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[[Image:Jupiter moons anim.gif|thumb|400px|right|Jupiter's outer moons and their highly inclined orbits]]
[[Image:Jupiter moons anim.gif|thumb|400px|right|Jupiter's outer moons and their highly inclined orbits]]
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In [[astronomy]], the '''moons of Jupiter''' are the [[natural satellite]]s of [[Jupiter]]. The most massive of them, the four [[Galilean moons]], were discovered in 1610 and were [[Timeline of discovery of Solar System planets and their moons|the first known objects]] found revolving a body that was neither [[Earth]] nor the [[Sun]]. From the end of the 19th century, dozens of much smaller Jovian moons were discovered, and as of 2008, 49 of these had received the names of lovers, conquests, or daughters of the [[Roman mythology|Roman god]] [[Jupiter (mythology)|Jupiter]], or his [[Greek mythology|Greek equivalent]], [[Zeus]]. Another 14 small unnamed bodies have been discovered since, raising the number of known moons to 63—the largest retinue of moons with "reasonably secure" orbits of any planet in the Solar System.<ref>{{cite web|url=http://ssd.jpl.nasa.gov/?bodies|title=Solar System Bodies|publisher=JPL/NASA|accessdate=2008-09-09}}</ref> However, aside from the Galileans, Jovian moons are very small; Europa, the smallest Galilean, is five thousand times more massive than all the non-Galilean moons combined. All but eight Jovian moons have irregular orbits, and most are likely to be small captured [[asteroid]]s.
[[Jupiter]] has 63 confirmed [[natural satellite|moons]].


⚫
Both physical and orbital characteristics of the moons vary widely: [[Ganymede (moon)|Ganymede]] is the [[List of moons by diameter|largest object]] in the [[Solar System]] outside the Sun and the eight [[planet]]s, but some moons are barely one km (half a mile) in diameter; from nearly perfect circular [[orbit]]s, to highly [[eccentricity (astronomy)|eccentric]] ones; from some with [[orbital period]]s taking less than Jupiter does to spin around its axis, to some taking 3,000 times more (almost three Earth [[year]]s). Furthermore, the great majority of these moons rotate in the opposite direction that Jupiter spins, a motion referred as [[Retrograde and direct motion|retrograde rotation]].
Only 8 of these are ''regular satellites'', which all have [[prograde]] orbits that are not greatly [[inclination|inclined]] with respect to Jupiter's equatorial plane. The most massive of them, the four [[Galilean moons]], were discovered in 1610 and were [[Timeline of discovery of Solar System planets and their moons|the first known objects]] found to be orbiting a body that was neither [[Earth]] nor the [[Sun]]. The Galilean satellites are [[hydrostatic equilibrium|spheroidal]] in shape, and so would be considered [[dwarf planet]]s if they were in direct orbit about the Sun. The other four regular satellites are much smaller and closer to Jupiter; these serve as sources of the dust that makes up [[Rings of Jupiter|Jupiter's rings]].

Jupiter's other 55 moons are ''irregular satellites'', whose orbits are much farther from Jupiter, have high [[inclination]]s, and are mixed between [[prograde]] and [[retrograde]]. These moons were likely captured by Jupiter from an original orbit about the Sun. Aside from the Galileans, Jovian moons are very small; Europa, the smallest Galilean, is five thousand times more massive than all the non-Galilean moons combined.

⚫
From the end of the 19th century, dozens of much smaller Jovian moons were discovered, and as of 2008, 49 of these had received the names of lovers, conquests, or daughters of the [[Roman mythology|Roman god]] [[Jupiter (mythology)|Jupiter]], or his [[Greek mythology|Greek equivalent]], [[Zeus]]. Another 14 small unnamed bodies have been discovered since, raising the number of known moons to 63—the largest retinue of moons with "reasonably secure" orbits of any planet in the Solar System.<ref>{{cite web|url=http://ssd.jpl.nasa.gov/?bodies|title=Solar System Bodies|publisher=JPL/NASA|accessdate=2008-09-09}}</ref>

⚫
Both physical and orbital characteristics of the moons vary widely: [[Ganymede (moon)|Ganymede]] is the [[List of moons by diameter|largest object]] in the [[Solar System]] outside the Sun and the eight [[planet]]s, but some moons are barely one km (half a mile) in diameter; from nearly perfect circular [[orbit]]s, to highly [[eccentricity (astronomy)|eccentric]] ones; from some with [[orbital period]]s taking less than Jupiter does to spin around its axis, to some taking 3,000 times more (almost three Earth [[year]]s).


==Discovery==
==Discovery==

Revision as of 17:23, 10 September 2008

Jupiter's outer moons and their highly inclined orbits

In astronomy, the moons of Jupiter are the natural satellites of Jupiter. The most massive of them, the four Galilean moons, were discovered in 1610 and were the first known objects found revolving a body that was neither Earth nor the Sun. From the end of the 19th century, dozens of much smaller Jovian moons were discovered, and as of 2008, 49 of these had received the names of lovers, conquests, or daughters of the Roman god Jupiter, or his Greek equivalent, Zeus. Another 14 small unnamed bodies have been discovered since, raising the number of known moons to 63—the largest retinue of moons with "reasonably secure" orbits of any planet in the Solar System.[1] However, aside from the Galileans, Jovian moons are very small; Europa, the smallest Galilean, is five thousand times more massive than all the non-Galilean moons combined. All but eight Jovian moons have irregular orbits, and most are likely to be small captured asteroids.

Both physical and orbital characteristics of the moons vary widely: Ganymede is the largest object in the Solar System outside the Sun and the eight planets, but some moons are barely one km (half a mile) in diameter; from nearly perfect circular orbits, to highly eccentric ones; from some with orbital periods taking less than Jupiter does to spin around its axis, to some taking 3,000 times more (almost three Earth years). Furthermore, the great majority of these moons rotate in the opposite direction that Jupiter spins, a motion referred as retrograde rotation.

Discovery

The Galilean moons. From left to right, in order of increasing distance from Jupiter: Io, Europa, Ganymede, Callisto.
The Galilean moons and their orbits around Jupiter
See also: Timeline of discovery of Solar System planets and their moons

The first claimed observation of one of Jupiter's moons is that of the Chinese astronomer Gan De around 364 BC.[2] However, the first certain observations of Jupiter's satellites were those of Galileo Galilei in 1609.[3] By March 1610, he had sighted the four massive Galilean moons with his 30x magnitude telescope:[4] Ganymede, Callisto, Io, and Europa. No additional satellites were discovered until E.E. Barnard observed Amalthea in 1892.[5] With the aid of telescopic photography, further discoveries followed quickly over the course of the twentieth century. Himalia was discovered in 1904,[6] Elara in 1905,[7] Pasiphaë in 1908,[8] Sinope in 1914,[9] Lysithea and Carme in 1938,[10] Ananke in 1951.[11] and Leda in 1974.[12] By the time Voyager space probes reached Jupiter around 1979, 13 moons had been discovered, while Themisto was observed in 1975,[13] but due to insufficient initial observation data, it was lost until 2000. The Voyager missions discovered an additional three inner moons in 1979: Metis, Adrastea, and Thebe.[14]

For two decades no additional moons were discovered; but between October 1999 and February 2003, researchers using sensitive ground-based detectors found another 32 moons, most of which were discovered by a team lead by Scott S. Sheppard and David C. Jewitt.[15] These are tiny moons, in long, eccentric, generally retrograde orbits, and average of 3 km (1.9 mi) in diameter, with the largest being just 9 km (5.6 mi) across. All of these moons are thought to be captured asteroidal or perhaps cometary bodies, possibly fragmented into several pieces,[16] but very little is actually known about them. A number of 14 additional moons were discovered since then, but not yet confirmed, bringing the total number of observed moons of Jupiter at 63.[17] This is currently the most of any planet in the Solar System, but additional tiny, undiscovered moons may exist.

Naming

Main article: Naming of moons
The relative masses of the Jovian moons. Those smaller than Europa are invisible at this scale, and taken together would only just be visible at 50x magnification.

The Galilean moons of Jupiter (Io, Europa, Ganymede and Callisto) were named by Simon Marius soon after their discovery in 1610.[18] However, until the 20th century these fell out of favor, and instead they were referred to in the astronomical literature simply as "Jupiter I", "Jupiter II", etc., or as "the first satellite of Jupiter", "Jupiter's second satellite", an so on.[18] The names Io, Europa, Ganymede, and Callisto became popular in the 20th century, while the rest of the moons, usually numbered in Roman numerals V (5) through XII (12), remained unnamed.[19] By a popular though unofficial convention, Jupiter V, discovered in 1892, was given the name Amalthea, first used by the French astronomer Camille Flammarion.[15]

The other moons, in the majority of astronomical literature, were simply labeled by their Roman numeral (i.e. Jupiter IX) until the 1970s.[20] In 1975, the International Astronomical Union's (IAU) "Task Group for Outer Solar System Nomenclature" granted names to satellites V–XIII,[21] and provided for a formal naming process for future satellites to be discovered.[21] The practice was that newly discovered moons of Jupiter to be named after lovers and favorites of the mythological Jupiter (Zeus), and since 2004, also after their descendants.[22] All of Jupiter's satellites from XXXIV (Euporie) are named after daughters of Jupiter or Zeus.[22]

Some asteroids share the same names as moons of Jupiter: 9 Metis, 38 Leda, 52 Europa, 85 Io, 113 Amalthea, 239 Adrastea. Two more asteroids previously shared the names of Jovian moons until spelling differences were made permanent by the IAU: Ganymede and asteroid 1036 Ganymed; and Callisto and asteroid 204 Kallisto.

Groups

The orbits of Jupiter's irregular satellites, and how they cluster into groups: by semi-major axis (the horizontal axis in Gm); by orbital inclination (the vertical axis); and orbital eccentricity (the yellow lines). The relative sizes are indicated by the circles.

Regular satellites

These are split into two groups:

  • Inner satellites or Amalthea group — they orbit very close to Jupiter: Metis, Adrastea, Amalthea, and Thebe. The innermost two orbit in less than a Jovian day, while the latter two are the fifth, respectively the seventh largest moons in the system. Observations suggest that at least the largest member, Amalthea, did not form on the present orbit, but that it was formed farther from the planet, or that it is captured Solar System body.[23] These moons, along with a number of as-yet-unseen inner moonlets, replenish and maintain Jupiter's faint ring system. Metis and Adrastea help to maintain Jupiter's main ring, while Amalthea and Thebe each maintain their own faint outer rings.[24][25]
  • Main group or Galilean moons — the four massive satellites: Ganymede, Callisto, Io, and Europa. With radii that are larger than any of the dwarf planets, they are some of the largest objects in the Solar System outside the Sun and the eight planets in terms of diameter. Respectively the first, third, fourth, and sixth largest natural satellites in the Solar System, they contain almost 99.999% of the total mass in orbit around Jupiter. The inner moons also participate in a 1:2:4 orbital resonance. Models suggest that they formed by slow accretion in the low-density Jovian subnebula—a disc of the gas and dust that existed around Jupiter after its formation—which lasted up to 10 million years in the case of Callisto.[26]

Irregular satellites

Main article: Irregular satellite

The irregular satellites are substantially smaller objects with more distant and eccentric orbits. They form families with shared similarities in orbit (semi-major axis, inclination, eccentricity) and composition; it is believed that these are at least partially collisional families that were created when larger (but still small) parent bodies were shattered by impacts from asteroids captured by Jupiter's gravitational field. These families bear the names of their largest members. The identification of satellite families is tentative, but the following are typically listed:[17][27][28]

  • Themisto[27] is the innermost irregular moon and not part of a known family.[17]
  • Carpo is the outermost prograde moon and not part of a known family.[17]
Retrograde satellites: inclinations (°) vs eccentricities, with Carme's (orange) and Ananke's (yellow) groups identified
  • The irregular retrograde satellites are thought to have originally been asteroids that were captured by drag from the tenuous outer regions of Jupiter's accretion disk while the Solar system was still forming, and were later shattered by impacts. They are far enough from Jupiter that their orbits are significantly disturbed by the gravitational field of the Sun.
  • S/2003 J 2 is the innermost of the retrograde moons, and is not part of a known family.
  • The Carme group is spread over only 1.2 Gm in semi-major axis, 1.6° in inclination (165.7 ± 0.8°), and eccentricities between 0.23 and 0.27. It is very homogeneous in color (light red) and is believed to have originated from a D-type asteroid progenitor, possibly a Jupiter trojan.[16]
  • The Ananke group has a relatively wider spread than the previous groups, over 2.4 Gm in semi-major axis, 8.1° in inclination (between 145.7° and 154.8°), and eccentricities between 0.02 and 0.28. Most of the members appear gray, and are believed to have formed from the breakup of a captured asteroid.[16]
  • The Pasiphae group is quite dispersed, with a spread over 1.3 Gm, inclinations between 144.5° and 158.3°, and their eccentricities between 0.25 and 0.43.[16] The colors also vary significantly, from red to grey, which might be the result of multiple collisions. Sinope, sometimes included into Pasiphae group,[16] is red and given the difference in inclination, it could have been captured independently;[27] Pasiphae and Sinope are also trapped in secular resonances with Jupiter.[29]
  • S/2003 J 2 is the outermost moon of Jupiter, and is not part of a known family.

Table

The moons of Jupiter are listed below by orbital period. Moons massive enough for their surfaces to have collapsed into a spheroid are highlighted in blue(†); these are the four Galilean moons, which are comparable in size to Earth's Moon. The four inner moons have no background color. Irregular, captured moons are indicated by gray shading: light for prograde satellites, and dark gray for retrograde.

Order
[note 1] 		Label
[note 2] 		Name
 Pronunciation
(key) 		Image Diameter
(km)[note 3] 		Mass
(×1016 kg) 		Semi-major axis
(km)[30] 		Orbital period
(d)[30][note 4] 		Inclination
(°)[30] 		Eccentricity
[17] 		Discovery year
[15] 		Discoverer
[15] 		Group
[note 5]
1 XVI Metis ˈmiːtɨs
File:Metis2.gif
 60×40×34 ~3.6 127,690 + 7h 4m 29s 0.06°[31] 0.00002 1979 Synnott
(Voyager 1)		 Inner
2 XV Adrastea ˌædrəˈstiːə
20×16×14 ~0.2 128,690 + 7h 9m 30s 0.03°[31] 0.0015 1979 Jewitt
(Voyager 2)		 Inner
3 V Amalthea ˌæməlˈθiːə
250×146×128 208 181,366 + 11h 57m 23s 0.374°[31] 0.0032 1892 Barnard Inner
4 XIV Thebe ˈθiːbi
116×98×84 ~43 221,889 + 16h 11m 17s 1.076°[31] 0.0175 1979 Synnott
(Voyager 1)		 Inner
5 I Io† ˈaɪ.oʊ
3660.0×3637.4
×3630.6		 8,900,000 421,700 + 1.769137786 0.050°[31] 0.0041 1610 Galilei Galilean
6 II Europa† jʊˈroʊpə
3121.6 4,800,000 671,034 + 3.551181041 0.471°[31] 0.0094 1610 Galilei Galilean
7 III Ganymede† ˈgænɨmiːd
5262.4 15,000,000 1,070,412 + 7.15455296 0.204°[31] 0.0011 1610 Galilei Galilean
8 IV Callisto† kəˈlɪstoʊ
4820.6 11,000,000 1,882,709 + 16.6890184 0.205°[31] 0.0074 1610 Galilei Galilean
9 XVIII Themisto θɨˈmɪstoʊ 8 0.069 7,393,216 + 129.87 45.762° 0.2115 1975/2000 Kowal & Roemer/
Sheppard et al.		 Themisto
10 XIII Leda ˈliːdə 16 0.6 11,187,781 + 241.75 27.562° 0.1673 1974 Kowal Himalia
11 VI Himalia haɪˈmeɪliə
170 670 11 451 971 + 250.37 30.486° 0.1513 1904 Perrine Himalia
12 X Lysithea laɪˈsɪθiə 36 6.3 11,740,560 + 259.89 27.006° 0.1322 1938 Nicholson Himalia
13 VII Elara ˈɛlərə 86 87 11,778,034 + 261.14 29.691° 0.1948 1905 Perrine Himalia
14 — S/2000 J 11 4 0.0090 12 570 424 + 287.93 27.584° 0.2058 2001 Sheppard et al. Himalia
15 XLVI Carpo ˈkɑrpoʊ 3 0.0045 17,144,873 + 458.62 56.001° 0.2735 2003 Sheppard et al. Carpo
16 — S/2003 J 12 1 0.00015 17,739,539 - 482.69 142.680° 0.4449 2003 Sheppard et al. ?
17 XXXIV Euporie juːˈpɔərɨ.i 2 0.0015 19,088,434 - 538.78 144.694° 0.0960 2002 Sheppard et al. Ananke
18 — S/2003 J 3 2 0.0015 19,621,780 - 561.52 146.363° 0.2507 2003 Sheppard et al. Ananke
19 — S/2003 J 18 2 0.0015 19,812,577 - 569.73 147.401° 0.1569 2003 Gladman et al. Ananke
20 XLII Thelxinoe θɛlkˈsɪnoʊ.i 2 0.0015 20,453,753 - 597.61 151.292° 0.2684 2003 Sheppard et al. Ananke
21 XXXIII Euanthe juːˈænθi 3 0.0045 20,464,854 - 598.09 143.409° 0.2000 2002 Sheppard et al. Ananke
22 XLV Helike ˈhɛlɨki 4 0.0090 20,540,266 - 601.40 154.586° 0.1374 2003 Sheppard et al. Ananke
23 XXXV Orthosie ɔrˈθɒsɨ.i 2 0.0015 20,567,971 - 602.62 142.366° 0.2433 2002 Sheppard et al. Ananke
24 XXIV Iocaste ˌaɪ.əˈkæsti 5 0.019 20,722,566 - 609.43 147.248° 0.2874 2001 Sheppard et al. Ananke
25 — S/2003 J 16 2 0.0015 20,743,779 - 610.36 150.769° 0.3184 2003 Gladman et al. Ananke
26 XXVII Praxidike prækˈsɪdɨki 7 0.043 20,823,948 - 613.90 144.205° 0.1840 2001 Sheppard et al. Ananke
27 XXII Harpalyke hɑrˈpælɨki 4 0.012 21,063,814 - 624.54 147.223° 0.2440 2001 Sheppard et al. Ananke
28 XL Mneme ˈniːmi 2 0.0015 21,129,786 - 627.48 149.732° 0.3169 2003 Gladman et al. Ananke
29 XXX Hermippe hɚˈmɪpi 4 0.0090 21,182,086 - 629.81 151.242° 0.2290 2002 Sheppard et al. Ananke?
30 XXIX Thyone θaɪˈoʊni 4 0.0090 21,405,570 - 639.80 147.276° 0.2525 2002 Sheppard et al. Ananke
31 XII Ananke əˈnæŋki 28 3.0 21,454,952 - 642.02 151.564° 0.3445 1951 Nicholson Ananke
32 — S/2003 J 17 2 0.0015 22,134,306 - 672.75 162.490° 0.2379 2003 Gladman et al. Carme
33 XXXI Aitne ˈaɪtni 3 0.0045 22,285,161 - 679.64 165.562° 0.3927 2002 Sheppard et al. Carme
34 XXXVII Kale ˈkeɪli 2 0.0015 22,409,207 - 685.32 165.378° 0.2011 2002 Sheppard et al. Carme
35 XX Taygete teiˈɪdʒɨti 5 0.016 22,438,648 - 686.67 164.890° 0.3678 2001 Sheppard et al. Carme
36 — S/2003 J 19 2 0.0015 22,709,061 - 699.12 164.727° 0.1961 2003 Gladman et al. Carme
37 XXI Chaldene kælˈdiːni 4 0.0075 22,713,444 - 699.33 167.070° 0.2916 2001 Sheppard et al. Carme
38 — S/2003 J 15 2 0.0015 22,720,999 - 699.68 141.812° 0.0932 2003 Sheppard et al. Ananke?
39 — S/2003 J 10 2 0.0015 22,730,813 - 700.13 163.813° 0.3438 2003 Sheppard et al. Carme?
40 — S/2003 J 23 2 0.0015 22,739,654 - 700.54 148.849° 0.3930 2004 Sheppard et al. Pasiphaë
41 XXV Erinome ɨˈrɪnəmi 3 0.0045 22,986,266 - 711.96 163.737° 0.2552 2001 Sheppard et al. Carme
42 XLI Aoede eɪˈiːdi 4 0.0090 23,044,175 - 714.66 160.482° 0.6011 2003 Sheppard et al. Pasiphaë
43 XLIV Kallichore kəˈlɪkəri 2 0.0015 23,111,823 - 717.81 164.605° 0.2041 2003 Sheppard et al. Carme?
44 XXIII Kalyke ˈkælɨki 5 0.019 23,180,773 - 721.02 165.505° 0.2139 2001 Sheppard et al. Carme
45 XI Carme ˈkɑrmi 46 13 23,197,992 - 721.82 165.047° 0.2342 1938 Nicholson Carme
46 XVII Callirrhoe kəˈlɪroʊ.i 9 0.087 23,214,986 - 722.62 139.849° 0.2582 2000 Gladman et al. Pasiphaë
47 XXXII Eurydome jʊˈrɪdəmi 3 0.0045 23,230,858 - 723.36 149.324° 0.3769 2002 Sheppard et al. Pasiphaë?
48 XXXVIII Pasithee pəˈsɪθɨ.i 2 0.0015 23,307,318 - 726.93 165.759° 0.3288 2002 Sheppard et al. Carme
49 XLVIII Cyllene sɨˈliːni 2 0.0015 23,396,269 - 731.10 140.148° 0.4115 2003 Sheppard et al. Pasiphaë
50 XLVII Eukelade juːˈkɛlədi 4 0.0090 23,483,694 - 735.20 163.996° 0.2828 2003 Sheppard et al. Carme
51 — S/2003 J 4 2 0.0015 23,570,790 - 739.29 147.175° 0.3003 2003 Sheppard et al. Pasiphaë
52 VIII Pasiphaë pəˈsɪfeɪ.i 60 30 23,609,042 - 741.09 141.803° 0.3743 1908 Gladman et al. Pasiphaë
53 XXXIX Hegemone hɨˈdʒɛməni 3 0.0045 23,702,511 - 745.50 152.506° 0.4077 2003 Sheppard et al. Pasiphaë
54 XLIII Arche ˈɑrki 3 0.0045 23,717,051 - 746.19 164.587° 0.1492 2002 Sheppard et al. Carme
55 XXVI Isonoe aɪˈsɒnoʊ.i 4 0.0075 23,800,647 - 750.13 165.127° 0.1775 2001 Sheppard et al. Carme
56 — S/2003 J 9 1 0.00015 23,857,808 - 752.84 164.980° 0.2761 2003 Sheppard et al. Carme
57 — S/2003 J 5 4 0.0090 23,973,926 - 758.34 165.549° 0.3070 2003 Sheppard et al. Carme
58 IX Sinope sɨˈnoʊpi 38 7.5 24,057,865 - 762.33 153.778° 0.2750 1914 Nicholson Pasiphaë
59 XXXVI Sponde ˈspɒndi 2 0.0015 24,252,627 - 771.60 154.372° 0.4431 2002 Sheppard et al. Pasiphaë
60 XXVIII Autonoe ɔːˈtɒnoʊ.i 4 0.0090 24,264,445 - 772.17 151.058° 0.3690 2002 Sheppard et al. Pasiphaë
61 XLIX Kore ˈkɔəri 2 0.0015 23,345,093 - 776.02 137.371° 0.1951 2003 Sheppard et al. Pasiphaë
62 XIX Megaclite ˌmɛgəˈklaɪti 5 0.021 24,687,239 - 792.44 150.398° 0.3077 2001 Sheppard et al. Pasiphaë
63 — S/2003 J 2 2 0.0015 30,290,846 - 1,077.02 153.521° 0.1882 2003 Sheppard et al. ?

See also

Notes

  1. ^ Order refers to the position among other moons with respect to their average distance from Jupiter.
  2. ^ Label refers to the Roman numeral attributed to each moon in order of their discovery.
  3. ^ Diameters with multiple entries such as "60×40×34" reflect that the body is not a perfect spheroid and that each of its dimensions have been measured well enough.
  4. ^ Periods with negative values are retrograde.
  5. ^ "?" refers to group assignments that are not considered sure yet.

References

  1. ^ "Solar System Bodies". JPL/NASA. Retrieved 2008-09-09.
  2. ^ Xi, Zezong Z. (1981). "The Discovery of Jupiter's Satellite Made by Gan De 2000 years Before Galileo". Acta Astrophysica Sinica. 1 (2): 87.
  3. ^ Galilei, Galileo (1989). Translated and prefaced by Albert Van Helden (ed.). Sidereus Nuncius. Chicago & London: University of Chicago Press. pp. 14–16. ISBN 0226279030.
  4. ^ Van Helden, Albert (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. {{cite journal}}: Unknown parameter |month= ignored (help)
  5. ^ Barnard, E. E. (1892). "Discovery and Observation of a Fifth Satellite to Jupiter". Astronomical Journal. 12: 81–85. doi:10.1086/101715.
  6. ^ "Discovery of a Sixth Satellite of Jupiter". Astronomical Journal. 24 (18): 154B, . 1905 January 9. doi:10.1086/103654. {{cite journal}}: Check date values in: |date= (help)CS1 maint: extra punctuation (link)
  7. ^ Perrine, C. D. (1905). "The Seventh Satellite of Jupiter". Publications of the Astronomical Society of the Pacific. 17 (101): 62–63.
  8. ^ Melotte, P. J. (1908). "Note on the Newly Discovered Eighth Satellite of Jupiter, Photographed at the Royal Observatory, Greenwich". Monthly Notices of the Royal Astronomical Society. 68 (6): 456–457.
  9. ^ Nicholson, S. B. (1914). "Discovery of the Ninth Satellite of Jupiter". Publications of the Astronomical Society of the Pacific. 26: pp. 197–198. doi:10.1086/122336. {{cite journal}}: |pages= has extra text (help)
  10. ^ Nicholson, S.B. (1938). "Two New Satellites of Jupiter". Publications of the Astronomical Society of the Pacific. 50: 292–293. doi:10.1086/124963.
  11. ^ Nicholson, S. B. (1951). "An unidentified object near Jupiter, probably a new satellite". Publications of the Astronomical Society of the Pacific. 63 (375): 297–299. doi:10.1086/126402.
  12. ^ Kowal, C. T. (1974). "Thirteenth satellite of Jupiter". Astronomical Journal. 80: pp. 460–464. doi:10.1086/111766. {{cite journal}}: |pages= has extra text (help); Unknown parameter |coauthors= ignored (|author= suggested) (help)
  13. ^ Marsden, Brian G. (1975). "Probable New Satellite of Jupiter" (discovery telegram sent to the IAU). International Astronomical Union Circulars. 2845. Cambridge, US: Smithsonian Astrophysical Observatory. Retrieved 2008-09-03. {{cite journal}}: Unknown parameter |day= ignored (help); Unknown parameter |month= ignored (help)
  14. ^ Synnott, S.P. (1980). "1979J2: The Discovery of a Previously Unknown Jovian Satellite". Science. 210 (4471): 786–788. doi:10.1126/science.210.4471.786. PMID 17739548.
  15. ^ a b c d "Gazetteer of Planetary Nomenclature". Working Group for Planetary System Nomenclature (WGPSN). U.S. Geological Survey. 2008-11-07 11:42:58. Retrieved 2008-08-02. {{cite web}}: Check date values in: |date= (help)
  16. ^ a b c d e Sheppard, Scott S. (May 5, 2003). "An abundant population of small irregular satellites around Jupiter". Nature. 423: 261–263. doi:10.1038/nature01584. {{cite journal}}: Check date values in: |date= (help); Unknown parameter |coauthors= ignored (|author= suggested) (help)
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  21. ^ a b Marsden, Brian G. (1975). "Satellites of Jupiter". International Astronomical Union Circulars. 2846. Retrieved 2008-08-28. {{cite journal}}: Unknown parameter |day= ignored (help); Unknown parameter |month= ignored (help)
  22. ^ a b Satellites of Jupiter, Saturn and Uranus. Working Group on Planetary System Nomenclature (Report). International Astronomical Union. Retrieved 2008-08-28.
  23. ^ Anderson, J.D. (2005). "Amalthea's Density Is Less Than That of Water". Science. 308: 1291–1293. doi:10.1126/science.1110422. PMID 15919987. {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help)
  24. ^ Burns, J.A.; Simonelli, D. P.; Showalter, M.R.; et al. (2004). "Jupiter's Ring-Moon System". In Bagenal, F.; Dowling, T.E.; McKinnon, W.B. (ed.). Jupiter: The Planet, Satellites and Magnetosphere. Cambridge University Press. {{cite book}}: Explicit use of et al. in: |author= (help)CS1 maint: multiple names: authors list (link)
  25. ^ Burns, J. A.; Showalter, M. R.; Hamilton, D. P.; et al. (1999). "The Formation of Jupiter's Faint Rings". Science. 284: 1146–1150. doi:10.1126/science.284.5417.1146. {{cite journal}}: Explicit use of et al. in: |author= (help)CS1 maint: multiple names: authors list (link)
  26. ^ 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)
  27. ^ a b c d Grav, Tommy; Holman, Matthew J.; Gladman, Brett J.; Aksnes, Kaare (2003). "Photometric survey of the irregular satellites". Icarus. 166 (1): 33–45. doi:arXiv:astro-ph/0301016v1. {{cite journal}}: Check |doi= value (help)CS1 maint: multiple names: authors list (link) Cite error: The named reference "Grav2003" was defined multiple times with different content (see the help page).
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