Helden, Albert (March 1974). "The Telescope in the Seventeenth Century". Isis. 65 (1). The University of Chicago Press on behalf of The History of Science Society: 38–58. doi:10.1086/351216. JSTOR 228880.
  4. ^ Galilei, Galileo (1610). The Starry Messenger (PDF). Venice. ISBN 0-374-37191-1. On the seventh day of January in this present date 1610....
  5. ^ "Satellites of Jupiter". The Galileo Project. Rice University. 1995. Retrieved 9 August 2007.
  6. ^ Zezong, Xi, "The Discovery of Jupiter's Satellite Made by Gan De 2000 years Before Galileo", Chinese Physics 2 (3) (1982): 664–67.
  7. ^ "Jovilabe". Museo Galileo. Retrieved 15 April 2015.
  8. ^ 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".
  9. ^ Annuaire de l'Observatoire royal de Bruxelles – Google Boeken. Books.google.com. Retrieved 11 November 2013.
  10. ^ a b c d e Marazzini, C. (2005). "The names of the satellites of Jupiter: from Galileo to Simon Marius". Lettere Italiana. 57 (3): 391–407.
  11. ^ Howse, Derek. Greenwich Time and the Discovery of the Longitude. Oxford: Oxford University Press, 1980, 12.
  12. ^ Howse, Derek (1997). Greenwich Time and the Longitude. Philip Wilson. pp. 26, 31.
  13. ^ 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.
  14. ^ a b c Chown, Marcus (7 March 2009). "Cannibalistic Jupiter ate its early moons". New Scientist. Retrieved 18 March 2009.
  15. ^ D'Angelo, G.; Podolak, M. (2015). "Capture and Evolution of Planetesimals in Circumjovian Disks". The Astrophysical Journal. 806 (1): 29pp. arXiv:1504.04364. Bibcode:2015ApJ...806..203D. doi:10.1088/0004-637X/806/2/203.
  16. ^ Computed using the IAU-MPC Satellites Ephemeris Service[permanent dead link] µ value
  17. ^ Source: JPL/NASA
  18. ^ Computed from IAG Travaux 2001.
  19. ^ Lopes, R. M. C.; et al. (2004). "Lava Lakes on Io: Observations of Io's Volcanic Activity from Galileo NIMS During the 2001 Fly-bys". Icarus. 169 (1): 140–174. Bibcode:2004Icar..169..140L. doi:10.1016/j.icarus.2003.11.013.
  20. ^ Schenk, P.; et al. (2001). "The Mountains of Io: Global and Geological Perspectives from Voyager and Galileo". Journal of Geophysical Research. 106 (E12): 33201–33222. Bibcode:2001JGR...10633201S. doi:10.1029/2000JE001408.
  21. ^ Porco, C. C.; et al. (2003). "Cassini imaging of Jupiter's atmosphere, satellites, and rings". Science. 299 (5612): 1541–1547. Bibcode:2003Sci...299.1541P. doi:10.1126/science.1079462. PMID 12624258.
  22. ^ McEwen, A. S.; et al. (1998). "High-temperature silicate volcanism on Jupiter's moon Io". Science. 281 (5373): 87–90. Bibcode:1998Sci...281...87M. doi:10.1126/science.281.5373.87. PMID 9651251.
  23. ^ Fanale, F. P.; et al. (1974). "Io: A Surface Evaporite Deposit?". Science. 186 (4167): 922–925. Bibcode:1974Sci...186..922F. doi:10.1126/science.186.4167.922. PMID 17730914.
  24. ^ "Europa: Another Water World?". Project Galileo: Moons and Rings of Jupiter. NASA, Jet Propulsion Laboratory. 2001. Retrieved 9 August 2007.
  25. ^ Schenk, P. M.; Chapman, C. R.; Zahnle, K.; Moore, J. M.; Chapter 18: Ages and Interiors: the Cratering Record of the Galilean Satellites, in Jupiter: The Planet, Satellites and Magnetosphere, Cambridge University Press, 2004
  26. ^ Hamilton, C. J. "Jupiter's Moon Europa".
  27. ^ 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. {{cite web}}: Unknown parameter |deadurl= ignored (|url-status= suggested) (help)
  28. ^ "Tidal Heating". geology.asu.edu. Archived from the original on 2006-03-29. Retrieved 2007-10-20.
  29. ^ Exotic Microbes Discovered near Lake Vostok, Science@NASA (December 10, 1999)
  30. ^ Jones, N.; Bacterial explanation for Europa's rosy glow, NewScientist.com (11 December 2001)
  31. ^ Phillips, Cynthia (28 September 2006). "Time for Europa". Space.com. Retrieved 5 January 2014. {{cite web}}: Unknown parameter |deadurl= ignored (|url-status= suggested) (help)
  32. ^ Arnett, B.; Europa (November 7, 1996)
  33. ^ Carlson, R.W.; M.S. Anderson (2005). "Distribution of hydrate on Europa: Further evidence for sulfuric acid hydrate". Icarus. 177: 461–471. Bibcode:2005Icar..177..461C. doi:10.1016/j.icarus.2005.03.026.
  34. ^ "Satellites of Jupiter". The Galileo Project. Retrieved 2007-11-24.
  35. ^ "Ganymede". nineplanets.org. October 31, 1997. Retrieved 2008-02-27.
  36. ^ Kivelson, M.G.; Khurana, K.K.; et al. (2002). "The Permanent and Inductive Magnetic Moments of Ganymede" (PDF). Icarus. 157 (2): 507–522. Bibcode:2002Icar..157..507K. doi:10.1006/icar.2002.6834.
  37. ^ "Solar System's largest moon likely has a hidden ocean". Jet Propulsion Laboratory. NASA. 2000-12-16. Retrieved 2008-01-11.
  38. ^ Hall, D.T.; Feldman, P.D.; et al. (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.
  39. ^ Eviatar, Aharon; Vasyliunas, Vytenis M.; et al. (2001). "The ionosphere of Ganymede" (ps). Planet. Space Sci. 49 (3–4): 327–336. Bibcode:2001P&SS...49..327E. doi:10.1016/S0032-0633(00)00154-9.
  40. ^ Musotto, Susanna; Varadi, Ferenc; Moore, William; Schubert, Gerald; Moore, William; Schubert, Gerald (2002). "Numerical Simulations of the Orbits of the Galilean Satellites". Icarus. 159 (2): 500–504. Bibcode:2002Icar..159..500M. doi:10.1006/icar.2002.6939.{{cite journal}}: CS1 maint: multiple names: authors list (link)
  41. ^ Carlson, R. W.; et al. (1999). "A Tenuous Carbon Dioxide Atmosphere on Jupiter's Moon Callisto" (PDF). Science. 283 (5403): 820–821. Bibcode:1999Sci...283..820C. doi:10.1126/science.283.5403.820. PMID 9933159.
  42. ^ Liang, M. C.; Lane, B. F.; Pappalardo, R. T.; et al. (2005). "Atmosphere of Callisto" (PDF). Journal of Geophysical Research. 110 (E2): E02003. Bibcode:2005JGRE..11002003L. doi:10.1029/2004JE002322.
  43. ^ Showman, Adam P.; Malhotra, Renu (1999). "The Galilean Satellites" (PDF). Science. 286 (5437): 77–84. doi:10.1126/science.286.5437.77. PMID 10506564.
  44. ^ Lipps, Jere H.; Delory, Gregory; Pitman, Joe; et al. (2004). Hoover, Richard B; Levin, Gilbert V; Rozanov, Alexei Y (eds.). "Astrobiology of Jupiter's Icy Moons" (PDF). Proc. SPIE. Instruments, Methods, and Missions for Astrobiology VIII. 5555: 10. doi:10.1117/12.560356.
  45. ^ Trautman, Pat; Bethke, Kristen (2003). "Revolutionary Concepts for Human Outer Planet Exploration(HOPE)" (PDF). NASA.
  46. ^ 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 20 September 2009. Retrieved 5 January 2014. {{cite web}}: Unknown parameter |deadurl= ignored (|url-status= suggested) (help)
  47. ^ a b c d e Canup, Robert M.; Ward, William R. (2009). "Origin of Europa and the Galilean Satellites". Europa. University of Arizona Press (in press). Bibcode:2008arXiv0812.4995C.
  48. ^ 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.
  49. ^ Yeomans, Donald K. (2006-07-13). "Planetary Satellite Physical Parameters". JPL Solar System Dynamics. Retrieved 2008-08-23.
  50. ^ 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
  51. ^ Jupiter near perihelion 2010-Sep-19: 656.7 (Callisto angular separation arcsec) − 24.9 (jup angular radius arcsec) = 631 arcsec = 10 arcmin
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