Difference between revisions of "Jupiter"

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{{other uses|Jupiter (disambiguation)}}
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{| cellpadding="2" cellspacing="0" style="margin:25px 0 0 10px; border:3px solid lightsteelblue;width:250px; font-size:90%; font-family:'Arial','Helvetica'; float: right; clear: right;"Template in Orbiter"
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!bgcolor="lightsteelblue" colspan="2" align="center" |Jupiter
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Additional parameters for this template are available at [[Template:Infobox Planet]].
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|colspan="2" align="center"|[[Image:JupiterScrshot.jpg|240px]]
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{{Infobox Planet
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|colspan="2" align="center"|'''Jupiter in Orbiter 2016 with D3D9'''
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| bgcolour=#FFC8A0
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|-
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| name = Jupiter
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!bgcolor="lightsteelblue" colspan="2"|Designation
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| symbol = [[Image:Jupiter symbol.svg|25px|Astronomical symbol of Jupiter]]
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| image = [[image:Jupiter.jpg|240px|Click for full caption.]]
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|Name||align="right"|Jupiter
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| caption = Click image for description
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| epoch = [[J2000]]
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|width="30%"|Reference body||align="right" width="30%"|Sun
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| aphelion = 816,620,000&nbsp;km<ref name="jupiterfactsheet">{{cite web | first=David R. | last=Williams | date = [[November 16]], [[2004]] | url = http://nssdc.gsfc.nasa.gov/planetary/factsheet/jupiterfact.html | title = Jupiter Fact Sheet | publisher = NASA | accessdate = 2007-02-21 }}</ref><ref>{{cite web | date = [[September 20]], [[2004]]  | url = http://sci.esa.int/science-e/www/object/index.cfm?fobjectid=35651 | title = Jupiter | publisher = European Space Agency | accessdate = 2007-02-21 }}</ref><br />5.46 AU<br />507,000,000&nbsp;miles
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|-
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| perihelion = 740,520,000&nbsp;km <br />4.95 AU<br />460,280,000&nbsp;miles
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|width="30%"|Number of satellites||align="right" width="30%"|95
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| semimajor = [[1 E11 m|778,300,000]]&nbsp;[[kilometre|km]]<br>5.20336301&nbsp;[[Astronomical unit|AU]]<br />483,680,000&nbsp;miles
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|-
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| eccentricity = 0.04839266
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!bgcolor="lightsteelblue" colspan="2"|Planetary mean orbits
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| inclination = 1.30530&deg;<br />(6.09° to [[Sun]]'s equator)
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|-
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| asc_node = 100.55615&deg;
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|width="30%"|Epoch||align="right" width="50%"|J2000 (1 January 2000)
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| arg_peri = 14.75385&deg;
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|-
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| orbital_circ = 4.888&nbsp;[[Tera|T]][[metre|m]]<br />32.675&nbsp;AU
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|width="30%"|Semimajor axis (a)||align="right" width="50%"|5.20336301 AU <br> (7.784120267×10<sup>11</sup> km)
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| sidereal_period = [[1 E8 s|4,332.589&nbsp;d]]<br />(11.862&nbsp;[[julian year (astronomy)|a]])
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|-
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| synodic_period = 398.88&nbsp;d
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|width="30%"|Eccentricity (e)||align="right" width="30%"|0.04839266
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| avg_speed = 13.07&nbsp;km/s
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|-
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| max_speed = 13.72&nbsp;km/s
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|width="30%"|Inclination (i)||align="right" width="30%"|1.30530° <br> (0.0227818 radian)
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| min_speed = 12.44&nbsp;km/s
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|-
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| satellites = [[Jupiter's natural satellites|63]]
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|width="30%"|Longitude of the ascending node (LAN, ☊)||align="right" width="30%"|100.55615° <br> (1.755036 radian)
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| physical_characteristics = yes
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|-
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| oblateness = 0.06487
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|width="30%"|Longitude of periapsis (ϖ)||align="right" width="30%"|14.75385° <br> (0.257503 radian)
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| equatorial_radius = [[1 E8 m|71,492&nbsp;km]]<br />(11.209 Earths)
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|-
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| polar_radius = 66,854&nbsp;km<br />(10.517&nbsp;Earths)
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|width="30%"|Mean longitude (L)||align="right" width="30%"|34.40438° <br> (0.600470 radian)
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| surface_area = [[1 E16 m²|6.14×10<sup>10</sup>]]&nbsp;[[square kilometre|km<sup>2</sup>]]<br />(120.5 Earths)
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|-
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| volume = 1.43128×10<sup>15</sup>&nbsp;[[cubic kilometre|km<sup>3</sup>]]<br />(1321.3&nbsp;Earths)
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!bgcolor="lightsteelblue" colspan="2"|Planetary orbital element centennial rates
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| mass = [[1 E27 kg|1.8986×10<sup>27</sup>]]&nbsp;[[kilogram|kg]]<br />(317.8&nbsp;Earths)
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|-
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| density = 1.326&nbsp;g/cm<sup>3</sup>
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|width="30%"|Semimajor axis (a)||align="right" width="50%"|0.00060737 AU/Century
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| surface_grav = 24.79&nbsp;[[Acceleration|m/s<sup>2</sup>]]<br>(2.358 [[Acceleration due to gravity|g]])
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|-
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| escape_velocity = 59.5&nbsp;km/s
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|width="30%"|Eccentricity (e)||align="right" width="50%"|-0.00012880 Century<sup>-1</sup>
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| sidereal_day = 9.9250&nbsp;h<ref>{{cite web | author = P. K. Seidelmann, V. K. Abalakin, M. Bursa, M. E. Davies, C. de Burgh, J. H. Lieske, J. Oberst, J. L. Simon, E. M. Standish, P. Stooke, P. C. Thomas | year = [[2001]] | url = http://www.hnsky.org/iau-iag.htm | title = Report of the IAU/IAG Working Group on Cartographic Coordinates and Rotational Elements of the Planets and Satellites: 2000 | publisher = HNSKY Planitarium Program | accessdate = 2007-02-02 }}</ref>
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|-
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| rot_velocity = 12.6&nbsp;km/s = 45,300&nbsp;km/h <br />
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|width="30%"|Inclination (i)||align="right" width="30%"|-4.15 seconds/Century
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| axial_tilt = 3.13&deg;
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|-
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| right_asc_north_pole = 268.05° (17&nbsp;h 52&nbsp;min 12&nbsp;s)
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|width="30%"|Longitude of the ascending node (LAN, ☊)||align="right" width="30%"|1217.17 seconds/Century
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| declination = 64.49°
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|-
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| albedo = 0.52
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|width="30%"|Longitude of periapsis (ϖ)||align="right" width="30%"|839.93 seconds/Century
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| adjectives = Jovian
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|-
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| atmosphere = yes
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|width="30%"|Mean longitude (L)||align="right" width="30%"|10925078.35 seconds/Century
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| temperatures = yes
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|-
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| temp_name1 = [[Kelvin]]
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!bgcolor="lightsteelblue" colspan="2"|Selected physical parameters
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| min_temp_1 = 110&nbsp;K
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|-
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| mean_temp_1 = [[1 E2 K|152&nbsp;K]]
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|width="30%"|Mean radius||align="right" width="30%"|69911.0±6 km
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| max_temp_1 = N/A
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|-
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| surface_pressure = 20&ndash;200&nbsp;[[Pascal (unit)|kPa]]<ref>{{cite journal | title=Probe Nephelometer | journal=Galileo Messenger | publisher=NASA/JPL | date=[[March]] [[1983]] | issue=6 | url=http://www2.jpl.nasa.gov/galileo/messenger/oldmess/2Probe.html | accessdate=2007-02-12 }}</ref> (cloud&nbsp;layer)
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|width="30%"|Mass||align="right" width="30%"|1.8986111×10<sup>27</sup> kg
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| atmosphere_composition = ~86% [[Hydrogen|H<sub>2</sub>]]<br />~13% [[Helium]]<br />0.1% [[Methane]]<br />0.1% [[Water]] vapor<br />0.02% [[Ammonia]]<br />0.0002% [[Ethane]]<br />0.0001% [[Phosphine]]<br />&lt;0.00010% [[Hydrogen sulfide]]
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|-
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}}
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|width="30%"|Density||align="right" width="30%"|1.326 g/m<sup>3</sup>
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'''Jupiter''' ({{IPA2|ˈdʒu.pə.tɚ}}, {{IPA2|ˈdʒu.pɪ.tə}}) is the fifth [[planet]] from the [[Sun]] and the [[Solar system by size|largest]] planet within the [[solar system]]. It is two and a half times as massive as all of the other planets in our solar system combined. Jupiter is classified as a [[gas giant]], a designation it shares with [[Saturn]], [[Uranus]], and [[Neptune]]. Together, these four planets are sometimes referred to as the '''[[Jovian planet]]s''' (''Jovian'' being the adjectival form of Jupiter, derived from the Latin [[genitive]] of the noun).
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|width="30%"|Sidereal rotation period||align="right" width="30%"|9.92425 hours
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When viewed from Earth, Jupiter can reach an [[apparent magnitude]] of -2.8, making it the third brightest object in the night sky. The planet was known by [[Astronomer|astronomers]] of ancient times and was associated with the mythology and religious beliefs of many cultures. The Romans named it after ''[[Jupiter (mythology)|Jupiter]]'', the principal [[God (male deity)|God]] of [[Roman mythology]] during the era of [[Classical antiquity|Classical Antiquity]]. The planet's name is a reduction of 'Deus Pater', meaning 'God father'.<ref>{{cite book | last=Lehrer | first=Seth | title=History of the English Language | publisher=The Teaching Company | format=audio tape | location=Stanford University }}</ref>
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|width="30%"|Sidereal orbit period||align="right" width="30%"|11.856523 years
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The planet Jupiter is primarily composed of [[hydrogen]], with a smaller portion of [[helium]] and possibly a rocky core. Because of its rapid rotation the planet possesses a slight but noticeable bulge around the equator, giving it an [[oblate]] appearance. The outer atmosphere is visibly segregated into several bands at different latitudes, resulting in turbulence and storms along their interacting boundaries. A prominent result is the [[Great Red Spot]], a giant storm that is known to have existed since at least the seventeenth century. Surrounding the planet is a faint planetary ring system and a powerful [[magnetosphere]]. There are also at least 63 moons, including the four large moons called the [[Galilean moons]] that were first discovered by [[Galileo Galilei]] in 1610. Two of these moons are bigger than the planet [[Mercury (planet)|Mercury]].
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|width="30%"|Magnitude V(1,0)||align="right" width="30%"|-9.4
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Jupiter has been explored on several occasions by robotic spacecraft; most notably during the early [[Pioneer program|Pioneer]] and [[Voyager program|Voyager]] fly-by missions, and later by the [[Galileo (spacecraft)|Galileo orbiter]]. Future targets for exploration include the possible ice-covered liquid ocean on the Jovian moon [[Europa (moon)|Europa]].
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|width="30%"|Geometric albedo||align="right" width="30%"|0.52
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==Structure==
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Jupiter is one of the four [[gas giant]]s, which means it is a planet that is not primarily composed of solid matter. It is the largest planet in the Solar System, with a diameter of 142,984&nbsp;km at its [[equator]]. The density of this planet is the second highest of the gas giant planets at 1.326&nbsp;g/cm<sup>3</sup>, but the density is lower than any of the four [[terrestrial planet]]s.
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|width="30%"|Equatorial gravity||align="right" width="30%"|23.12±0.01 m/s<sup>2</sup>
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===Composition===
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|width="30%"|Escape velocity||align="right" width="30%"|59.5 km/s
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Jupiter's upper atmosphere is composed of about 93%&nbsp;[[hydrogen]] and 7%&nbsp;[[helium]] by number of [[atom]]s (86%&nbsp;H<sub>2</sub> and 13%&nbsp;He by fraction of gas molecules&mdash;see table at top), or approximately 75%&nbsp;hydrogen and 24%&nbsp;helium by mass, with the remaining 1% of the mass consisting of other elements. The interior contains denser materials such that the distribution is roughly 71%&nbsp;hydrogen, 24%&nbsp;helium and 5% other elements, by mass. The atmosphere contains trace amounts of [[methane]], [[water vapor]], [[ammonia]], and "rock". There are also traces of [[carbon]], [[ethane]], [[hydrogen sulphide]], [[neon]], [[oxygen]], [[phosphine]], and [[sulphur]]. The outermost layer of the atmosphere contains [[crystal]]s of frozen ammonia.<ref name=voyager>{{cite journal
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|-
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| author= Gautier D., Conrath B., Flasar M., Hanel R., Kunde V., Chedin A., Scott N.| title = The helium abundance of Jupiter from Voyager | journal = Journal of Geophysical Research| volume = 86| pages = 8713-8720 | year = [[1981]] | url = http://adsabs.harvard.edu/abs/1981JGR....86.8713G}}</ref><ref name=cassini>Kunde, V. G. et al, [http://www.sciencemag.org/cgi/content/full/305/5690/1582 "Jupiter's Atmospheric Composition from the Cassini Thermal Infrared Spectroscopy Experiment"] - ''[[Science (magazine)|Science]]'' 10 September 2004,
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!bgcolor="lightsteelblue" colspan="2"|Rotation elements
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Vol. 305. no. 5690, pp. 1582 - 1586. URL accessed 15 April 2006.</ref> Through [[infrared]] and [[ultraviolet]] measurements, trace amounts of [[benzene]] and other [[hydrocarbon]]s have also been found.<ref>{{cite journal
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| journal = Icarus| volume = 64| pages = 233-248 | year = [[1985]] | title = Infrared Polar Brightening on Jupiter III. Spectrometry from the Voyager 1 IRIS Experiment | url=http://adsabs.harvard.edu/abs/1985Icar...64..233K | author= Kim S. J., Caldwell J., Rivolo A. R., Wagner R. | doi = 10.1016/0019-1035(85)90201-5 }}</ref>
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|width="30%"|North pole right ascension (α)||align="right" width="30%"|268.04°
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This atmospheric proportions of hydrogen and helium are very close to the theoretical composition of the primordial [[solar nebula]]. However, neon in the upper atmosphere only consists of 20 parts per million by mass, which is about a tenth as abundant as in the Sun.<ref>{{cite journal | author=H. B. Niemann, S. K. Atreya, G. R. Carignan, T. M. Donahue, J. A. Haberman, D. N. Harpold, R. E. Hartle, D. M. Hunten, W. T. Kasprzak, P. R. Mahaffy, T. C. Owen, N. W. Spencer, S. H. Way | title=The Galileo Probe Mass Spectrometer: Composition of Jupiter's Atmosphere | journal=Science | year=[[1996]] | volume=272 | issue=5263 | pages=846-849 | url=http://adsabs.harvard.edu/abs/1996Sci...272..846N | accessdate=2007-02-19 }}</ref>This depletion may be a result of the ice that carried heavier elements into Jupiter during its formation being still too warm to hold all of its nebular neon (this requires temperatures below 17&nbsp;Kelvins). Abundances of heavier inert gases in Jupiter's atmosphere are about 2 to 3 times solar abundance. 
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|width="30%"|North pole declination (δ)||align="right" width="30%"|64.49°
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Based on [[spectroscopy]], [[Saturn]] is thought to have a quite similar composition to Jupiter, but [[Uranus]] and [[Neptune]] have relatively much less hydrogen and helium.<ref>{{cite web | author=A. P. Ingersoll, H. B. Hammel, T. R. Spilker, R. E. Young | url = http://www.lpi.usra.edu/opag/outer_planets.pdf | format=PDF | title = Outer Planets: The Ice Giants | publisher = Lunar & Planetary Institute | accessdate = 2007-02-01
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|width="30%"|Obliqutiy of ecliptic||align="right" width="30%"|2.22°
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}}</ref> However, because of the lack of atmospheric entries probes, high quality abundance numbers of the heavier elements are lacking for the other outer planets (besides Jupiter).
 
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===Mass===
 
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[[Image:Jupiter-Earth-Spot_comparison.jpg|thumb|left|Approximate size comparison of Earth and Jupiter, including the [[Great Red Spot]]]]
 
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Jupiter is 2.5 times more [[mass]]ive than all the other planets in our solar system combined; so massive that its [[Center of mass#Barycenter|barycenter]] with the Sun actually lies above the Sun's surface (1.068&nbsp;[[solar radius|solar radii]] from the Sun's center). Although this planet dwarfs the Earth (with a diameter 11 times as great) it is considerably less dense. A volume equal to 1,317 Earths only contains 318 times as much mass.<ref name="worldbook" /><ref name="burgess">{{cite book  | first=Eric | last=Burgess | year=[[1982]] | title=By Jupiter: Odysseys to a Giant | publisher=Columbia University Press | location=New York | id=ISBN 0-231-005176-X }}</ref>
 
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[[Extrasolar planet]]s have been discovered with much greater masses. There is no clear-cut definition of what distinguishes a large planet such as Jupiter from a [[brown dwarf]] star, although the latter possesses rather specific [[spectral line]]s. Currently, if an object of solar [[metallicity]] is 13 Jupiter masses or above, large enough to burn [[deuterium]], it is categorized as a brown dwarf; below that mass (and orbiting a star or stellar remnant), it is a planet.<ref>{{cite web | title=Working Group on Extrasolar Planets: Definition of a "Planet" | work=IAU position statement |date=[[February 28]], [[2003]] | url=http://www.dtm.ciw.edu/boss/definition.html | accessdate=2006-09-09}}</ref> Jupiter is thought to have about as large a diameter as a planet of its composition can; adding extra mass would cause the planet to shrink because of increased gravitational compression. The process of further shrinkage with increasing mass would continue until [[Nuclear fusion|stellar ignition]] is achieved.<ref name="tristan286">{{cite journal | last = Guillot | first = Tristan | title=Interiors of Giant Planets Inside and Outside the Solar System | journal=Science | year=[[1999]] | volume=286 | issue=5437 | pages=72-77 | url=http://www.sciencemag.org/cgi/content/full/286/5437/72 }}</ref> This has led some astronomers to term it a "failed star". Although Jupiter would need to be about seventy-five times as massive to become a [[star]], the smallest [[red dwarf]] is only about 30% larger in radius than Jupiter.<ref>{{cite journal | author = A. Burrows, W. B. Hubbard, D. Saumon, J. I. Lunine | title=An expanded set of brown dwarf and very low mass star models | journal=Astrophysical Journal | year=[[1993]] | volume=406 | issue=1 | pages=158-171 | url=http://adsabs.harvard.edu/abs/1993ApJ...406..158B }}</ref><ref>{{cite news | first=Didier | last=Queloz |title=VLT Interferometer Measures the Size of Proxima Centauri and Other Nearby Stars | publisher=European Southern Observatory | date=[[November 19]], [[2002]] | url=http://www.eso.org/outreach/press-rel/pr-2002/pr-22-02.html | accessdate=2007-01-12 }}</ref>
 
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In spite of this, Jupiter still radiates more heat than it receives from the Sun. The amount of heat produced inside the planet is nearly equal to the total solar radiation it receives.<ref name="elkins-tanton">{{cite book | first=Linda T. | last=Elkins-Tanton | year=[[2006]] | title=Jupiter and Saturn | publisher=Chelsea House | location=New York | id=ISBN 0-8160-5196-8 }}</ref> This additional heat radiation is generated by the [[Kelvin-Helmholtz mechanism]] through [[adiabatic]] contraction. This process results in the planet shrinking by about 2&nbsp;cm each year.<ref>{{cite book | editor=F. Bagenal, T. E. Dowling, W. B. McKinnon | author=T. Guillot, D. J. Stevenson, W. B. Hubbard, D. Saumon | year=[[2004]] | title=Jupiter: The Planet, Satellites and Magnetosphere | chapterurl= http://www.gps.caltech.edu/faculty/stevenson/pdfs/guillot_etal'04.pdf | chapter=Chapter 3: The Interior of Jupiter | publisher=Cambridge University Press | id=ISBN 0521818087 }}</ref> When it was first formed, Jupiter was much hotter and was about twice its current diameter.<ref>{{cite journal | last = Bodenheimer | first = P. | title=Calculations of the early evolution of Jupiter | journal=Icarus | year=[[1974]] | volume=23 | pages=319-325 | url=http://adsabs.harvard.edu/abs/1974Icar...23..319B | accessdate=2007-02-01 }}</ref>
 
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===Internal structure===
 
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There is still some uncertainty regarding the interior structure of Jupiter. One model shows a homogeneous model with no solid surface; the density may simply increase gradually toward the core. Alternatively Jupiter may possess a dense, [[Rock (geology)|rock]]y [[planetary core|core]] with a mass of up to twelve times the Earth's total mass; roughly 3% of the total mass.<ref>{{cite journal | author=T. Guillot, D. Gautier, W. B. Hubbard | title=New Constraints on the Composition of Jupiter from Galileo Measurements and Interior Models | journal=Icarus | year=[[1997]] | volume=130 | pages=534-539 | url=http://adsabs.harvard.edu/abs/1997astro.ph..7210G }}</ref><ref name="elkins-tanton" /> The core region is surrounded by dense [[metallic hydrogen]], which extends outward to about 78% of the radius of the planet.<ref name="elkins-tanton" /> Above lies a transparent interior atmosphere of [[phase (matter)|liquid]] hydrogen and [[gas]]eous hydrogen, with the gaseous portion extending downward from the cloud layer to a depth of about 1,000&nbsp;km.<ref name="elkins-tanton" /> There may be no clear boundary or surface between these different phases of hydrogen; the conditions blend smoothly from gas to liquid as one descends.<ref>{{cite journal | last = Guillot | first = T. | title=A comparison of the interiors of Jupiter and Saturn | journal=Planetary and Space Science | year=[[1999]] | volume=47 | issue=10-11 | pages=1183-1200 | url=http://adsabs.harvard.edu/abs/1999astro.ph..7402G }}</ref><ref name="lang03">{{cite web | last = R. Lang | first = Kenneth | year = [[2003]] | url = http://ase.tufts.edu/cosmos/view_chapter.asp?id=9&page=3 | title = Jupiter: a giant primitive planet | publisher = NASA | accessdate = 2007-01-10 }}</ref>
 
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The temperature and pressure inside Jupiter increase steadily toward the core. At the layer at which hydrogen transitions to metallic, the temperature is believed to be 10,000&nbsp;K and the pressure is 200&nbsp;[[Pascal (unit)|gPa]]. The temperature at the core boundary is estimated to be 36,000&nbsp;K and the interior pressure is roughly 3,000&ndash;4,500 gPa.<ref name="elkins-tanton" />
 
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===Cloud layers===
 
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{{seealso|Cloud pattern on Jupiter}}
 
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[[Image:PIA02863 - Jupiter surface motion animation.gif|left|thumb|250 px|This looping animation shows the movement of Jupiter's counter-rotating cloud bands. In this image, the planet's exterior is mapped onto a cylindrical projection.]]
 
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Jupiter is perpetually covered with clouds composed of [[ammonia]] crystals and possibly ammonium hydrosulphide. The clouds are located in the [[tropopause]] and are arranged into bands of different [[latitude]]s, known as tropical regions. These are sub-divided into lighter-hued ''zones'' and darker ''belts''. The interactions of these conflicting [[Atmospheric circulation|circulation]] patterns cause storms and [[turbulence]]. [[Wind speed]]s of 100&nbsp;m/s (360&nbsp;km/hr) are common in zonal jets.<ref>{{cite web | author=A. P. Ingersol, T. E. Dowling, P. J. Gierasch, G. S. Orton, P. L. Read, A. Sanchez-Lavega, A. P. Showman, A. A. Simon-Miller, A. R. Vasavada | url = http://www.lpl.arizona.edu/~showman/publications/ingersolletal-2004.pdf | format=PDF | title = Dynamics of Jupiter’s Atmosphere | publisher = Lunar & Planetary Institute | accessdate = 2007-02-01 }}</ref> The zones have been observed to vary in width, color and intensity from year to year, but they have remained sufficiently stable for astronomers to give them identifying designations.<ref name="burgess" /> (See [[cloud pattern on Jupiter]].)
 
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The cloud layer is only about 50&nbsp;km deep, and consists of at least two decks of clouds: a thick lower deck and a thin clearer region. There may also be a thin layer of water clouds underlying the ammonia layer, as evidence by flashes of [[lightning]] detected in the atmosphere of Jupiter.<ref name="elkins-tanton" /> These electrical discharges can be up to a thousand times as powerful as lightning on the Earth.<ref>{{cite web | editor=Susan Watanabe | date = [[February 25]], [[2006]] | url = http://www.nasa.gov/vision/universe/solarsystem/galileo_end.html | title = Surprising Jupiter: Busy Galileo spacecraft showed jovian system is full of surprises | publisher = NASA | accessdate = 2007-02-20 }}</ref>
 
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The orange and brown coloration in the clouds of Jupiter are caused by upwelling compounds that change color when they are exposed to [[ultraviolet]] light from the Sun. The exact ingredients remain uncertain, but they are believed to be compounds of phosphorus, sulfur or possibly hydrocarbons.<ref>{{cite conference | author=P. D. Strycker, N. Chanover, M. Sussman, A. Simon-Miller | title = A Spectroscopic Search for Jupiter's Chromophores | booktitle = DPS meeting #38, #11.15 | publisher = American Astronomical Society | year = [[2006]] | url = http://adsabs.harvard.edu/abs/2006DPS....38.1115S | accessdate = 2007-02-20 }}</ref><ref name="elkins-tanton" /> These colorful compounds, known as [[chromophore]]s, mix with the warmer, lower deck of clouds. The zones are formed when rising convection cells form crystallizing ammonia that masks out these lower clouds from view.<ref name="worldbook" />
 
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Jupiter's low [[obliquity]] means that the poles constantly receive less [[solar radiation]] than at the planet's [[equator]]ial region. Internal [[convection]] processes transport more energy to the poles, however, balancing out the surface temperature across the planet.<ref name="burgess" />
 
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The only spacecraft to have descended into Jupiter's atmosphere and take scientific measurements is the ''[[Galileo spacecraft|Galileo]]'' probe (see [[#Galileo mission|Galileo mission]]). It sent an atmospheric probe into Jupiter upon arrival in 1995, then itself entered Jupiter's atmosphere and burned up in 2003.
 
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===Great Red Spot===
 
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{{main|Great Red Spot}}
 
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[[Image:Redspot.jpg|thumbnail|250px|This dramatic view of Jupiter's Great Red Spot and its surroundings was obtained by [[Voyager 1]] on February 25, 1979, when the spacecraft was 9.2&nbsp;million&nbsp;km (5.7&nbsp;million&nbsp;miles) from Jupiter. Cloud details as small as 160&nbsp;km (100&nbsp;miles) across can be seen here. The colorful, wavy cloud pattern to the left of the Red Spot is a region of extraordinarily complex and variable wave motion. To give a sense of Jupiter's scale, the white oval storm directly below the Great Red Spot is approximately the same diameter as Earth. ]]
 
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The best known feature on Jupiter is the '''[[Great Red Spot]]''', a persistent [[anticyclone|anticyclonic]] [[storm]] located 22° south of the equator that is larger than Earth. It has lasted from at least 1831,<ref>{{cite journal | last=Denning | first=W. F. | title=Jupiter, early history of the great red spot on | journal=Monthly Notices of the Royal Astronomical Society | year=[[1899]] | volume=59 | pages=574-584 | url=http://adsabs.harvard.edu/abs/1899MNRAS..59..574D | accessdate=2007-02-09 }}</ref> and possibly since 1665.<ref name="kyrala26">{{cite journal | last = Kyrala | first = A. | title=An explanation of the persistence of the Great Red Spot of Jupiter | journal=Moon and the Planets | year=[[1982]] | volume=26 | pages=105-107 | url=http://adsabs.harvard.edu/abs/1982M&P....26..105K }}</ref> [[Mathematical model]]s suggest that the storm is stable and may be a permanent feature of the planet.<ref>{{cite journal |url=http://adsabs.harvard.edu/abs/1988Natur.331..689S |title=Laboratory simulation of Jupiter's Great Red Spot |first=Jöel |last=Sommeria |coauthors=Steven D. Meyers & Harry L. Swinney |journal=Nature |volume=331 |pages=689-693 |month=25 February |year=[[1988]] }}</ref>  The storm is large enough to be visible through Earth-based [[telescope]]s.
 
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The [[oval]] object [[rotation|rotates]] [[counterclockwise]], with a [[periodicity|period]] of about 6 days.<ref>{{cite web | author=C. Y. Cardall, S. J. Daunt | url = http://csep10.phys.utk.edu/astr161/lect/jupiter/redspot.html | title = The Great Red Spot | publisher = University of Tennessee | accessdate = 2007-02-02 }}</ref> The Great Red Spot's [[dimension]]s are 24&ndash;40,000&nbsp;km × 12&ndash;14,000&nbsp;km. It is large enough to contain two or three planets of Earth's diameter.<ref>{{cite web | url = http://www.space.com/scienceastronomy/solarsystem/jupiter-ez.html | title = Jupiter Data Sheet | publisher = Space.com | accessdate = 2007-02-02 }}</ref> The tops of this storm is about 8&nbsp;km above the surrounding cloudtops.<ref>{{cite web | first=Tony | last=Phillips | date = [[March 3]], [[2006]] | url=http://science.nasa.gov/headlines/y2006/02mar_redjr.htm | title=Jupiter's New Red Spot | publisher=NASA | accessdate=2007-02-02 }}</ref>
 
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Storms such as this are not uncommon within the [[turbulent]] [[celestial body atmosphere|atmospheres]] of [[gas giant]]s. Jupiter also has white ovals and brown ovals, which are lesser unnamed storms. White ovals tend to consist of relatively [[heat|cool]] clouds within the upper atmosphere. Brown ovals are warmer and located within the "normal cloud layer". Such storms can last hours or [[century|centuries]].
 
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Before the Voyager missions, astronomers were uncertain of the nature of Jupiter's Great Red Spot. Many believed it to be either a solid or a liquid feature on the planet's surface as this appears consistent with the observable turbulence patterns.<ref>{{cite web | url = http://spacephysics.ucr.edu/index.php?content=v25/v4.html | title = Grand Tour of the Outer Planets &mdash; Jupiter | publisher = UCR Space Physics | accessdate = 2007-02-02 }}</ref> However, even before Voyager proved that the feature was a storm, there was strong evidence that the spot cannot be associated with any deeper feature on the planet's surface, as the Spot rotates differentially with respect to the rest of the atmosphere, sometimes faster and sometimes more slowly. During its recorded history it has traveled several times around the planet with regard to any possible fixed rotational marker below it.
 
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In 2000, several smaller storms located near to the Giant Red Spot were observed to merge and form a larger spot named [[Oval BA]], which increasing in intensity and changed colour from white to red.<ref>{{cite web |url=http://science.nasa.gov/headlines/y2006/02mar_redjr.htm |title=Jupiter's New Red Spot |year=[[2006]]
 
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|accessdate=2006-03-09}}</ref><ref>{{cite web | first=Bill  | last=Steigerwald |date = [[October 14]], [[2006]] | url = http://www.nasa.gov/centers/goddard/news/topstory/2006/little_red_spot.html | title = Jupiter's Little Red Spot Growing Stronger | publisher = NASA | accessdate = 2007-02-02 }}</ref> The resulting storm was named Oval BA, but gained the nickname Red Spot Junior.<ref>{{cite web | last = Goudarzi | first = Sara | date = [[May 4]], [[2006]] | url = http://www.usatoday.com/tech/science/space/2006-05-04-jupiter-jr-spot_x.htm | title = New storm on Jupiter hints at climate change | publisher = USA Today | accessdate = 2007-02-02 }}</ref> Further investigations using spectroscopy have been delayed because of the movement of Jupiter behind the Sun and it is yet to be verified if the phenomena is caused by increased wind speed, comparable to the 400 mph speeds in the larger anomaly, drawing similar materials from deeper in the atmosphere and exposing them to sunlight.
 
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<div style="clear: both"></div>
 
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===Planetary rings===
 
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[[Image:PIA01627 Ringe.jpg|thumb|right|The rings of Jupiter.]]
 
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{{main|Rings of Jupiter}}
 
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Jupiter has a faint [[planetary ring]] system composed of three main segments: an inner [[torus]] of particles known as the [[halo]], a relatively bright main ring, and an outer "gossamer" ring.<ref>{{cite journal | last = Showalter | first =  M.A. | coauthors = J.A. Burns, J. N. Cuzzi, and J. B. Pollack | title=Jupiter's ring system: New results on structure and particle properties | url=http://adsabs.harvard.edu/abs/1987Icar...69..458S | journal=Icarus | year=[[1987]] | volume=69 | issue=3 | pages=458-498 | doi = 10.1016/0019-1035(87)90018-2 }}</ref> These rings appear to be made of dust, rather than ice as is the case for Saturn's rings.<ref name="elkins-tanton" /> The main ring is probably made of material ejected from the satellites [[Adrastea (moon)|Adrastea]] and [[Metis (moon)|Metis]]. Material that would normally fall back to the moon is pulled into Jupiter because of its strong gravitational pull. The orbit of the material veers towards Jupiter and new material is added by additional impacts.<ref>{{cite journal | title=Tiny moon source of Jupiter's Ring | journal=Science | year=[[1998]] | volume=281 | issue=5385 | pages=1951 | doi = 10.1126/science.281.5385.1951b}}</ref>  In a similar way, the moons [[Thebe (moon)|Thebe]] and [[Amalthea (moon)|Amalthea]] probably produce the two distinct components of the gossamer ring.<ref>{{cite journal | last = Burns | first =  J.A. | coauthors = M. A. Showalter, D.P. Hamilton, P.D. Nicholson, I. de Pater, M. E. Ockert-Bell, and P. C. Thomas| title=The formation of Jupiter's faint rings | journal=Science | year=[[1999]] | volume=284 | issue=5417 | pages=1146-1150 | doi = 10.1126/science.284.5417.1146}}</ref>
 
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===Magnetosphere===
 
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{{main|Jupiter's magnetosphere}}
 
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Jupiter's broad magnetic field is 14 times as strong as the Earth's, ranging from 4.2&nbsp;[[gauss (unit)|gauss]] at the equator to 10&ndash;14 gauss at the poles, making it the strongest in the solar system (with the exception of [[sunspot]]s.)<ref name="worldbook" /> This field is believed to be generated by [[eddy current]]s within the metallic hydrogen core. The field traps a sheet of [[plasma]] particles from the [[solar wind]], generating a highly energetic magnetosphere. Electrons from this plasma sheet ionize the torus of [[sulfur dioxide]] generated by the [[tectonics|tectonic]] activity on the moon Io. Hydrogen particles from Jupiter's atmosphere are also trapped in the magnetosphere. Electrons within the magnetosphere generate a strong radio signature that produces bursts in the range of 0.6&ndash;30&nbsp;[[hertz|GHz]].<ref>{{cite news | title=Jupiter's Magnetosphere | publisher=The Astrophysics Spectator | date=[[November 24]], [[2004]] | url=http://www.astrophysicsspectator.com/topics/planets/JupiterMagnetosphere.html | accessdate=2006-05-24 }}</ref>
 
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At about 75 Jupiter radii from the planet, the interaction of the magnetosphere with the [[solar wind]] generates a [[bow shock]]. Surrounding Jupiter's magnetosphere is a [[magnetopause]], located at the inner edge of a [[magnetosheath]], where the planet's magnetic field becomes weak and disorganized. The solar wind interacts with these regions, elongating the magnetosphere on the side away from the Sun and extending it outward until nearly it reaches the orbit of Saturn. The four largest moons of Jupiter all orbit within the magnetosphere, which protects them from the solar wind.<ref name="elkins-tanton" />
 
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[[Image: Jupiter.Aurora.HST.UV.jpg|left|250px|thumb|[[Aurora borealis]] on Jupiter. The three brightest regions are created by tubes of magnetic flux that connect to the Jovian moons Io, Ganymede and Europa.]]
 
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The magnetosphere of Jupiter is responsible for intense episodes of [[radio]] emission from the planet's polar regions. Volcanic activity on the Jovian moon [[Io]] (see below) injects gas into Jupiter's magnetosphere, producing a torus of particles about the planet. As Io moves through this torus, the interaction generates [[Alfven wave]]s that carry ionized matter into the polar regions of Jupiter. As a result, radio waves are generated through a [[cyclotron]] [[Astrophysical maser|maser mechanism]], and the energy is transmitted out along a cone-shaped surface. When the Earth intersects this cone, the radio emissions from Jupiter can exceed the solar radio output.<ref>{{cite web | date = [[February 20]], [[2004]] | url = http://science.nasa.gov/headlines/y2004/20feb_radiostorms.htm | title = Radio Storms on Jupiter | publisher = NASA | accessdate = 2007-02-01 }}</ref>
 
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==Orbit and rotation==
 
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The average distance between Jupiter and the Sun is 778 million&nbsp;km (about 5.2 times the average distance from the Earth to the Sun) and it completes an orbit every 11.86&nbsp;years. The elliptical orbit of Jupiter is inclined 1.31&deg; compared to the Earth. Because of an [[eccentricity]] of 0.048, the distance from Jupiter and the
 
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Sun varies by 75 million&nbsp;km between [[perihelion]] and [[aphelion]], or the nearest and most distant points of the planet along the orbital path respectively.
 
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The axial tilt of Jupiter is relatively small: only 3.13&deg;. As a result this planet does not experience significant [[season]]al changes, in contrast to Earth and Mars for example.<ref>{{cite web | url = http://science.nasa.gov/headlines/y2000/interplanetaryseasons.html | title = Interplanetary Seasons | publisher = Science@NASA | accessdate = 2007-02-20 }}</ref>
 
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Jupiter's [[rotation]] is the solar system's fastest, completing a rotation on its [[Coordinate axis|axis]] in slightly less than ten hours; this creates an [[equatorial bulge]] easily seen through an Earth-based amateur [[telescope]]. This rotation produces a [[centripetal acceleration]] at the equator that results is a net acceleration of 23.12&nbsp;m/s<sup>2</sup>, compared to the equatorial surface gravity of 24.79&nbsp;m/s<sup>2</sup>. The planet is shaped as an [[oblate]] spheroid, meaning that the [[diameter]] across its [[equator]] is longer than the diameter measured between its [[geographic pole|poles]]. On Jupiter, the equatorial diameter is 9275&nbsp;km longer than the diameter measured through the poles.<ref name="lang03" />
 
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Because Jupiter is not a solid body, its upper atmosphere undergoes [[differential rotation]]. The rotation of Jupiter's [[polar region|polar]] atmosphere is ~5&nbsp;minutes longer than that of the [[equator]]ial atmosphere; three "systems" are used as frames of reference, particularly when graphing the motion of atmospheric features. System I applies from the latitudes 10º&nbsp;N to 10º&nbsp;S; its period is the planet's shortest, at 9h 50m 30.0s. System II applies at all latitudes north and south of these; its period is 9h 55m 40.6s. System III was first defined by [[radio astronomy|radio astronomers]], and corresponds to the rotation of the planet's [[magnetosphere]]; its period is Jupiter's "official" rotation.<ref>{{cite book | first=Ian | last=Ridpath | year=[[1998]] | title=Norton's Star Atlas | edition=19th ed. | publisher=Prentice Hall | id=ISBN 0582356555 }}</ref>
 
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==Observation==
 
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Jupiter is usually the fourth brightest object in the sky (after the Sun, the [[Moon]] and [[Venus]]);<ref name="worldbook">{{cite web | author=Peter J. Gierasch, Philip D. Nicholson | year = [[2004]] | url = http://www.nasa.gov/worldbook/jupiter_worldbook.html | title = Jupiter | publisher = World Book @ NASA | accessdate = 2006-08-10 }}</ref> however at times [[Mars]] appears brighter than Jupiter. Depending on Jupiter's position with respect to the Earth, it can vary in visual magnitude from as high as -2.9 at [[Opposition (astronomy)|opposition]] down to -1.6 during [[Conjunction (astronomy)|conjunction]] with the Sun. The [[angular diameter]] of Jupiter likewise varies from 47.1 to 30.6 [[arc second]]s.<ref>{{cite web | last = Espenak | first = Fred | date = [[July 25]], [[1996]] | url = http://sunearth.gsfc.nasa.gov/eclipse/TYPE/preface.html | title = NASA Reference Publication 1349&mdash;Twelve Year Planetary Ephemeris: 1995 - 2006 | publisher = NASA | accessdate = 2006-08-10 }}</ref>
 
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[[Image:Retrogadation1.png|right|thumb|Retrograde motion of a planet caused by its relative location with the Earth.]]
 
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Earth overtakes Jupiter every 398.9 days as it orbits the Sun, a duration called the [[synodic period]]. As it does so, Jupiter appears to undergo [[Retrograde and direct motion|retrograde motion]] with respect to the background stars. That is, for a period of time Jupiter seems to move backward in the night sky, forming a graceful looping motion.
 
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Jupiter's orbital period of approximately 12 years is, not uncoincidentally, also equal to the number of star [[constellation]]s in the [[zodiac]].<ref name="burgess" /> As a result, each time Jupiter reaches opposition it has advanced eastward by about the width of a zodiac constellation. The orbital period of Jupiter is also about two-thirds the orbital period of Saturn, forming a 5:2 [[orbital resonance]] between the two largest planets in the Solar System.
 
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Because the orbit of Jupiter is outside the Earth's, the [[phase angle]] of Jupiter as viewed from the Earth never exceeds 11.5&deg;, and is almost always close to 100%. That is, the planet always appears nearly fully illuminated when viewed through Earth-based telescopes. It was only during spacecraft missions to Jupiter that crescent views of
 
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the planet were obtained.<ref>{{cite web | year=[[1974]] | url = http://history.nasa.gov/SP-349/ch8.htm | title = Encounter with the Giant | publisher = NASA | accessdate = 2007-02-17 }}</ref>
 
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−
==Studies of Jupiter==
 
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The planet Jupiter has been known since ancient times and is visible to the naked eye in the night sky. To the [[Babylon]]ians, this object represented their god [[Marduk]]. They used the roughly 12-year orbit of this planet along the [[ecliptic]] to define the [[constellation]]s of the [[zodiac]].<ref name="burgess" /> The [[Ancient Rome|Romans]] named the planet after the [[Roman mythology|Roman god]] [[Jupiter (mythology)|Jupiter]] (also called Jove). The [[astronomical symbol]] for the planet is a stylized representation of the god's lightning bolt. (&#9795; is found at [[Unicode]] position U+2643.) The Greeks called it Φαέθων, ''Phaethon'', "blazing".
 
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The [[China|Chinese]], [[Korea]]n, [[Japan]]ese, and [[Vietnam]]ese refer to the planet as the ''wood star'', 木星,<ref>{{cite web
 
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|url=http://www.crystalinks.com/jupiter.html
 
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|title=JUPITER
 
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|accessdate=2006-03-09}}</ref> based on the Chinese [[Five elements (Chinese philosophy)|Five Elements]]. In [[Jyotisha|Vedic Astrology]], Hindu astrologers refer to Jupiter as [[Brihaspati]], or "[[Guru]]" which means the "Big One".<ref>{{cite web | url = http://www.webonautics.com/mythology/guru_jupiter.html | title = Guru | publisher = Indian Divinity.com | accessdate = 2007-02-14 }}</ref> In [[Hindi]], Thursday is referred to as ''[[Guruvaar]]'' (day of Jupiter). In the [[English language]] Thursday is rendered as Thor's day, with [[Thor]] being identified with the Roman god Jupiter.<ref>{{cite journal | last = Falk | first = Michael | title=Astronomical Names for the Days of the Week | journal=Journal of the Royal Astronomical Society of Canada | year=[[1999]] | volume=93 | pages=122-133 | url=http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1999JRASC..93..122F | accessdate=2007-02-14 }}</ref>
 
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===Ground-based telescope research===
 
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In 1610, [[Galileo Galilei]] discovered the four largest [[natural satellite|moons]] of Jupiter, [[Io (moon)|Io]], [[Europa (moon)|Europa]], [[Ganymede (moon)|Ganymede]] and [[Callisto (moon)|Callisto]] (now known as the [[Galilean moon]]s) using a telescope, the first observation of moons other than Earth's. This was also the first discovery of a [[celestial mechanics|celestial motion]] not apparently centered on the Earth. It was a major point in favor of [[Nicolaus Copernicus|Copernicus]]' [[heliocentrism|heliocentric]] theory of the motions of the planets; Galileo's outspoken support of the Copernican theory placed him under the threat of the [[Inquisition]].<ref>{{cite web | last =  S. Westfall | first = Richard | url = http://galileo.rice.edu/Catalog/NewFiles/galilei_gal.html | title = Galilei, Galileo | publisher = The Galileo Project | accessdate = 2007-01-10 }}</ref>
 
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During 1660's, Cassini used a new telescope to discover spots and colorful bands on Jupiter and observed that the planet appeared oblate; that is, flattened at the poles. He was also able to estimate the rotation period of the planet.<ref name=
 
−
"cassini">{{cite web | author=J. J. O'Connor, E. F. Robertson | date = [[April]], [[2003]] | url = http://www-history.mcs.st-andrews.ac.uk/Biographies/Cassini.html | title = Giovanni Domenico Cassini | publisher = University of St. Andrews | accessdate = 2007-02-14 }}</ref> In 1690 Cassini noticed that the atmosphere undergoes [[differential rotation]].<ref name="elkins-tanton" />
 
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[[Image:Jupiter from Voyager 1.jpg|thumb|240px|right|[[False-color]] detail of Jupiter's atmosphere, imaged by ''[[Voyager 1]]'', showing the [[Great Red Spot]] and a passing white oval.]]
 
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The [[Great Red Spot]], a prominent oval-shaped feature in the southern hemisphere of Jupiter, may have been observed as early as 1664 by [[Robert Hooke]] and in 1665 by [[Giovanni Domenico Cassini|Giovanni Cassini]], although this is disputed. The pharmacist [[Samuel Heinrich Schwabe|Heinrich Schwabe]] produced the earliest known drawing to show details of the Great Red Spot in 1831.<ref>{{cite book | first=Paul | last=Murdin | year=[[2000]] | title=Encyclopedia of Astronomy and Astrophysics | publisher=Institute of Physics Publishing | location=Bristol | id=ISBN 0122266900 }}</ref>
 
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The Red Spot was reportedly lost from sight on several occasions between 1665 and 1708 before becoming quite conspicuous in 1878. It was recorded as fading again in 1883 and at the start of the 20th century.<ref>{{cite web | date = [[August]] [[1974]] | url = http://history.nasa.gov/SP-349/ch1.htm | title = SP-349/396 Pioneer Odyssey&mdash;Jupiter, Giant of the Solar System. | publisher = NASA | accessdate = 2006-08-10 }}</ref>
 
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Both [[Giovanni Alfonso Borelli|Giovanni Borelli]] and Cassini made careful tables of the motions of the Jovian moons, allowing prections of the times when the moons would pass before or behind the planet. By the 1670s, however, it was observed that when Jupiter was on the opposite side of the Sun from the Earth, these events would occur about 17&nbsp;minutes later than expected. [[Ole Roemer]] deduced that sight is not instantaneous (a finding that Cassini had earlier rejected<ref name="cassini" />), and this timing discrepancy was used to estimate the [[speed of light]].<ref>{{cite web | url = http://www.mathpages.com/home/kmath203/kmath203.htm | title = Roemer's Hypothesis | publisher = MathPages | accessdate = 2007-01-12 }}</ref>
 
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In 1892, [[E. E. Barnard]] observed a fifth satellite of Jupiter with the 36-inch refractor at [[Lick Observatory]] in California. The discovery, a testament to his extraordinary eyesight, made him quickly famous. The moon was later named [[Amalthea (moon)|Amalthea]].<ref>{{cite web | first = Joe | last = Tenn | date = [[March 10]], [[2006]] | url = http://www.phys-astro.sonoma.edu/BruceMedalists/Barnard/ | title = Edward Emerson Barnard | publisher = Sonoma State University | accessdate = 2007-01-10 }}</ref> An additional eight satellites were subsequently discovered prior to the fly-by of the [[Voyager 1]] probe in 1979.
 
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In 1932, [[Rupert Wildt]] identified absorbtion bands of ammonia and methane in the spectra of Jupiter.<ref>{{cite journal | last = Dunham Jr. | first = Theodore | title=Note on the Spectra of Jupiter and Saturn | journal=Publications of the Astronomical Society of the Pacific | year=[[1933]] | volume=45 | pages=42-44 | url=http://adsabs.harvard.edu/abs/1933PASP...45...42D | accessdate=2007-02-18 }}</ref>
 
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Three long-lived anticyclonic features termed white ovals were observed in 1938. For several decades the remained as separate features in the atmosphere, sometimes approaching each other but never merging. Finally, two of the ovals merged in 1998, then absorbed the third in 2000.<ref>{{cite journal | author= A. Youssef, P. S. Marcus | title=The dynamics of jovian white ovals from formation to merger | journal=Icarus | year=[[2003]] | volume=162 | issue=1 | pages=74-93 | url=http://adsabs.harvard.edu/abs/2003Icar..162...74Y | accessdate=2007-04-17 }}</ref>
 
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In 1955, Bernard Burke and Kenneth Franklin detected bursts of radio signals coming from Jupiter at 22.2 MHz.<ref name="elkins-tanton" /> The period of these bursts matched the rotation of the planet, and they were able to use this information to refine the rotation rate. Radio bursts from Jupiter were found to come in two forms: long bursts (or L-bursts) lasting up to several seconds, and short bursts (or S-bursts) that had a duration of less than a hundredth of a second.<ref>{{cite web | last = Weintraub | first = Rachel A. | date = [[September 26]], [[2005]] | url = http://www.nasa.gov/vision/universe/solarsystem/radio_jupiter.html | title = How One Night in a Field Changed Astronomy | publisher = NASA | accessdate = 2007-02-18 }}</ref>
 
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Scientists discovered that there were three forms of radio signals being transmitted from Jupiter.
 
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−
* Decametric radio bursts (with a wavelength of tens of meters) vary with the rotation of Jupiter, and are influenced by interaction of Io with Jupiter's magnetic field.<ref>{{cite web | last = Garcia | first = Leonard N. | url = http://radiojove.gsfc.nasa.gov/library/sci_briefs/decametric.htm | title = The Jovian Decametric Radio Emission | publisher = NASA | accessdate = 2007-02-18 }}</ref>
 
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* Decimetric radio emission (with wavelengths measured in centimeters) was first observed by [[Frank Drake]] and Hein Hvatum in 1959.<ref name="elkins-tanton" /> The origin of this signal was from a torus-shaped belt around Jupiter's equator. This signal is caused by[[cyclotron radiation]] from electrons that are accelerated in Jupiter's magnetic field.<ref>{{cite web | author=M. J. Klein, S. Gulkis, S. J. Bolton | year=[[1996]] | url =http://deepspace.jpl.nasa.gov/technology/TMOT_News/AUG97/jupsrado.html | title=Jupiter's Synchrotron Radiation: Observed Variations Before, During and After the Impacts of Comet SL9 | publisher = NASA | accessdate = 2007-02-18 }}</ref>
 
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* Thermal radiation is produced by heat in the atmosphere of Jupiter.<ref name="elkins-tanton" />
 
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During the period July 16 to July 22, 1994, over twenty fragments from the [[comet]] [[Comet Shoemaker-Levy 9|Shoemaker-Levy&nbsp;9]] hit Jupiter's southern hemisphere, providing the first direct observation of a collision between two solar system objects. This impact provided useful data on the composition of Jupiter's atmosphere.<ref>{{cite web | last = Baalke | first = Ron | url = http://www2.jpl.nasa.gov/sl9/ | title = Comet Shoemaker-Levy Collision with Jupiter | publisher = NASA | accessdate = 2007-01-02 }}</ref><ref>{{cite news | first=Robert R. | last=Britt | title=Remnants of 1994 Comet Impact Leave Puzzle at Jupiter | publisher=space.com | date=[[August 23]], [[2004]] | url=http://www.space.com/scienceastronomy/mystery_monday_040823.html | accessdate=2007-02-20 }}</ref>
 
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===Research with space probes===
 
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{{main|Exploration of Jupiter}}
 
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Since 1973 a number of automated spacecraft have visited Jupiter. Flights to other planets within the Solar System are accomplished at a cost in [[energy]], which is described by the net change in velocity of the spacecraft, or [[delta-v]]. Reaching Jupiter
 
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from Earth requires a delta-v of 9.2&nbsp;km/s,<ref name="delta-v">{{cite web | last = Wong | first = Al |date= [[May 28]], [[1998]] | url = http://www2.jpl.nasa.gov/galileo/faqnav.html | title = Galileo FAQ - Navigation | publisher = NASA | accessdate = 2006-11-28 }}</ref> which is comparable to the 9.7&nbsp;km/s delta-v needed to reach low Earth orbit.<ref>{{cite web | last = Hirata | first = Chris | url = http://www.pma.caltech.edu/~chirata/deltav.html | title = Delta-V in the Solar System | publisher = California Institute of Technology | accessdate = 2006-11-28 }}</ref> Fortunately, [[Gravitational slingshot|gravity assists]] through planetary [[flyby]]s can be used to reduce the energy required to reach Jupiter, albeit at the cost of a significantly longer flight duration.<ref name="delta-v" />
 
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====Fly-by missions====
 
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{| class="wikitable" style="float: right; margin-right: 0px;"
 
−
|+ Fly-by missions
 
 
|-
 
|-
−
!Spacecraft
+
|width="30%"|Longitude of Sun's transit||align="right" width="30%"|157.68°
−
!Closest<br />approach
 
−
!Distance
 
 
|-
 
|-
−
|[[Pioneer 10]]
+
!bgcolor="lightsteelblue" colspan="2"|Atmospheric parameters
−
|December 3, 1973
 
−
|style="text-align: right;"|130,000&nbsp;km
 
 
|-
 
|-
−
|[[Pioneer 11]]
+
|width="30%"|Surface Pressure||align="right" width="30%"|>>10<sup>4</sup> kPa
−
|December 4, 1974
 
−
|style="text-align: right;"|34,000&nbsp;km
 
 
|-
 
|-
−
|[[Voyager 1]]
+
|width="30%"|Surface Density||align="right" width="30%"|~0.16 kg/m<sup>3</sup> at 1 bar
−
|March 5, 1979
 
−
|style="text-align: right;"|349,000&nbsp;km
 
 
|-
 
|-
−
|[[Voyager 2]]
+
|width="30%"|Scale height||align="right" width="30%"|27 km
−
|July 9, 1979
 
−
|style="text-align: right;"|570,000&nbsp;km
 
 
|-
 
|-
−
|rowspan="2"|[[Ulysses probe|Ulysses]]
+
|width="30%"|Average temperature||align="right" width="30%"|~210 K
−
|February 1992
 
−
|style="text-align: right;"|409,000&nbsp;km
 
 
|-
 
|-
−
|February 2004
+
|width="30%"|Wind speeds||align="right" width="30%"|up to 150 m/s at <30° latitude <br> up to 40 m/s else
−
|style="text-align: right;"|240,000,000&nbsp;km
 
 
|-
 
|-
−
|[[Cassini–Huygens|Cassini]]
+
!bgcolor="lightsteelblue" colspan="2"|Ecliptic position from primary*
−
|December 30, 2000
 
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|style="text-align: right;"|10,000,000&nbsp;km
 
 
|-
 
|-
−
|[[New Horizons]]
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|width="30%"|Note||align="right" width="30%"|*Elements given are from Orbiter.pdf (2016)
−
|February 28, 2007
 
−
|style="text-align: right;"|2,304,535&nbsp;km
 
 
|}
 
|}
−
[[Image:Jupiter gany.jpg|thumb|200px|right|''Voyager 1'' took this photo of the planet Jupiter on [[January 24]], [[1979]] while still more than 25&nbsp;million&nbsp;miles (40&nbsp;million&nbsp;kilometres) away. Click image for full caption.]]
 
−
Beginning in 1973, several spacecraft have performed planetary fly-by maneuvers that brought them within observation range of Jupiter. The Pioneer missions obtained the first ever close up images of Jupiter's atmosphere and several of its moons. They discovered that the radiation fields in the vicinity of the planet were much higher than expected, but managed to survive in that environment. The trajectories of these spacecraft were used to refine the mass estimates of the Jovian system. Occultations of the radio signals by the planet resulted in better measurements of Jupiter's diameter and the amount of polar flattening.<ref name="burgess" /><ref name="cosmology 101">{{cite web | last = Lasher | first = Lawrence |date= [[August 1]], [[2006]] | url = http://spaceprojects.arc.nasa.gov/Space_Projects/pioneer/PNhome.html | title = Pioneer Project Home Page | publisher = NASA Space Projects Division | accessdate = 2006-11-28 }}</ref>
 
  
−
Six years later the ''Voyager'' missions vastly improved the understanding of the [[Galilean moon]]s and discovered Jupiter's rings. They also took the first close up images of the planet's atmosphere, and confirmed that the Great Red Spot was anticyclonic. Comparison of the images showed that the Red Spot had changed hue since the Pioneer missions, turning from orange to dark brown. A torus of ionized atoms was discovered along Io's orbital path, and volcanoes were found on the moon's surface. As the spacecraft passed behind the planet, it observed flashes of lightning in the night side atmosphere.<ref name="burgess" /><ref name="voyager">{{cite web |date= [[January 14]], [[2003]] | url = http://voyager.jpl.nasa.gov/science/jupiter.html | title = Jupiter | publisher = NASA Jet Propulsion Laboratory | accessdate = 2006-11-28 }}</ref>
+
'''Jupiter''' is the 5th planet from the [[Sun]] and the largest of the planets and one of two gas giant planets in our [[Solar System]].
  
−
The next mission to encounter Jupiter, the ''Ulysses'' solar probe, performed a fly-by maneuver in order to attain a polar orbit around the Sun. During this pass the probe conducted studies on Jupiter's magnetosphere. However, since there are no cameras onboard the probe, no images were taken. A second fly-by six years later was at a much greater distance.<ref name="ulysses">{{cite web | author = K. Chan, E. S. Paredes, M. S. Ryne | year = [[2004]] | url = http://www.aiaa.org/Spaceops2004Archive/downloads/papers/SPACE2004sp-template00447F.pdf | title = Ulysses Attitude and Orbit Operations: 13+ Years of International Cooperation | format = PDF | publisher = American Institute of Aeronautics and Astronautics | accessdate = 2006-11-28 }}</ref>
+
Jupiter is an oblate spheroid, which is quite noticeable in a telescope, but, in [[Orbiter]], it is modeled as a sphere.
  
−
In 2000, the ''Cassini'' probe, ''en route'' to [[Saturn]], flew by Jupiter and provided some of the highest-resolution images ever made of the planet. On December 19, 2000, the ''Cassini'' spacecraft, captured a very low resolution image of the moon [[Himalia (moon)|Himalia]], but it was too distant to show any surface details.<ref>{{cite journal | author=C. J. Hansen, S. J. Bolton, D. L. Matson, L. J. Spilker, J.-P. Lebreton | title=The Cassini-Huygens flyby of Jupiter | url=http://adsabs.harvard.edu/abs/2004Icar..172....1H | journal=Icarus | year=[[2004]] | volume=172 | issue=1 | pages=1-8 | url=http://adsabs.harvard.edu/abs/2004Icar..172....1H | doi = 10.1016/j.icarus.2004.06.018}}</ref>
+
Jupiter is frequently used as a slingshot to boost the speed of spacecraft enroute to bodies beyond Jupiter to realize a huge savings on fuel.
  
−
The ''[[New Horizons]]'' probe, en route to [[Pluto]], will flyby Jupiter for a gravity assist. Closest approach will be February 28, 2007. While at Jupiter, New Horizon's instruments will refine the [[orbital elements]] of Jupiter's inner moons, particularly [[Amalthea (moon)|Amalthea]]. The probe's cameras will measure plasma output from volcanoes on [[Io (moon)|Io]] and study all four Galilean moons in detail.<ref>{{cite web | last = | first = | date= [[January 19]], [[2007]]  | url = http://news.bbc.co.uk/2/hi/science/nature/6279423.stm | title = New Horizons targets Jupiter kick | publisher = BBC News Online | accessdate = 2007-01-20 }}</ref> Imaging of the Jovian system began September 4, 2006.<ref>{{cite web | last = Alexander | first = Amir |date= [[September 27]], [[2006]]  |
+
== Orbital characteristics ==
−
url = http://www.planetary.org/news/2006/0927_New_Horizons_Snaps_First_Picture_of.html | title = New Horizons Snaps First Picture of Jupiter | publisher = The Planetary Society | accessdate = 2006-12-19 }}</ref>
+
Jupiter is the fifth planet from the Sun located after Mars beyond the main asteroid belt. It orbits the Sun at about 5.2 astronomical units with an eccentricity of about 0.048 and an inclincation of about 1.3°. It orbits the Sun in just under 12 years (4332 days).
  
−
====Galileo mission====
+
== Physical characteristics ==
−
[[Image:PIA04866_modest.jpg|thumb|left|Jupiter as seen by the space probe [[Cassini-Huygens|Cassini]]. This is the most detailed global color portrait of Jupiter ever assembled.]]
+
Jupiter is just under 140000 km diameter, or about 11 times that of [[Earth]], with a mass of about 1.9×10<sup>27</sup> kg, or about 317 times that of Earth.
−
So far the only spacecraft to orbit Jupiter is the ''[[Galileo spacecraft|Galileo]]'' orbiter, which went into orbit around Jupiter on December 7, 1995. It orbited the planet for over seven years, conducting multiple flybys of all of the Galilean moons and [[Amalthea (moon)|Amalthea]]. The spacecraft also witnessed the impact of [[Comet Shoemaker-Levy 9]] as it approached Jupiter in 1994, giving a unique vantage point for the event. However, while the information gained about the Jovian system from ''Galileo'' was extensive, its originally-designed capacity was limited by the failed deployment of its high-gain radio transmitting antenna.<ref name="galileo">{{cite web | last = McConnell | first = Shannon |date= [[April 14]], [[2003]] | url = http://www2.jpl.nasa.gov/galileo/ | title = Galileo: Journey to Jupiter | publisher = NASA Jet Propulsion Laboratory | accessdate = 2006-11-28 }}</ref>
 
  
−
An atmospheric probe was released from the spacecraft in July, 1995, entering the planet's atmosphere on December 7. It parachuted through 150&nbsp;km of the atmosphere, collecting data for 57.6&nbsp;minutes, before being crushed by the pressure to which it was subjected by that time (about 22 times Earth normal, at a temperature of 153&nbsp;<sup>o</sup>C).<ref>{{cite web | first = Julio | last = Magalhães | date = [[December 10]], [[1996]] | url = http://spaceprojects.arc.nasa.gov/Space_Projects/galileo_probe/htmls/probe_events.html | title = Galileo Probe Mission Events | publisher = NASA Space Projects Division | accessdate = 2007-02-02 }}</ref> It would have melted thereafter, and possibly vaporized. The ''Galileo'' orbiter itself experienced a more rapid version of the same fate when it was deliberately steered into the planet on September 21, 2003 at a speed of over 50&nbsp;km/s, in order to avoid any possibility of it crashing into and possibly contaminating [[Europa (moon)|Europa]].<ref name="galileo" />
+
== Jupiter in Orbiter ==
 +
Jupiter has been a part of Orbiter since the earliest versions. In Orbiter 2001, Jupiter's orbit was defined in the Jupiter.cfg file and had no moons. but, in Orbiter 2002 onward, its orbit was defined in the Vsop87.dll file, and the four Galilean moons were added, and has been so ever since.  A large number of moons are available as add-ons.
  
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====Future probes====
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=== Orbiter versions and add-ons which include Jupiter ===
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NASA is planning a mission to study Jupiter in detail from a [[polar orbit]]. Named ''[[Juno (spacecraft)|Juno]]'', the spacecraft is planned to launch by 2010.<ref>{{cite web | url = http://newfrontiers.nasa.gov/missions_juno.html | title = New Frontiers - Missions - Juno | publisher = NASA | accessdate = 2007-01-02 }}</ref>
+
{|class="wikitable sortable” style="text-align: center"
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|-
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Because of the possibility of a liquid ocean on Jupiter's moon [[Europa (moon)|Europa]], there has been great interest to study the icy moons in detail. A mission proposed by NASA was dedicated to study them. The [[Jupiter Icy Moons Orbiter|JIMO]] (Jupiter Icy Moons Orbiter) was expected to be launched sometime after 2012. However, the mission was deemed too ambitious and its funding was cancelled.<ref>{{cite news | first=Brian | last=Berger | title=White House scales back space plans | publisher=MSNBC | date=[[February 7]], [[2005]] | url=http://www.msnbc.msn.com/id/6928404/ | accessdate=2007-01-02 }}</ref>
+
!Add-on!!Source!!Version!!Author!!Type!!Release Date!!Compatibility!!Wiki article
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==Moons==
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|[https://www.orbiter-forum.com/resources/orbiter-2016-torrent-files.5427/ Orbiter 2016 - torrent files]||O-F Resources||2016||martins||Orbiter Download||23 August 2016||Orbiter 2016||
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{{main|Jupiter's natural satellites}}
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|-
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{{see_also|Timeline of discovery of Solar System planets and their natural satellites}}
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|[https://www.orbiter-forum.com/resources/orbiter-2016-core-msi-exe-edition.5426/ Orbiter 2016 Core - MSI / EXE edition]||O-F Resources||2016||martins||Orbiter Download||23 August 2016||Orbiter 2016||
−
Jupiter has at least 63 [[natural satellite]]s. Of these, 47 are less than 10&nbsp;kilometres in diameter and were only discovered since 1975. The four largest moons, known as the "[[Galilean moons]]", are [[Io (moon)|Io]], [[Europa (moon)|Europa]], [[Ganymede (moon)|Ganymede]] and [[Callisto (moon)|Callisto]].
+
|-
−
 
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|[https://www.orbiter-forum.com/resources/orbiter-2016-core-zip-edition.5425/ Orbiter 2016 Core - ZIP edition]||O-F Resources||2016||martins||Orbiter download||23 August 2016||Orbiter 2016||
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[[Image:Jupiter.moons2.jpg|thumb|left|300px|Jupiter's 4 Galilean moons, in a composite image comparing their sizes and the size of Jupiter ([[Great Red Spot]] visible). From the top they are: [[Callisto (moon)|Callisto]], [[Ganymede (moon)|Ganymede]], [[Europa (moon)|Europa]] and [[Io (moon)|Io]].]]
+
|-
−
===Galilean moons===
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|[http://orbit.medphys.ucl.ac.uk/download.html Orbiter core package download]<br>(The actual download page for Orbiter 2016)||Orbiter download page||Orbiter 2016||martins||Orbiter download||23 August 2016||Orbiter 2016||
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The orbits of Io, Europa, and Ganymede, the largest moons in the solar system, form a pattern known as a [[Laplace resonance]]; for every four orbits that Io makes around Jupiter, Europa makes exactly two orbits and Ganymede makes exactly one. This resonance causes the [[gravity|gravitational]] effects of the three moons to distort their orbits into elliptical shapes, since each moon receives an extra tug from its neighbors at the same point in every orbit it makes.
+
|-
−
 
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|[https://www.orbiter-forum.com/resources/celestial-bodies-motion-part-1-4-v2-0-0.132/ Celestial Bodies Motion - Part 1/4 - v2.0.0]||O-F Resources||v2.0.0||cristiapi||Scenery||2 July 2015||*module only||
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The [[tidal force]] from Jupiter, on the other hand, works to circularize their orbits.<ref>{{cite journal | author= S. Musotto, F. Varadi, W. B. Moore, G. Schubert | title=Numerical simulations of the orbits of the Galilean satellites | url=http://cat.inist.fr/?aModele=afficheN&cpsidt=13969974 | journal=Icarus | year=[[2002]] | volume=159 | pages=500-504 }}</ref> This constant tug of war causes regular flexing of the three moons' shapes, with Jupiter's gravity stretching the moons more strongly during the portion of their orbits that are closest to it and allowing them to spring back to more spherical shapes when they're farther away. This flexing causes tidal heating of the three moons' cores. This is seen most dramatically in Io's extraordinary volcanic activity, and to a somewhat less dramatic extent in the geologically young surface of Europa indicating recent resurfacing.
+
|-
−
 
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|[https://www.orbiter-forum.com/resources/orbiter-2010-p1.5428/ Orbiter 2010-P1]||O-F Resources||100830||martins||Orbiter Download||30 August 2010||Orbiter 2010-P1||
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{| class="wikitable" style="float:left"
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|-
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|- style="background:#efefef;"
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|[https://www.orbiter-forum.com/resources/orbiter-2010.5429/ Orbiter 2010]||O-F Resources||100606||martins||Orbiter Download||5 June 2010||Orbiter 2010||
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! colspan="10" | The [[Galilean moons]], compared to Earth's [[Moon]]
+
|-
 +
|[https://library.avsim.net/esearch.php?DLID=&Name=&FileName=outer_planets-060929-base.zip&Author=&CatID=root The Outer Planets 060929 Base]||AVSIM||||Rolf Keibel<br>Carl Romanik<br>Tony Dunn||Scenery||30 September 2006||Orbiter 2006-P1||
 +
|-
 +
|[https://www.orbiter-forum.com/resources/orbiter-2006-p1.5430/ Orbiter 2006-P1]||O-F Resources||060929||martins||Orbiter Download||29 September 2006||Orbiter 2006-P1||
 +
|-
 +
|[https://www.orbiter-forum.com/resources/orbiter-2006.5431/ Orbiter 2006]||O-F Resources||060504||martins||Orbiter Download||4 May 2006||Orbiter 2006||
 +
|-
 +
|[https://library.avsim.net/esearch.php?DLID=&Name=&FileName=outerplanets-050329_update.zip&Author=&CatID=root The Outer Planets 050329 Update]||AVSIM||050329||Rolf Keibel<br>Tony Dunn<br>Carl Romanik||Scenery||30 March 2005||||
 
|-
 
|-
−
|- style="background:#efefef;"
+
|[https://library.avsim.net/esearch.php?DLID=&Name=&FileName=outerplanets-050223_update.zip&Author=&CatID=root The Outer Planets 050223 Update]||AVSIM||050223||Rolf Keibel<br>Tony Dunn<br>Carol Romanik||Scenery||23 February 2005||||
−
! colspan="2" rowspan="2" | Name<br/>
 
−
([[Help:Pronunciation respelling key|Pronunciation key]])
 
−
! colspan="2" | Diameter
 
−
! colspan="2" | Mass
 
−
! colspan="2" | Orbital radius
 
−
! colspan="2" | Orbital period
 
−
|- style="background:#efefef;"
 
−
! km
 
−
! %
 
−
! kg
 
−
! %
 
−
! km
 
−
! %
 
−
! days
 
−
! %
 
−
|- style="background:#ccccff;" align="right"
 
−
| align="left" | '''[[Io (moon)|Io]]''' || align="left" | ''eye'-oe''<br>{{IPA|ˈaɪəʊ}} || 3643 || 105% || 8.9×10<sup>22</sup> || 120% ||421,700 || 110% ||1.77 || 7%
 
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|- style="background:#ccccff" align="right"
 
−
| align="left" | '''[[Europa (moon)|Europa]]''' || align="left" | ''ew-roe'-pə''<br>{{IPA|jʊˈrəʊpə}} || 3122 || 90% || 4.8×10<sup>22</sup> || 65% || 671,034 || 175% || 3.55 || 13%
 
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|- style="background:#ccccff" align="right"
 
−
| align="left" | '''[[Ganymede (moon)|Ganymede]]''' || align="left" | ''gan'-ə-meed''<br>{{IPA|ˈgænəmid}} || 5262 || 150% || 14.8×10<sup>22</sup> || 200% || 1,070,412 || 280% || 7.15 || 26%
 
−
|- style="background:#ccccff" align="right"
 
−
| align="left" | '''[[Callisto (moon)|Callisto]]''' || align="left" | ''kə-lis'-toe''<br>{{IPA|kəˈlɪstəʊ}} || 4821 || 140% || 10.8×10<sup>22</sup> || 150% || 1,882,709 || 490% || 16.69 || 61%
 
−
|}
 
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<!-- Please don't remove the following template.  It is needed for proper display. -->
 
−
{{-}}
 
−
 
 
−
===Classification of moons===
 
−
[[Image:Europa-moon.jpg|thumb|right|150px|[[Europa (moon)|Europa]], one of Jupiter's many [[natural satellite|moons]].]]
 
−
Before the discoveries of the Voyager missions, Jupiter's moons were arranged neatly into four groups of four, based on commonality of their [[orbital elements]]. Since then, the large number of new small outer moons has complicated this picture. There are now thought to be six main groups, although some are more distinct than others.
 
−
 
 
−
A basic sub-division is a grouping of the eight inner regular moons, which have nearly circular orbits near the plane of Jupiter's equator and are believed to have formed with Jupiter. The remainder of the moons consist of an unknown number of small irregular moons with elliptical and inclined orbits, which are believed to be captured asteroids or fragments of captured asteroids. Irregular moons that belong to a group share similar orbital elements and thus may have a common origin, perhaps as a larger moon or captured body that broke up.<ref>{{cite book | author=D. C. Jewitt, S. Sheppard, C. Porco | editor=F. Bagenal, T. Dowling and W. McKinnon | year=[[2004]] | title=Jupiter: The Planet, Satellites and Magnetosphere | publisher=Cambridge University Press | id=ISBN 0521818087 | url =http://www.ifa.hawaii.edu/~jewitt/papers/JUPITER/JSP.2003.pdf}}</ref><ref>{{cite journal | author=D. Nesvorný, J. L. A. Alvarellos, L. Dones, H. F. Levison | title=Orbital and Collisional Evolution of the Irregular Satellites | journal=The Astronomical Journal | year=[[2003]] | volume=126 | issue=1 | pages=398-429 | url=http://adsabs.harvard.edu/abs/2003AJ....126..398N | accessdate=2007-02-19 }}</ref>
 
−
 
 
−
{| class="wikitable"
 
−
|rowspan="2"|Regular moons
 
−
|Inner group
 
−
|The inner group of four small moons all have diameters of less than 200&nbsp;km, orbit at radii less than 200,000&nbsp;km, and have orbital inclinations of less than half a degree.
 
 
|-
 
|-
−
|[[Galilean moons|Galilean&nbsp;moons]]<ref>{{cite journal
+
|[https://library.avsim.net/esearch.php?DLID=&Name=&FileName=outerplanets-050125.zip&Author=&CatID=root The Outer Planets 050125]||AVSIM||050125||Rolf Keibel<br>Tony Dunn||Scenery||26 January 2005||Orbiter 2005-P1||
−
| title = The Galilean Satellites | author = A. P. Showman, R. Malhotra | journal = Science | year = [[1999]]
 
−
| volume = 286
 
−
| issue = 5437
 
−
| pages = 77 - 84
 
−
| doi =  10.1126/science.286.5437.77
 
−
}}</ref>
 
−
|These four moons, discovered by [[Galileo Galilei]] and by [[Simon Marius]] in parallel, orbit between 400,000 and 2,000,000&nbsp;km, and include some of the largest moons in the solar system.
 
 
|-
 
|-
−
|rowspan="6"|Irregular moons
+
|[https://www.orbiter-forum.com/resources/2005-with-p1-patch-files.5432/ 2005 (with P1 patch files)]||O-F Resources||050216||martins||Orbiter Download||16 February 2005||Orbiter 2005||
−
|[[Themisto (moon)|Themisto]]
 
−
|This is a single moon belonging to a group of its own, orbiting halfway between the Galilean moons and the next group.
 
 
|-
 
|-
−
|[[Himalia group|Himalia&nbsp;group]]
+
|[https://www.orbiter-forum.com/resources/orbiter-2003-p2.5433/ Orbiter 2003-P2]||O-F Resources||031217||martins||Orbiter Download||17 December 2003||Orbiter 2003-P2||
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|A tightly clustered group of moons with orbits around 11,000,000-12,000,000&nbsp;km from Jupiter.
 
 
|-
 
|-
−
|[[Carpo (moon)|Carpo]]
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|[https://www.orbiter-forum.com/resources/orbiter-2003-p1.5434/ Orbiter 2003-P1]||O-F Resources||031105||martins||Orbiter Download||5 November 2003||Orbiter 2003-P1|
−
|Another isolated case; at the inner edge of the Ananke group, it revolves in the direct sense.
 
 
|-
 
|-
−
|[[Ananke group|Ananke&nbsp;group]]
+
|[https://library.avsim.net/esearch.php?DLID=&Name=&FileName=jupiter_i.zip&Author=&CatID=root Jupiter I]||AVSIM||||Rolf Keibel||Scenery||25 October 2002||||
−
|This group has rather indistinct borders, averaging 21,276,000&nbsp;km from Jupiter with an average inclination of 149 degrees.
 
 
|-
 
|-
−
|[[Carme group|Carme&nbsp;group]]
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|[https://www.orbiter-forum.com/resources/orbiter-2002.5436/ Orbiter 2002]||O-F Resources||020419||martins||Orbiter Download||12 June 2022||Orbiter 2002||
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|A fairly distinct group that averages 23,404,000&nbsp;km from Jupiter with an average inclination of 165 degrees.
 
 
|-
 
|-
−
|[[Pasiphaë group|Pasiphaë&nbsp;group]]
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|[https://www.orbiter-forum.com/resources/orbiter-2001.5437/ Orbiter 2001]||O-F Resources||010503||martins||Orbiter Download||12 June 2022||Orbiter 2001||
−
|A dispersed and only vaguely distinct group that covers all the outermost moons.
 
 
|}
 
|}
  
−
==Effect on the Solar System==
+
== See also:  ==
−
Along with the Sun, the [[gravity|gravitational]] influence of Jupiter has helped shape the Solar System. The orbits of most of the system's planets lie closer to Jupiter's [[orbital plane (astronomy)|orbital plane]] than the Sun's [[celestial equator|equatorial plane]] ([[Mercury (planet)|Mercury]] is the only planet which is closer to the Sun's equator in orbital tilt), the [[Kirkwood gap]]s in the [[asteroid belt]] are mostly due to Jupiter, and the planet may have been responsible for the [[Late Heavy Bombardment]] of the inner solar system's history.<ref>{{cite journal | last = Kerr | first = Richard A. | title=Did Jupiter and Saturn Team Up to Pummel the Inner Solar System? | journal=Science | year=[[2004]] | volume=306 | issue=5702 | pages=1676 | url=http://www.sciencemag.org/cgi/content/full/306/5702/1676a?etoc }}</ref>
+
*[[w:Jupiter|Jupiter]] at Wikipedia.
−
 
 
−
[[Image:Asteroid Belt.jpg|right|thumb|This diagram shows the Trojan Asteroids in Jupiter's orbit, as well as the main [[asteroid belt]].]]
 
−
In addition to its moons, Jupiter's gravitational field controls numerous [[asteroid]]s that have settled into the regions of the [[Lagrangian point]]s preceding and following Jupiter in its orbit around the sun. These are known as the [[Trojan asteroid]]s, and are divided into [[List of Trojan asteroids (Greek camp)|Greek]] and [[List of Trojan asteroids (Trojan camp)|Trojan]] "camps" to commemorate the ''[[Iliad]]''. The first of these, [[588 Achilles]], was discovered by [[Max Wolf]] in 1906; since then hundreds more have been discovered. The largest is [[624 Hektor]].
 
−
 
 
−
Jupiter has been called the solar system's vacuum cleaner,<ref>{{cite news | first=Richard A. | last=Lovett |title=Stardust's Comet Clues Reveal Early Solar System | publisher=National Geographic News | date=[[December 15]], [[2006]] | url=http://news.nationalgeographic.com/news/2006/12/061215-comet-stardust.html | accessdate=2007-01-08 }}</ref> because of its immense [[gravity well]] and location near the inner solar system. It receives the most frequent comet impacts of the solar system's planets.<ref>{{cite journal | author=T. Nakamura, H. Kurahashi | title=Collisional Probability of Periodic Comets with the Terrestrial Planets: An Invalid Case of Analytic Formulation | journal=Astronomical Journal | year=[[1998]] | volume=115 | issue=1 | pages=848–854 | url=http://www.journals.uchicago.edu/cgi-bin/resolve?id=doi:10.1086/300206 }}</ref>
 
−
 
 
−
The majority of [[List of periodic comets|short-period comets]] belong to the Jupiter family&mdash;defined as comets with [[semi-major axis|semi-major axes]] smaller than Jupiter's. Jupiter family comets are believed to form in the [[Kuiper belt]] outside the orbit of Neptune. During close encounters with Jupiter their orbits are perturbed into a smaller period and then circularized by regular gravitational interaction with the Sun and Jupiter.<ref>{{cite journal | author=T. Quinn, S. Tremaine, M. Duncan | title=Planetary perturbations and the origins of short-period comets | journal=Astrophysical Journal, Part 1 | year=[[1990]] | volume=355 | pages=667-679 | url=http://adsabs.harvard.edu/abs/1990ApJ...355..667Q | accessdate=2007-02-17 }}</ref>
 
−
 
 
−
==Possibility of life==
 
−
It is considered highly unlikely that there is any Earth-like [[extraterrestrial life|life]] on Jupiter, as there is little water in the atmosphere and any possible solid surface deep within Jupiter would be under extraordinary pressures. However, in 1976, before the [[Voyager program|Voyager]] missions, it was hypothesized<!---What about the "sinkers"?---><ref>{{cite web
 
−
|url=http://www.daviddarling.info/encyclopedia/J/Jupiterlife.html
 
−
|title=Jupiter, life on
 
−
|publisher=Encyclopedia of Astrobiology, Astronomy & Spaceflight
 
−
|accessdate=2006-03-09}}</ref><ref>{{cite journal
 
−
| title = Particles, environments, and possible ecologies in the Jovian atmosphere
 
−
| author = C. Sagan, E. E. Salpeter
 
−
| journal = The Astrophysical Journal Supplement Series
 
−
| year = [[1976]]
 
−
| volume = 32
 
−
| issue =
 
−
| pages = 633-637
 
−
| doi = 10.1086/190414
 
−
}}</ref>
 
−
that [[ammonia]]- or [[water]]-based life could evolve in Jupiter's upper atmosphere. This hypothesis is based on the ecology of terrestrial seas which have simple [[Photosynthesis|photosynthetic]] [[plankton]] at the top level, [[fish]] at lower levels feeding on these creatures, and marine [[predator]]s which hunt the fish.
 
−
 
 
−
==See also==
 
−
* [[Aspects of Jupiter]] - for data of opposition, conjunction to sun, etc.
 
−
* [[Planets in astrology#Jupiter|Jupiter in astrology]]
 
−
* [[Jupiter in fiction]]
 
−
 
 
−
==References==
 
−
===Notes===
 
−
<div class="references-small" style="-moz-column-count:2; column-count:2;">
 
−
<references />
 
−
</div>
 
−
 
 
−
===Bibliography===
 
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* {{ cite book | editor = Bagenal, F. & Dowling, T. E. & McKinnon, W. B. | year = [[2004]] | title =Jupiter: The planet, satellites, and magnetosphere | location = Cambridge | publisher = Cambridge University Press | id=ISBN 0521818087 }}
 
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* {{ cite book | last=Beebe | first=Reta | title=Jupiter: The Giant Planet | edition=Second edition| year=[[1996]] | publisher=Smithsonian Institute Press | location=Washington, D.C. | id=ISBN 1560986859 }}
 
  
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==External links==
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== Gallery ==
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{{sisterlinks|Jupiter}}
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<gallery widths="100" heights="100">
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* [http://www.nasa.gov/worldbook/jupiter_worldbook.html Nasa - Jupiter]
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JupiterOrbiter2001.jpg|<center>Jupiter in Orbiter 2001</center>
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* [http://www.vias.org/spacetrip/jupiter_1.html A Trip Into Space] Data and photos on Jupiter
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Jupiter-jupiterizip.jpg|<center>Jupiter from ''jupiter_i.zip'' in Orbiter 2002</center>
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* [http://www.ibiblio.org//e-notes/VRML/Globe/Globe.htm 3D VRML Jupiter globe] and its satellites Io, Callisto, Europa and Ganymede
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Jupiter-orbiter2002p3.jpg|<center>Jupiter in Orbiter 2002P3</center>
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* [http://www.projectshum.org/Planets/jupiter.html Planets - Jupiter] A kid's guide to Jupiter.
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Jupiter-Orbiter2003P2.jpg|<center>Jupiter in Orbiter 2003P2</center>
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*[http://www.pbs.org/empires/medici/renaissance/galileo.html Galileo and the Medici Family]
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Jupiter-Orbiter2005P1.jpg|<center>Jupiter in Orbiter 2005P1</center>
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*[http://orbitsimulator.com/gravity/articles/joviansystem.html A simulation of the 62 Jovian moons]
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Jupiter-outerplanets050125zip-Orbiter2005P1.jpg|<center>Jupiter from ''outerplanets050125.zip'' in Orbiter 2005P1</center>
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*[http://astroclub.tau.ac.il/ephem/Jupiter/ Observing Jupiter - Position, central meridian and moons]
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Jupiter-Orbiter2006P1.jpg|<center>Jupiter in Orbiter 2006P1</center>
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*[http://skytonight.com/observing/objects/planets/3307071.html?page=2&c=y Observing Jupiter's moons]
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Jupiter-Orbiter2010P1-Orbiter2010P1.jpg|<center>Jupiter in Orbiter 2010P1</center>
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JupiterScrshot.jpg|<center>Jupiter in Orbiter 2016 with D3D9</center>
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Jupiter rotation over 3 hours with 11 inch telescope.gif|<center>Jupiter rotation over 3 hours with 11 inch telescope,<br>From Wikimedia Commons</center>
  
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{{Moons of Jupiter}}
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==Natural satellites==
 
==Natural satellites==
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Latest revision as of 03:11, 12 November 2024

Jupiter
JupiterScrshot.jpg
Jupiter in Orbiter 2016 with D3D9
Designation
Name Jupiter
Reference body Sun
Number of satellites 95
Planetary mean orbits
Epoch J2000 (1 January 2000)
Semimajor axis (a) 5.20336301 AU
(7.784120267×1011 km)
Eccentricity (e) 0.04839266
Inclination (i) 1.30530°
(0.0227818 radian)
Longitude of the ascending node (LAN, ☊) 100.55615°
(1.755036 radian)
Longitude of periapsis (ϖ) 14.75385°
(0.257503 radian)
Mean longitude (L) 34.40438°
(0.600470 radian)
Planetary orbital element centennial rates
Semimajor axis (a) 0.00060737 AU/Century
Eccentricity (e) -0.00012880 Century-1
Inclination (i) -4.15 seconds/Century
Longitude of the ascending node (LAN, ☊) 1217.17 seconds/Century
Longitude of periapsis (ϖ) 839.93 seconds/Century
Mean longitude (L) 10925078.35 seconds/Century
Selected physical parameters
Mean radius 69911.0±6 km
Mass 1.8986111×1027 kg
Density 1.326 g/m3
Sidereal rotation period 9.92425 hours
Sidereal orbit period 11.856523 years
Magnitude V(1,0) -9.4
Geometric albedo 0.52
Equatorial gravity 23.12±0.01 m/s2
Escape velocity 59.5 km/s
Rotation elements
North pole right ascension (α) 268.04°
North pole declination (δ) 64.49°
Obliqutiy of ecliptic 2.22°
Longitude of Sun's transit 157.68°
Atmospheric parameters
Surface Pressure >>104 kPa
Surface Density ~0.16 kg/m3 at 1 bar
Scale height 27 km
Average temperature ~210 K
Wind speeds up to 150 m/s at <30° latitude
up to 40 m/s else
Ecliptic position from primary*
Note *Elements given are from Orbiter.pdf (2016)

Jupiter is the 5th planet from the Sun and the largest of the planets and one of two gas giant planets in our Solar System.

Jupiter is an oblate spheroid, which is quite noticeable in a telescope, but, in Orbiter, it is modeled as a sphere.

Jupiter is frequently used as a slingshot to boost the speed of spacecraft enroute to bodies beyond Jupiter to realize a huge savings on fuel.

Orbital characteristics[edit]

Jupiter is the fifth planet from the Sun located after Mars beyond the main asteroid belt. It orbits the Sun at about 5.2 astronomical units with an eccentricity of about 0.048 and an inclincation of about 1.3°. It orbits the Sun in just under 12 years (4332 days).

Physical characteristics[edit]

Jupiter is just under 140000 km diameter, or about 11 times that of Earth, with a mass of about 1.9×1027 kg, or about 317 times that of Earth.

Jupiter in Orbiter[edit]

Jupiter has been a part of Orbiter since the earliest versions. In Orbiter 2001, Jupiter's orbit was defined in the Jupiter.cfg file and had no moons. but, in Orbiter 2002 onward, its orbit was defined in the Vsop87.dll file, and the four Galilean moons were added, and has been so ever since. A large number of moons are available as add-ons.

Orbiter versions and add-ons which include Jupiter[edit]

Add-on Source Version Author Type Release Date Compatibility Wiki article
Orbiter 2016 - torrent files O-F Resources 2016 martins Orbiter Download 23 August 2016 Orbiter 2016
Orbiter 2016 Core - MSI / EXE edition O-F Resources 2016 martins Orbiter Download 23 August 2016 Orbiter 2016
Orbiter 2016 Core - ZIP edition O-F Resources 2016 martins Orbiter download 23 August 2016 Orbiter 2016
Orbiter core package download
(The actual download page for Orbiter 2016)		 Orbiter download page Orbiter 2016 martins Orbiter download 23 August 2016 Orbiter 2016
Celestial Bodies Motion - Part 1/4 - v2.0.0 O-F Resources v2.0.0 cristiapi Scenery 2 July 2015 *module only
Orbiter 2010-P1 O-F Resources 100830 martins Orbiter Download 30 August 2010 Orbiter 2010-P1
Orbiter 2010 O-F Resources 100606 martins Orbiter Download 5 June 2010 Orbiter 2010
The Outer Planets 060929 Base AVSIM Rolf Keibel
Carl Romanik
Tony Dunn		 Scenery 30 September 2006 Orbiter 2006-P1
Orbiter 2006-P1 O-F Resources 060929 martins Orbiter Download 29 September 2006 Orbiter 2006-P1
Orbiter 2006 O-F Resources 060504 martins Orbiter Download 4 May 2006 Orbiter 2006
The Outer Planets 050329 Update AVSIM 050329 Rolf Keibel
Tony Dunn
Carl Romanik		 Scenery 30 March 2005
The Outer Planets 050223 Update AVSIM 050223 Rolf Keibel
Tony Dunn
Carol Romanik		 Scenery 23 February 2005
The Outer Planets 050125 AVSIM 050125 Rolf Keibel
Tony Dunn		 Scenery 26 January 2005 Orbiter 2005-P1
2005 (with P1 patch files) O-F Resources 050216 martins Orbiter Download 16 February 2005 Orbiter 2005
Orbiter 2003-P2 O-F Resources 031217 martins Orbiter Download 17 December 2003 Orbiter 2003-P2
Orbiter 2003-P1 O-F Resources 031105 martins Orbiter Download 5 November 2003
Jupiter I AVSIM Rolf Keibel Scenery 25 October 2002
Orbiter 2002 O-F Resources 020419 martins Orbiter Download 12 June 2022 Orbiter 2002
Orbiter 2001 O-F Resources 010503 martins Orbiter Download 12 June 2022 Orbiter 2001

See also:[edit]

Gallery[edit]

  • Jupiter in Orbiter 2001
  • Jupiter from jupiter_i.zip in Orbiter 2002
  • Jupiter in Orbiter 2002P3
  • Jupiter in Orbiter 2003P2
  • Jupiter in Orbiter 2005P1
  • Jupiter from outerplanets050125.zip in Orbiter 2005P1
  • Jupiter in Orbiter 2006P1
  • Jupiter in Orbiter 2010P1
  • Jupiter in Orbiter 2016 with D3D9
  • Jupiter rotation over 3 hours with 11 inch telescope,
    From Wikimedia Commons

Natural satellites[edit]

Jupiter's natural satellites

edit

Named Satellites:

Adrastea | Aitne | Amalthea | Ananke | Aoede | Arche | Autonoe | Callirrhoe | Callisto | Carme | Carpo | Chaldene | Cyllene | Dia | Eirene | Elara | Erinome | Ersa | Euanthe | Eukelade | Eupheme | Euporie | Europa | Eurydome | Ganymede | Harpalyke | Hegemone | Helike | Hermippe | Herse | Himalia | Io | Iocaste | Isonoe | Kale | Kallichore | Kalyke | Kore | Leda | Lysithea | Megaclite | Metis | Mneme | Orthosie | Pandia | Pasiphae | Pasithee | Philophrosyne | Praxidike | Sinope | Sponde | Taygete | Thebe | Thelxinoe | Themisto | Thyone | Valetudo

Numbered Satellites:

S/2003 J 2 | S/2003 J 4 | S/2003 J 9 | S/2003 J 10 | S/2003 J 12 | S/2003 J 16 | S/2003 J 18 | S/2003 J 19 | S/2003 J 23 | S/2003 J 24 |S/2010 J 1 | S/2010 J 2 | S/2011 J 1 | S/2011 J 2 S/2011 J 3 | S/2016 J 1 | S/2016 J 3 | S/2016 J 4 | S/2017 J 1 | S/2017 J 2 | S/2017 J 3 | S/2017 J 5 | S/2017 J 6 | S/2017 J 7 | S/2017 J 8 | S/2017 J 9 | S/2018 J 2 |S/2018 J 3 | S/2018 J 4 | S/2021 J 1 S/2021 J 2 | S/2021 J 3 | S/2021 J 4 | S/2021 J 5 | S/2021 J 6 | S/2022 J 1 | S/2022 J 2 | S/2022 J 3

edit The Solar System
Central star

Sun (Sol)

Planets

Mercury - Venus - Earth - Mars - Jupiter - Saturn - Uranus - Neptune

Natural satellites

Moon - Phobos - Deimos - Io - Europa - Ganymede - Titan - more...

Add-ons

Planets - Dwarf Planets - Small objects - Natural satellites - Alternative star systems

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