Jupiter

This article is about the planet. For the Roman god, see Jupiter (god). For other uses, see Jupiter (disambiguation).

Jupiter is the fifth planet from the Sun and the largest in the Solar System. It is a gas giant with a mass more than 2.5 times that of all the other planets in the Solar System combined and slightly less than one-thousandth the mass of the Sun. Its diameter is eleven times that of Earth, and a tenth that of the Sun. Jupiter orbits the Sun at a distance of 5.20 AU (778.5 Gm), with an orbital period of 11.86 years. It is the third brightest natural object in the Earth's night sky, after the Moon and Venus, and has been observed since prehistoric times. Its name derives from that of Jupiter, the chief deity of ancient Roman religion.

Jupiter

Full disk view in natural colour, taken by the Hubble Space Telescope in April 2014[a]
Designations
Pronunciation	/ˈdʒuːpɪtər/ ⓘ[1]
Named after	Jupiter
Adjectives	Jovian (/ˈdʒoʊviən/)
Symbol
Orbital characteristics[2]
Epoch J2000
Aphelion	5.4570 AU (816.363 million km)
Perihelion	4.9506 AU (740.595 million km)
Semi-major axis	5.2038 AU (778.479 million km)
Eccentricity	0.0489
Orbital period (sidereal)	11.862 yr 4,332.59 d 10,476.8 Jovian solar days[3]
Orbital period (synodic)	398.88 d
Average orbital speed	13.06 km/s
Mean anomaly	20.020°[4]
Inclination	1.303° to ecliptic[4] 6.09° to Sun's equator[4] 0.32° to invariable plane[5]
Longitude of ascending node	100.464°
Time of perihelion	January 21, 2023[6]
Argument of perihelion	273.867°[4]
Known satellites	95 (as of 2023[update])[7]
Physical characteristics[2][8][9]
Mean radius	69911 km[b] 10.973 of Earth's
Equatorial radius	71492 km[b] 11.209 R🜨 (of Earth's) 0.10276 R☉ (of Sun's)
Polar radius	66854 km[b] 10.517 of Earth's
Flattening	0.06487
Surface area	6.1469×1010 km2 120.4 of Earth's
Volume	1.4313×1015 km3[b] 1,321 of Earth's
Mass	1.8982×1027 kg 317.8 M🜨 (of Earth's) 0.001 M☉ (of Sun's)[10]
Mean density	1.326 g/cm3[c]
Surface gravity	24.79 m/s2 2.528 g0[b][11]
Moment of inertia factor	0.2756±0.0006[12]
Escape velocity	59.5 km/s[b]
Synodic rotation period	9.9258 h (9 h 55 m 33 s)[3]
Sidereal rotation period	9.9250 hours (9 h 55 m 30 s)
Equatorial rotation velocity	12.6 km/s
Axial tilt	3.13° (to orbit)
North pole right ascension	268.057°; 17h 52m 14s[13]
North pole declination	64.495°[13]
Albedo	0.503 (Bond)[14] 0.538 (geometric)[15]
Temperature	88 K (−185 °C) (blackbody temperature)
Surface temp. min mean max 1 bar 165 K 0.1 bar 78 K 128 K
Apparent magnitude	−2.94[16] to −1.66[16]
Absolute magnitude (H)	−9.4[17]
Angular diameter	29.8" to 50.1"
Atmosphere[2]
Surface pressure	200–600 kPa (30–90 psi) (opaque cloud deck)[18]
Scale height	27 km (17 mi)
Composition by volume	89%±2.0% hydrogen 10%±2.0% helium 0.3%±0.1% methane 0.026%±0.004% ammonia 0.0028%±0.001% hydrogen deuteride 0.0006%±0.0002% ethane 0.0004%±0.0004% water

Jupiter was the first of the Sun's planets to form, and its inward migration during the primordial phase of the Solar System affected much of the formation history of the other planets. Jupiter's atmosphere consists of 76% hydrogen and 24% helium by mass, with a denser interior. It contains trace elements like carbon, oxygen, sulfur, neon, ammonia, water vapour, phosphine, hydrogen sulfide, and hydrocarbons. Jupiter's helium abundance is 80% of the Sun's, similar to Saturn's composition. The ongoing contraction of Jupiter's interior generates more heat than the planet receives from the Sun. Its internal structure is believed to consist of an outer mantle of fluid metallic hydrogen and a diffuse inner core of denser material. Because of its rapid rate of rotation, one turn in ten hours, Jupiter is an oblate spheroid; it has a slight but noticeable bulge around the equator. The outer atmosphere is divided into a series of latitudinal bands, with turbulence and storms along their interacting boundaries; the most obvious result of this is the Great Red Spot, a giant storm that has been recorded since 1831.

Jupiter's magnetic field is the strongest and second-largest contiguous structure in the Solar System, generated by eddy currents within the fluid, metallic hydrogen core. The solar wind interacts with the magnetosphere, extending it outward and affecting Jupiter's orbit. Jupiter is surrounded by a faint system of planetary rings that were discovered in 1979 by Voyager 1 and further investigated by the Galileo orbiter in the 1990s. The Jovian ring system consists mainly of dust and has three main segments: an inner torus of particles known as the halo, a relatively bright main ring, and an outer gossamer ring. The rings have a reddish colour in visible and near-infrared light. The age of the ring system is unknown, possibly dating back to Jupiter's formation.

At least 95 moons orbit the planet; the four largest moons—Io, Europa, Ganymede, and Callisto—orbit within the magnetosphere, and were discovered by Galileo Galilei in 1610. Ganymede, the largest of the four, is larger than the planet Mercury. Since 1973, Jupiter has been visited by nine robotic probes: seven flybys and two dedicated orbiters, with two more en route.

Name and symbol

In both the ancient Greek and Roman civilizations, Jupiter was named after the chief god of the divine pantheon: Zeus to the Greeks and Jupiter to the Romans.^[19] The International Astronomical Union formally adopted the name Jupiter for the planet in 1976 and has since named its newly discovered satellites for the god's lovers, favourites, and descendants.^[20] The planetary symbol for Jupiter, , descends from a Greek zeta with a horizontal stroke, ⟨Ƶ⟩, as an abbreviation for Zeus.^[21][22]

In Latin, Iovis is the genitive case of Iuppiter, i.e. Jupiter. It is associated with the etymology of Zeus ('sky father'). The English equivalent, Jove, is known to have come into use as a poetic name for the planet around the 14th century.^[23]

Jovian is the adjectival form of Jupiter. The older adjectival form jovial, employed by astrologers in the Middle Ages, has come to mean 'happy' or 'merry', moods ascribed to Jupiter's influence in astrology.^[24]

The original Greek deity Zeus supplies the root zeno-, which is used to form some Jupiter-related words, such as zenography.^[d]

Formation and migration

Main article: Grand tack hypothesis

See also: Formation and evolution of the Solar System

Jupiter is believed to be the oldest planet in the Solar System, having formed just one million years after the Sun and roughly 50 million years before Earth.^[25] Current models of Solar System formation suggest that Jupiter formed at or beyond the snow line: a distance from the early Sun where the temperature was sufficiently cold for volatiles such as water to condense into solids.^[26] First forming a solid core, the planet then accumulated its gaseous atmosphere. Therefore, the planet must have formed before the solar nebula was fully dispersed.^[27] During its formation, Jupiter's mass gradually increased until it had 20 times the mass of the Earth, approximately half of which was made up of silicates, ices and other heavy-element constituents.^[25] When the proto-Jupiter grew larger than 50 Earth masses it created a gap in the solar nebula.^[25] Thereafter, the growing planet reached its final mass in 3–4 million years.^[25][27] Since Jupiter is made of the same elements as the Sun (hydrogen and helium) it has been suggested that the Solar System might have been early in its formation a system of multiple protostars, which are quite common, with Jupiter being the second but failed protostar. But the Solar System never developed into a system of multiple stars and Jupiter does not qualify as a protostar or brown dwarf since it does not have enough mass to fuse hydrogen.^[28][29]

According to the "grand tack hypothesis", Jupiter began to form at a distance of roughly 3.5 AU (520 million km; 330 million mi) from the Sun. As the young planet accreted mass, its interaction with the gas disk orbiting the Sun and the orbital resonances from Saturn caused it to migrate inward.^[26][30] This upset the orbits of several super-Earths orbiting closer to the Sun, causing them to collide destructively.^[31] Saturn would later have begun to migrate inwards at a faster rate than Jupiter until the two planets became captured in a 3:2 mean motion resonance at approximately 1.5 AU (220 million km; 140 million mi) from the Sun.^[32] This changed the direction of migration, causing them to migrate away from the Sun and out of the inner system to their current locations.^[31] All of this happened over a period of 3–6 million years, with the final migration of Jupiter occurring over several hundred thousand years.^[30][33] Jupiter's migration from the inner solar system eventually allowed the inner planets—including Earth—to form from the rubble.^[34]

There are several unresolved issues with the grand tack hypothesis. The resulting formation timescales of terrestrial planets appear to be inconsistent with the measured elemental composition.^[35] Jupiter would likely have settled into an orbit much closer to the Sun if it had migrated through the solar nebula.^[36] Some competing models of Solar System formation predict the formation of Jupiter with orbital properties that are close to those of the present-day planet.^[27] Other models predict Jupiter forming at distances much farther out, such as 18 AU (2.7 billion km; 1.7 billion mi).^[37][38]

According to the Nice model, the infall of proto-Kuiper belt objects over the first 600 million years of Solar System history caused Jupiter and Saturn to migrate from their initial positions into a 1:2 resonance, which caused Saturn to shift into a higher orbit, disrupting the orbits of Uranus and Neptune, depleting the Kuiper belt, and triggering the Late Heavy Bombardment.^[39]

Based on Jupiter's composition, researchers have made the case for an initial formation outside the molecular nitrogen (N₂) snow line, which is estimated at 20–30 AU (3.0–4.5 billion km; 1.9–2.8 billion mi) from the Sun, and possibly even outside the argon snow line, which may be as far as 40 AU (6.0 billion km; 3.7 billion mi).^[40][41] Having formed at one of these extreme distances, Jupiter would then have, over a roughly 700,000-year period, migrated inwards to its current location,^[37][38] during an epoch approximately 2–3 million years after the planet began to form. In this model, Saturn, Uranus, and Neptune would have formed even further out than Jupiter, and Saturn would also have migrated inwards.^[37]

Physical characteristics

Jupiter is a gas giant, meaning its chemical composition is primarily hydrogen and helium. These materials are classified as gasses in planetary geology, a term that does not denote the state of matter. It is the largest planet in the Solar System, with a diameter of 142,984 km (88,846 mi) at its equator, giving it a volume 1,321 times that of the Earth.^[2][42] Its average density, 1.326 g/cm³,^[e] is lower than those of the four terrestrial planets.^[44][45]

Composition

The atmosphere of Jupiter is approximately 76% hydrogen and 24% helium by mass. By volume, the upper atmosphere is about 90% hydrogen and 10% helium, with the lower proportion owing to the individual helium atoms being more massive than the molecules of hydrogen formed in this part of the atmosphere.^[46] The atmosphere contains trace amounts of elemental carbon, oxygen, sulfur, and neon,^[47] as well as ammonia, water vapour, phosphine, hydrogen sulfide, and hydrocarbons like methane, ethane and benzene.^[48] Its outermost layer contains crystals of frozen ammonia.^[49] The planet's interior is denser, with a composition of roughly 71% hydrogen, 24% helium, and 5% other elements by mass.^[50][51]

The atmospheric proportions of hydrogen and helium are close to the theoretical composition of the primordial solar nebula.^[52] Neon in the upper atmosphere consists of 20 parts per million by mass, which is about a tenth as abundant as in the Sun.^[53] Jupiter's helium abundance is about 80% that of the Sun due to the precipitation of these elements as helium-rich droplets, a process that happens deep in the planet's interior.^[54][55]

Based on spectroscopy, Saturn is thought to be similar in composition to Jupiter, but the other giant planets Uranus and Neptune have relatively less hydrogen and helium and relatively more of the next most common elements, including oxygen, carbon, nitrogen, and sulfur.^[56] These planets are known as ice giants because during their formation, these elements are thought to have been incorporated into them as ice; however, they probably contain very little ice.^[57]

Size and mass

Main article: Jupiter mass

Size of Jupiter compared to Earth and Earth's Moon

Jupiter is about ten times larger than Earth (11.209 R_🜨) and smaller than the Sun (0.10276 R_☉). Jupiter's mass is 318 times that of Earth;^[2] 2.5 times that of all the other planets in the Solar System combined. It is so massive that its barycentre with the Sun lies above the Sun's surface at 1.068 solar radii from the Sun's centre.^{[58][59]: 6} Jupiter's radius is about one tenth the radius of the Sun,^[60] and its mass is one thousandth the mass of the Sun, as the densities of the two bodies are similar.^[61] A "Jupiter mass" (M_J or M_Jup) is used as a unit to describe masses of other objects, particularly extrasolar planets and brown dwarfs. For example, the extrasolar planet HD 209458 b has a mass of 0.69 M_J, while the brown dwarf Gliese 229 b has a mass of 60.4 M_J.^[62][63]

Theoretical models indicate that if Jupiter had over 40% more mass, the interior would be so compressed that its volume would decrease despite the increasing amount of matter. For smaller changes in its mass, the radius would not change appreciably.^[64] As a result, Jupiter is thought to have about as large a diameter as a planet of its composition and evolutionary history can achieve.^[65] The process of further shrinkage with increasing mass would continue until appreciable stellar ignition was achieved.^[66] Although Jupiter would need to be about 75 times more massive to fuse hydrogen and become a star,^[67] its diameter is sufficient as the smallest red dwarf may be slightly larger in radius than Saturn.^[68]

Jupiter radiates more heat than it receives through solar radiation, due to the Kelvin–Helmholtz mechanism within its contracting interior.^{[69]: 30 [70]} This process causes Jupiter to shrink by about 1 mm (0.039 in) per year.^[71][72] At the time of its formation, Jupiter was hotter and was about twice its current diameter.^[73]

Internal structure

Diagram of Jupiter with its interior, surface features, rings, and inner moons

Before the early 21st century, most scientists proposed one of two scenarios for the formation of Jupiter. If the planet accreted first as a solid body, it would consist of a dense core, a surrounding layer of fluid metallic hydrogen (with some helium) extending outward to about 80% of the radius of the planet,^[74] and an outer atmosphere consisting primarily of molecular hydrogen.^[72] Alternatively, if the planet collapsed directly from the gaseous protoplanetary disk, it was expected to completely lack a core, consisting instead of a denser and denser fluid (predominantly molecular and metallic hydrogen) all the way to the centre. Data from the Juno mission showed that Jupiter has a diffuse core that mixes into its mantle, extending for 30–50% of the planet's radius, and comprising heavy elements with a combined mass 7–25 times the Earth.^[75][76][77] This mixing process could have arisen during formation, while the planet accreted solids and gases from the surrounding nebula.^[78] Alternatively, it could have been caused by an impact from a planet of about ten Earth masses a few million years after Jupiter's formation, which would have disrupted an originally compact Jovian core.^[76][79]

Outside the layer of metallic hydrogen lies a transparent interior atmosphere of hydrogen. At this depth, the pressure and temperature are above molecular hydrogen's critical pressure of 1.3 MPa and critical temperature of 33 K (−240.2 °C; −400.3 °F).^[80] In this state, there are no distinct liquid and gas phases—hydrogen is said to be in a supercritical fluid state. The hydrogen and helium gas extending downward from the cloud layer gradually transitions to a liquid in deeper layers, possibly resembling something akin to an ocean of liquid hydrogen and other supercritical fluids.^{[69]: 22 [81][82]} Physically, the gas gradually becomes hotter and denser as depth increases.^[83][84]

Rain-like droplets of helium and neon precipitate downward through the lower atmosphere, depleting the abundance of these elements in the upper atmosphere.^[54][85] Calculations suggest that helium drops separate from metallic hydrogen at a radius of 60,000 km (37,000 mi) (11,000 km (6,800 mi) below the cloud tops) and merge again at 50,000 km (31,000 mi) (22,000 km (14,000 mi) beneath the clouds).^[86] Rainfalls of diamonds have been suggested to occur, as well as on Saturn^[87] and the ice giants Uranus and Neptune.^[88]

The temperature and pressure inside Jupiter increase steadily inward as the heat of planetary formation can only escape by convection.^[55] At a surface depth where the atmospheric pressure level is 1 bar (0.10 MPa), the temperature is around 165 K (−108 °C; −163 °F). The region where supercritical hydrogen changes gradually from a molecular fluid to a metallic fluid spans pressure ranges of 50–400 GPa with temperatures of 5,000–8,400 K (4,730–8,130 °C; 8,540–14,660 °F), respectively. The temperature of Jupiter's diluted core is estimated to be 20,000 K (19,700 °C; 35,500 °F) with a pressure of around 4,000 GPa.^[89]

Atmosphere

Main article: Atmosphere of Jupiter

Timelapse of Jupiter's cloud system moving over the course of one month (photographed during Voyager 1 flyby in 1979)

The atmosphere of Jupiter is primarily composed of molecular hydrogen and helium, with a smaller amount of other compounds such as water, methane, hydrogen sulfide, and ammonia.^[90] Jupiter's atmosphere extends to a depth of approximately 3,000 km (2,000 mi) below the cloud layers.^[89]

Cloud layers

Jupiter is perpetually covered with clouds of ammonia crystals, which may contain ammonium hydrosulfide as well.^[91] The clouds are located in the tropopause layer of the atmosphere, forming bands at different latitudes, known as tropical regions. These are subdivided into lighter-hued zones and darker belts. The interactions of these conflicting circulation patterns cause storms and turbulence. Wind speeds of 100 metres per second (360 km/h; 220 mph) are common in zonal jet streams.^[92] The zones have been observed to vary in width, colour and intensity from year to year, but they have remained stable enough for scientists to name them.^[59]: 6

View of Jupiter's south pole

Enhanced colour view of Jupiter's southern storms

The cloud layer is about 50 km (31 mi) deep and consists of at least two decks of ammonia clouds: a thin, clearer region on top and a thicker, lower deck. There may be a thin layer of water clouds underlying the ammonia clouds, as suggested by flashes of lightning detected in the atmosphere of Jupiter.^[93] These electrical discharges can be up to a thousand times as powerful as lightning on Earth.^[94] The water clouds are assumed to generate thunderstorms in the same way as terrestrial thunderstorms, driven by the heat rising from the interior.^[95] The Juno mission revealed the presence of "shallow lightning" which originates from ammonia-water clouds relatively high in the atmosphere.^[96] These discharges carry "mushballs" of water-ammonia slushes covered in ice, which fall deep into the atmosphere.^[97] Upper-atmospheric lightning has been observed in Jupiter's upper atmosphere, bright flashes of light that last around 1.4 milliseconds. These are known as "elves" or "sprites" and appear blue or pink due to the hydrogen.^[98][99]

The orange and brown colours in the clouds of Jupiter are caused by upwelling compounds that change colour when they are exposed to ultraviolet light from the Sun. The exact makeup remains uncertain, but the substances are thought to be made up of phosphorus, sulfur or possibly hydrocarbons.^{[69]: 39 [100]} These colourful compounds, known as chromophores, mix with the warmer clouds of the lower deck. The light-coloured zones are formed when rising convection cells form crystallising ammonia that hides the chromophores from view.^[101]

Jupiter has a low axial tilt, thus ensuring that the poles always receive less solar radiation than the planet's equatorial region. Convection within the interior of the planet transports energy to the poles, balancing out temperatures at the cloud layer.^[59]: 54

Great Red Spot and other vortices

Close-up of the Great Red Spot imaged by the Juno spacecraft in true colour. Due to the way Juno takes photographs, stitched image has extreme barrel distortion.

A well-known feature of Jupiter is the Great Red Spot,^[102] a persistent anticyclonic storm located 22° south of the equator. It was first observed in 1831,^[103] and possibly as early as 1665.^[104][105] Images by the Hubble Space Telescope have shown two more "red spots" adjacent to the Great Red Spot.^[106][107] The storm is visible through Earth-based telescopes with an aperture of 12 cm or larger.^[108] The storm rotates counterclockwise, with a period of about six days.^[109] The maximum altitude of this storm is about 8 km (5 mi) above the surrounding cloud tops.^[110] The Spot's composition and the source of its red colour remain uncertain, although photodissociated ammonia reacting with acetylene is a likely explanation.^[111]

The Great Red Spot is larger than the Earth.^[112] Mathematical models suggest that the storm is stable and will be a permanent feature of the planet.^[113] However, it has significantly decreased in size since its discovery. Initial observations in the late 1800s showed it to be approximately 41,000 km (25,500 mi) across. As of 2015^[update], the storm was measured at approximately 16,500 by 10,940 km (10,250 by 6,800 mi),^[114] and was decreasing in length by about 930 km (580 mi) per year.^[112][115] In October 2021, a Juno flyby mission measured the depth of the Great Red Spot, putting it at around 300–500 kilometres (190–310 miles).^[116]

Juno missions found several cyclone groups at Jupiter's poles. The northern group contains nine cyclones, with a large one in the centre and eight others around it, while its southern counterpart also consists of a centre vortex but is surrounded by five large storms and a single smaller one for a total of 7 storms.^[117][118]

Formation of Oval BA from three white ovals

In 2000, an atmospheric feature formed in the southern hemisphere that is similar in appearance to the Great Red Spot, but smaller. This was created when smaller, white oval-shaped storms merged to form a single feature—these three smaller white ovals were formed in 1939–1940. The merged feature was named Oval BA. It has since increased in intensity and changed from white to red, earning it the nickname "Little Red Spot".^[119][120]

In April 2017, a "Great Cold Spot" was discovered in Jupiter's thermosphere at its north pole. This feature is 24,000 km (15,000 mi) across, 12,000 km (7,500 mi) wide, and 200 °C (360 °F) cooler than surrounding material. While this spot changes form and intensity over the short term, it has maintained its general position in the atmosphere for more than 15 years. It may be a giant vortex similar to the Great Red Spot, and appears to be quasi-stable like the vortices in Earth's thermosphere. This feature may be formed by interactions between charged particles generated from Io and the strong magnetic field of Jupiter, resulting in a redistribution of heat flow.^[121]

Magnetosphere

Main article: Magnetosphere of Jupiter

Aurorae on the north and south poles
(animation)

Aurorae on the north pole
(Hubble). False colour image composite.

Infrared view of southern lights
(Jovian IR Mapper). False colour image.

Jupiter's magnetic field is the strongest of any planet in the Solar System,^[101] with a dipole moment of 4.170 gauss (0.4170 mT) that is tilted at an angle of 10.31° to the pole of rotation. The surface magnetic field strength varies from 2 gauss (0.20 mT) up to 20 gauss (2.0 mT).^[122] This field is thought to be generated by eddy currents—swirling movements of conducting materials—within the fluid, metallic hydrogen core. 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—a region between it and the bow shock. The solar wind interacts with these regions, elongating the magnetosphere on Jupiter's lee side and extending it outward until it nearly reaches the orbit of Saturn. The four largest moons of Jupiter all orbit within the magnetosphere, which protects them from solar wind.^[69]: 69

The volcanoes on the moon Io emit large amounts of sulfur dioxide, forming a gas torus along its orbit. The gas is ionized in Jupiter's magnetosphere, producing sulfur and oxygen ions. They, together with hydrogen ions originating from the atmosphere of Jupiter, form a plasma sheet in Jupiter's equatorial plane. The plasma in the sheet co-rotates with the planet, causing deformation of the dipole magnetic field into that of a magnetodisk. Electrons within the plasma sheet generate a strong radio signature, with short, superimposed bursts in the range of 0.6–30 MHz that are detectable from Earth with consumer-grade shortwave radio receivers.^[123][124] As Io moves through this torus, the interaction generates Alfvén waves that carry ionized matter into the polar regions of Jupiter. As a result, radio waves are generated through a cyclotron maser mechanism, and the energy is transmitted out along a cone-shaped surface. When Earth intersects this cone, the radio emissions from Jupiter can exceed the radio output of the Sun.^[125]

Jovian radiation

Moon	rem/day
Io	3600[126]
Europa	540[126]
Ganymede	8[126]
Callisto	0.01[126]
Earth (Max)	0.07
Earth (Avg)	0.0007

Planetary rings

Main article: Rings of Jupiter

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.^[127] These rings appear to be made of dust, whereas Saturn's rings are made of ice.^[69]: 65 The main ring is most likely made out of material ejected from the satellites Adrastea and Metis, which is drawn into Jupiter because of the planet's strong gravitational influence. New material is added by additional impacts.^[128] In a similar way, the moons Thebe and Amalthea are believed to produce the two distinct components of the dusty gossamer ring.^[128] There is evidence of a fourth ring that may consist of collisional debris from Amalthea that is strung along the same moon's orbit.^[129]

Orbit and rotation

3-hour timelapse showing rotation of Jupiter and orbital motion of the moons

Jupiter is the only planet whose barycentre with the Sun lies outside the volume of the Sun, though by 7% of the Sun's radius.^[130][131] The average distance between Jupiter and the Sun is 778 million km (5.2 AU) and it completes an orbit every 11.86 years. This is approximately two-fifths the orbital period of Saturn, forming a near orbital resonance.^[132] The orbital plane of Jupiter is inclined 1.30° compared to Earth. Because the eccentricity of its orbit is 0.049, Jupiter is slightly over 75 million km nearer the Sun at perihelion than aphelion,^[2] which means that its orbit is nearly circular. This low eccentricity is at odds with exoplanet discoveries, which have revealed Jupiter-sized planets with very high eccentricities. Models suggest this may be due to there being two giant planets in our Solar System, as the presence of a third or more giant planets tends to induce larger eccentricities.^[133]

The axial tilt of Jupiter is 3.13°, which is relatively small, so its seasons are insignificant compared to those of Earth and Mars.^[134]

Jupiter's rotation is the fastest of all the Solar System's planets, completing a rotation on its axis in slightly less than ten hours; this creates an equatorial bulge easily seen through an amateur telescope. Because Jupiter is not a solid body, its upper atmosphere undergoes differential rotation. The rotation of Jupiter's polar atmosphere is about 5 minutes longer than that of the equatorial atmosphere.^[135] The planet is an oblate spheroid, meaning that the diameter across its equator is longer than the diameter measured between its poles.^[84] On Jupiter, the equatorial diameter is 9,276 km (5,764 mi) longer than the polar diameter.^[2]

Three systems are used as frames of reference for tracking planetary rotation, particularly when graphing the motion of atmospheric features. System I applies to latitudes from 7° N to 7° S; its period is the planet's shortest, at 9h 50 m 30.0s. System II applies at latitudes north and south of these; its period is 9h 55 m 40.6s.^[136] System III was defined by radio astronomers and corresponds to the rotation of the planet's magnetosphere; its period is Jupiter's official rotation.^[137]

Observation

Jupiter and four Galilean moons seen through an amateur telescope

Jupiter is usually the fourth brightest object in the sky (after the Sun, the Moon, and Venus),^[101] although at opposition Mars can appear brighter than Jupiter. Depending on Jupiter's position with respect to the Earth, it can vary in visual magnitude from as bright as −2.94 at opposition down to −1.66 during conjunction with the Sun.^[16] The mean apparent magnitude is −2.20 with a standard deviation of 0.33.^[16] The angular diameter of Jupiter likewise varies from 50.1 to 30.5 arc seconds.^[2] Favourable oppositions occur when Jupiter is passing through the perihelion of its orbit, bringing it closer to Earth.^[138] Near opposition, Jupiter will appear to go into retrograde motion for a period of about 121 days, moving backward through an angle of 9.9° before returning to prograde movement.^[139]

Because the orbit of Jupiter is outside that of Earth, the phase angle of Jupiter as viewed from Earth is always less than 11.5°; thus, Jupiter always appears nearly fully illuminated when viewed through Earth-based telescopes. It was during spacecraft missions to Jupiter that crescent views of the planet were obtained.^[140] A small telescope will usually show Jupiter's four Galilean moons and the cloud belts across Jupiter's atmosphere. A larger telescope with an aperture of 4–6 inches (10–15 cm) will show Jupiter's Great Red Spot when it faces Earth.^[141][142]

History

Pre-telescopic research

Model in the Almagest of the longitudinal motion of Jupiter (☉) relative to Earth (🜨)

Observation of Jupiter dates back to at least the Babylonian astronomers of the 7th or 8th century BC.^[143] The ancient Chinese knew Jupiter as the "Suì Star" (Suìxīng 歲星) and established their cycle of 12 earthly branches based on the approximate number of years it takes Jupiter to rotate around the Sun; the Chinese language still uses its name (simplified as 歲) when referring to years of age. By the 4th century BC, these observations had developed into the Chinese zodiac,^[144] and each year became associated with a Tai Sui star and god controlling the region of the heavens opposite Jupiter's position in the night sky. These beliefs survive in some Taoist religious practices and in the East Asian zodiac's twelve animals. The Chinese historian Xi Zezong has claimed that Gan De, an ancient Chinese astronomer,^[145] reported a small star "in alliance" with the planet,^[146] which may indicate a sighting of one of Jupiter's moons with the unaided eye. If true, this would predate Galileo's discovery by nearly two millennia.^[147][148]

A 2016 paper reports that trapezoidal rule was used by Babylonians before 50 BC for integrating the velocity of Jupiter along the ecliptic.^[149] In his 2nd century work the Almagest, the Hellenistic astronomer Claudius Ptolemaeus constructed a geocentric planetary model based on deferents and epicycles to explain Jupiter's motion relative to Earth, giving its orbital period around Earth as 4332.38 days, or 11.86 years.^[150]

Ground-based telescope research

Galileo's drawings of Jupiter and its "Medicean Stars" from Sidereus Nuncius

In 1610, Italian polymath Galileo Galilei discovered the four largest moons of Jupiter (now known as the Galilean moons) using a telescope. This is thought to be the first telescopic observation of moons other than Earth's. Just one day after Galileo, Simon Marius independently discovered moons around Jupiter, though he did not publish his discovery in a book until 1614.^[151] It was Marius's names for the major moons, however, that stuck: Io, Europa, Ganymede, and Callisto. The discovery was a major point in favour of the heliocentric theory of the motions of the planets by Nicolaus Copernicus; Galileo's outspoken support of the Copernican theory led to him being tried and condemned by the Inquisition.^[152]

In the autumn of 1639, the Neapolitan optician Francesco Fontana tested a 22-palm telescope of his own making and discovered the characteristic bands of the planet's atmosphere.^[153]

During the 1660s, Giovanni Cassini used a new telescope to discover spots in Jupiter's atmosphere, observe that the planet appeared oblate, and estimate its rotation period.^[154] In 1692, Cassini noticed that the atmosphere undergoes a differential rotation.^[155]

The Great Red Spot may have been observed as early as 1664 by Robert Hooke and in 1665 by Cassini, although this is disputed. The pharmacist Heinrich Schwabe produced the earliest known drawing to show details of the Great Red Spot in 1831.^[156] The Red Spot was reportedly lost from sight on several occasions between 1665 and 1708 before becoming quite conspicuous in 1878.^[157] It was recorded as fading again in 1883 and at the start of the 20th century.^[158]

Both Giovanni Borelli and Cassini made careful tables of the motions of Jupiter's moons, which allowed predictions of when the moons would pass before or behind the planet. By the 1670s, Cassini observed that when Jupiter was on the opposite side of the Sun from Earth, these events would occur about 17 minutes later than expected. Ole Rømer deduced that light does not travel instantaneously (a conclusion that Cassini had earlier rejected),^[51] and this timing discrepancy was used to estimate the speed of light.^[159][160]

In 1892, E. E. Barnard observed a fifth satellite of Jupiter with the 36-inch (910 mm) refractor at Lick Observatory in California. This moon was later named Amalthea.^[161] It was the last planetary moon to be discovered directly by a visual observer through a telescope.^[162] An additional eight satellites were discovered before the flyby of the Voyager 1 probe in 1979.^[f]

In 1932, Rupert Wildt identified absorption bands of ammonia and methane in the spectra of Jupiter.^[163] Three long-lived anticyclonic features called "white ovals" were observed in 1938. For several decades, they remained as separate features in the atmosphere that approach each other but never merge. Finally, two of the ovals merged in 1998, then absorbed the third in 2000, becoming Oval BA.^[164]

Radiotelescope research

In 1955, Bernard Burke and Kenneth Franklin discovered that Jupiter emits bursts of radio waves at a frequency of 22.2 MHz.^[69]: 36 The period of these bursts matched the rotation of the planet, and they used this information to determine a more precise value for Jupiter's 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) lasting less than a hundredth of a second.^[165]

Scientists have discovered three forms of radio signals transmitted from Jupiter:

• Decametric radio bursts (with a wavelength of tens of metres) vary with the rotation of Jupiter, and are influenced by the interaction of Io with Jupiter's magnetic field.^[166]
• Decimetric radio emission (with wavelengths measured in centimetres) was first observed by Frank Drake and Hein Hvatum in 1959.^[69]: 36 The origin of this signal is a torus-shaped belt around Jupiter's equator, which generates cyclotron radiation from electrons that are accelerated in Jupiter's magnetic field.^[167]
• Thermal radiation is produced by heat in the atmosphere of Jupiter.^[69]: 43

Exploration

Main article: Exploration of Jupiter

Jupiter has been visited by automated spacecraft since 1973, when the space probe Pioneer 10 passed close enough to Jupiter to send back revelations about its properties and phenomena.^[168][169] Missions to Jupiter are accomplished at a cost in energy, which is described by the net change in velocity of the spacecraft, or delta-v. Entering a Hohmann transfer orbit from Earth to Jupiter from low Earth orbit requires a delta-v of 6.3 km/s,^[170] which is comparable to the 9.7 km/s delta-v needed to reach low Earth orbit.^[171] Gravity assists through planetary flybys can be used to reduce the energy required to reach Jupiter.^[172]

Flyby missions

Spacecraft	Closest approach	Distance (km)
Pioneer 10	December 3, 1973	130,000
Pioneer 11	December 4, 1974	34,000
Voyager 1	March 5, 1979	349,000
Voyager 2	July 9, 1979	570,000
Ulysses	February 8, 1992[173]	408,894
	February 4, 2004[173]	120,000,000
Cassini	December 30, 2000	10,000,000
New Horizons	February 28, 2007	2,304,535

Beginning in 1973, several spacecraft performed planetary flyby manoeuvres that brought them within the observation range of Jupiter. The Pioneer missions obtained the first close-up images of Jupiter's atmosphere and several of its moons. They discovered that the radiation fields near the planet were much stronger than expected, but both spacecraft managed to survive in that environment. The trajectories of these spacecraft were used to refine the mass estimates of the Jovian system. Radio occultations by the planet resulted in better measurements of Jupiter's diameter and the amount of polar flattening.^{[59]: 47 [174]}

Six years later, the Voyager missions vastly improved the understanding of the Galilean moons and discovered Jupiter's rings. They also confirmed that the Great Red Spot was anticyclonic. Comparison of images showed that the Spot had changed hues since the Pioneer missions, turning from orange to dark brown. A torus of ionized atoms was discovered along Io's orbital path, which were found to come from erupting volcanoes on the moon's surface. As the spacecraft passed behind the planet, it observed flashes of lightning in the night side atmosphere.^{[59]: 87 [175]}

The next mission to encounter Jupiter was the Ulysses solar probe. In February 1992, it performed a flyby manoeuvre to attain a polar orbit around the Sun. During this pass, the spacecraft studied Jupiter's magnetosphere, although it had no cameras to photograph the planet. The spacecraft passed by Jupiter six years later, this time at a much greater distance.^[173]

In 2000, the Cassini probe flew by Jupiter on its way to Saturn, and provided higher-resolution images.^[176]

The New Horizons probe flew by Jupiter in 2007 for a gravity assist en route to Pluto.^[177] The probe's cameras measured plasma output from volcanoes on Io and studied all four Galilean moons in detail.^[178]

Galileo mission

Main article: Galileo (spacecraft)

Galileo in preparation for mating with the rocket, 1989

The first spacecraft to orbit Jupiter was the Galileo mission, which reached the planet on December 7, 1995.^[65] It remained in orbit for over seven years, conducting multiple flybys of all the Galilean moons and Amalthea. The spacecraft also witnessed the impact of Comet Shoemaker–Levy 9 when it collided with Jupiter in 1994. Some of the goals for the mission were thwarted due to a malfunction in Galileos high-gain antenna.^[179]

A 340-kilogram titanium atmospheric probe was released from the spacecraft in July 1995, entering Jupiter's atmosphere on December 7.^[65] It parachuted through 150 km (93 mi) of the atmosphere at a speed of about 2,575 km/h (1,600 mph)^[65] and collected data for 57.6 minutes until the spacecraft was destroyed.^[180] 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. NASA destroyed the spacecraft to avoid any possibility of the spacecraft crashing into and possibly contaminating the moon Europa, which may harbour life.^[179]

Data from this mission revealed that hydrogen composes up to 90% of Jupiter's atmosphere.^[65] The recorded temperature was more than 300 °C (570 °F), and the wind speed measured more than 644 km/h (>400 mph) before the probes vaporized.^[65]

Juno mission

Main article: Juno (spacecraft)

Juno preparing for testing in a rotation stand, 2011

NASA's Juno mission arrived at Jupiter on July 4, 2016, with the goal of studying the planet in detail from a polar orbit. The spacecraft was originally intended to orbit Jupiter thirty-seven times over a period of twenty months.^{[181][77][182]} During the mission, the spacecraft will be exposed to high levels of radiation from Jupiter's magnetosphere, which may cause the failure of certain instruments.^[183] On August 27, 2016, the spacecraft completed its first flyby of Jupiter and sent back the first-ever images of Jupiter's north pole.^[184]

Juno completed 12 orbits before the end of its budgeted mission plan, ending in July 2018.^[185] In June of that year, NASA extended the mission operations plan to July 2021, and in January of that year the mission was extended to September 2025 with four lunar flybys: one of Ganymede, one of Europa, and two of Io.^[186][187] When Juno reaches the end of the mission, it will perform a controlled deorbit and disintegrate into Jupiter's atmosphere. This will avoid the risk of collision with Jupiter's moons.^[188][189]

Cancelled missions and future plans

There is an interest in missions to study Jupiter's larger icy moons, which may have subsurface liquid oceans.^[190] Funding difficulties have delayed progress, causing NASA's JIMO (Jupiter Icy Moons Orbiter) to be cancelled in 2005.^[191] A subsequent proposal was developed for a joint NASA/ESA mission called EJSM/Laplace, with a provisional launch date around 2020. EJSM/Laplace would have consisted of the NASA-led Jupiter Europa Orbiter and the ESA-led Jupiter Ganymede Orbiter.^[192] However, the ESA formally ended the partnership in April 2011, citing budget issues at NASA and the consequences on the mission timetable. Instead, ESA planned to go ahead with a European-only mission to compete in its L1 Cosmic Vision selection.^[193] These plans have been realized as the European Space Agency's Jupiter Icy Moon Explorer (JUICE), launched on April 14, 2023,^[194] followed by NASA's Europa Clipper mission, launched on October 14, 2024.^[195]

Other proposed missions include the Chinese National Space Administration's Tianwen-4 mission which aims to launch an orbiter to the Jovian system and possibly Callisto around 2035,^[196] and CNSA's Interstellar Express^[197] and NASA's Interstellar Probe,^[198] which would both use Jupiter's gravity to help them reach the edges of the heliosphere.

Moons

Main article: Moons of Jupiter

See also: Timeline of discovery of Solar System planets and their moons and Satellite system (astronomy)

Jupiter has 95 known natural satellites,^[199] and it is likely that this number would go up due to improved instrumentation.^[200] Of these, 79 are less than 10 km in diameter.^[7] The four largest moons are Ganymede, Callisto, Io, and Europa (in order of decreasing size), collectively known as the "Galilean moons", and are visible from Earth with binoculars on a clear night.^[201]

Galilean moons

Main article: Galilean moons

The moons discovered by Galileo—Io, Europa, Ganymede, and Callisto—are among the largest in the Solar System. The orbits of Io, Europa, and Ganymede 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 gravitational effects of the three large moons to distort their orbits into elliptical shapes, because each moon receives an extra tug from its neighbours at the same point in every orbit it makes. The tidal force from Jupiter, on the other hand, works to circularize their orbits.^[202]

The eccentricity of their orbits causes regular flexing of the three moons' shapes, with Jupiter's gravity stretching them out as they approach it and allowing them to spring back to more spherical shapes as they swing away. The friction created by this tidal flexing generates heat in the interior of the moons.^[203] This is seen most dramatically in the volcanic activity of Io (which is subject to the strongest tidal forces),^[203] and to a lesser degree in the geological youth of Europa's surface, which indicates recent resurfacing of the moon's exterior.^[204]

The Galilean moons compared to the Earth's Moon Name IPA Diameter Mass Orbital radius Orbital period km D☾ kg M☾ km a☾ days T☾ Io /ˈaɪ.oʊ/ 3,643 1.05 8.9×1022 1.20 421,700 1.10 1.77 0.07 Europa /jʊˈroʊpə/ 3,122 0.90 4.8×1022 0.65 671,034 1.75 3.55 0.13 Ganymede /ˈɡænɪmiːd/ 5,262 1.50 14.8×1022 2.00 1,070,412 2.80 7.15 0.26 Callisto /kəˈlɪstoʊ/ 4,821 1.40 10.8×1022 1.50 1,882,709 4.90 16.69 0.61

The Galilean satellites in false colour. From left to right, in order of increasing distance from Jupiter: Io, Europa, Ganymede, Callisto.

The Galilean satellites Io, Europa, Ganymede, and Callisto (in order of increasing distance from Jupiter) in false colour

Classification

Jupiter's moons were classified into four groups of four, based on their similar orbital elements.^[205] This picture has been complicated by the discovery of numerous small outer moons since 1999. Jupiter's moons are divided into several different groups, although there are two known moons which are not part of any group (Themisto and Valetudo).^[206]

The eight innermost regular moons, which have nearly circular orbits near the plane of Jupiter's equator, are thought to have formed alongside Jupiter, while the remainder are irregular moons and are thought to be captured asteroids or fragments of captured asteroids. The irregular moons within each group may have a common origin, perhaps as a larger moon or captured body that broke up.^[207][208]

Regular moons
Inner group	The inner group of four small moons all have diameters of less than 200 km, orbit at radii less than 200,000 km, and have orbital inclinations of less than half a degree.[209]
Galilean moons[210]	These four moons, discovered by Galileo Galilei and by Simon Marius in parallel, orbit between 400,000 and 2,000,000 km, and are some of the largest moons in the Solar System.
Irregular moons
Himalia group	A tightly clustered group of prograde-orbiting moons with orbits around 11,000,000–12,000,000 km from Jupiter.[211]
Carpo group	A sparsely populated group of small moons with highly inclined prograde orbits around 16,000,000–17,000,000 km from Jupiter.[7]
Ananke group	This group of retrograde-orbiting moons has rather indistinct borders, averaging 21,276,000 km from Jupiter with an average inclination of 149 degrees.[208]
Carme group	A tightly clustered group of retrograde-orbiting moons that averages 23,404,000 km from Jupiter with an average inclination of 165 degrees.[208]
Pasiphae group	A dispersed and vaguely distinct retrograde group that covers all the outermost moons.[212]

Interaction with the Solar System

As the most massive of the eight planets, the gravitational influence of Jupiter has helped shape the Solar System. With the exception of Mercury, the orbits of the system's planets lie closer to Jupiter's orbital plane than the Sun's equatorial plane. The Kirkwood gaps in the asteroid belt are mostly caused by Jupiter,^[213] and the planet may have been responsible for the Late Heavy Bombardment in the inner Solar System's history.^[214]

In addition to its moons, Jupiter's gravitational field controls numerous asteroids that have settled around the Lagrangian points that precede and follow the planet in its orbit around the Sun. These are known as the Trojan asteroids, and are divided into Greek and Trojan "camps" to honour the Iliad. The first of these, 588 Achilles, was discovered by Max Wolf in 1906; since then more than two thousand have been discovered.^[215] The largest is 624 Hektor.^[216]

The Jupiter family is defined as comets that have a semi-major axis smaller than Jupiter's; most short-period comets belong to this group. Members of the Jupiter family are thought to form in the Kuiper belt outside the orbit of Neptune. During close encounters with Jupiter, they are perturbed into orbits with a smaller period, which then becomes circularized by regular gravitational interactions with the Sun and Jupiter.^[217]

Impacts

Main article: Impact events on Jupiter

Brown spots mark Comet Shoemaker–Levy 9's impact sites on Jupiter

Jupiter has been called the Solar System's vacuum cleaner^[218] because of its immense gravity well and location near the inner Solar System. There are more impacts on Jupiter, such as comets, than on any other planet in the Solar System.^[219] For example, Jupiter experiences about 200 times more asteroid and comet impacts than Earth.^[65] Scientists used to believe that Jupiter partially shielded the inner system from cometary bombardment.^[65] However, computer simulations in 2008 suggest that Jupiter does not cause a net decrease in the number of comets that pass through the inner Solar System, as its gravity perturbs their orbits inward roughly as often as it accretes or ejects them.^[220] This topic remains controversial among scientists, as some think it draws comets towards Earth from the Kuiper belt, while others believe that Jupiter protects Earth from the Oort cloud.^[221]

In July 1994, the Comet Shoemaker–Levy 9 comet collided with Jupiter.^[222][223] The impacts were closely observed by observatories around the world, including the Hubble Space Telescope and Galileo spacecraft.^{[224][225][226]} The event was widely covered by the media.^[227]

Surveys of early astronomical records and drawings produced eight examples of potential impact observations between 1664 and 1839. However, a 1997 review determined that these observations had little or no possibility of being the results of impacts. Further investigation by this team revealed a dark surface feature discovered by astronomer Giovanni Cassini in 1690 may have been an impact scar.^[228]

In culture

See also: Jupiter in fiction and Planets in astrology § Jupiter

Jupiter, woodcut from a 1550 edition of Guido Bonatti's Liber Astronomiae

The existence of the planet Jupiter has been known since ancient times. It is visible to the naked eye in the night sky and can be seen in the daytime when the Sun is low.^[229] To the Babylonians, this planet represented their god Marduk,^[230] chief of their pantheon from the Hammurabi period.^[231] They used Jupiter's roughly 12-year orbit along the ecliptic to define the constellations of their zodiac.^[230]

The mythical Greek name for this planet is Zeus (Ζεύς), also referred to as Dias (Δίας), the planetary name of which is retained in modern Greek.^[232] The ancient Greeks knew the planet as Phaethon (Φαέθων), meaning "shining one" or "blazing star".^[233][234] The Greek myths of Zeus from the Homeric period showed particular similarities to certain Near-Eastern gods, including the Semitic El and Baal, the Sumerian Enlil, and the Babylonian god Marduk.^[235] The association between the planet and the Greek deity Zeus was drawn from Near Eastern influences and was fully established by the fourth century BC, as documented in the Epinomis of Plato and his contemporaries.^[236]

The god Jupiter is the Roman counterpart of Zeus, and he is the principal god of Roman mythology. The Romans originally called Jupiter the "star of Jupiter" (Iuppiter Stella), as they believed it to be sacred to its namesake god. This name comes from the Proto-Indo-European vocative compound *Dyēu-pəter (nominative: *Dyēus-pətēr, meaning "Father Sky-God", or "Father Day-God").^[237] As the supreme god of the Roman pantheon, Jupiter was the god of thunder, lightning, and storms, and was called the god of light and sky.^[238]

In Vedic astrology, Hindu astrologers named the planet after Brihaspati, the religious teacher of the gods, and called it "Guru", which means the "Teacher".^[239][240] In Central Asian Turkic myths, Jupiter is called Erendiz or Erentüz, from eren (of uncertain meaning) and yultuz ("star"). The Turks calculated the period of the orbit of Jupiter as 11 years and 300 days. They believed that some social and natural events connected to Erentüz's movements in the sky.^[241] The Chinese, Vietnamese, Koreans, and Japanese called it the "wood star" (Chinese: 木星; pinyin: mùxīng), based on the Chinese Five Elements.^{[242][243][244]} In China, it became known as the "Year-star" (Sui-sing), as Chinese astronomers noted that it jumped one zodiac constellation each year (with corrections). In some ancient Chinese writings, the years were, in principle, named in correlation with the Jovian zodiac signs.^[144]

See also

• Outline of Jupiter – Overview of and topical guide to Jupiter
• Eccentric Jupiter – Jovian planet that orbits its star in an eccentric orbit
• Hot Jupiter – Class of high mass planets orbiting close to a star
• Super-Jupiter – Class of planets with more mass than Jupiter
• Jovian–Plutonian gravitational effect – Astronomical hoax
• List of gravitationally rounded objects of the Solar System

Notes

1. This image was taken by the Hubble Space Telescope, using the Wide Field Camera 3, on April 21, 2014. Jupiter's atmosphere and its appearance constantly changes, and hence its current appearance today may not resemble what it was when this image was taken. Depicted in this image, however, are a few features that remain consistent, such as the famous Great Red Spot, featured prominently in the lower right of the image, and the planet's recognizable banded appearance.
2. Refers to the level of 1 bar atmospheric pressure
3. Based on the volume within the level of 1 bar atmospheric pressure
4. See for example: "IAUC 2844: Jupiter; 1975h". International Astronomical Union. October 1, 1975. Retrieved October 24, 2010. That particular word has been in use since at least 1966. See: "Query Results from the Astronomy Database". Smithsonian/NASA. Retrieved July 29, 2007.
5. About the same as sugar syrup (syrup USP),^[43]
6. See Moons of Jupiter for details and cites

References

1. Simpson, J. A.; Weiner, E. S. C. (1989). "Jupiter". Oxford English Dictionary. Vol. 8 (2nd ed.). Clarendon. ISBN 978-0-19-861220-9.
2. Williams, David R. (December 23, 2021). "Jupiter Fact Sheet". NASA. Archived from the original on December 29, 2019. Retrieved October 13, 2017.
3. Seligman, Courtney. "Rotation Period and Day Length". Archived from the original on September 29, 2018. Retrieved August 13, 2009.
4. Simon, J. L.; Bretagnon, P.; Chapront, J.; Chapront-Touzé, M.; Francou, G.; Laskar, J. (February 1994). "Numerical expressions for precession formulae and mean elements for the Moon and planets". Astronomy and Astrophysics. 282 (2): 663–683. Bibcode:1994A&A...282..663S.
5. Souami, D.; Souchay, J. (July 2012). "The solar system's invariable plane". Astronomy & Astrophysics. 543: 11. Bibcode:2012A&A...543A.133S. doi:10.1051/0004-6361/201219011. A133.
6. "HORIZONS Planet-center Batch call for January 2023 Perihelion". ssd.jpl.nasa.gov (Perihelion for Jupiter's planet-centre (599) occurs on 2023-Jan-21 at 4.9510113au during a rdot flip from negative to positive). NASA/JPL. Archived from the original on September 7, 2021. Retrieved September 7, 2021.
7. Sheppard, Scott S. "Moons of Jupiter". Earth & Planets Laboratory. Carnegie Institution for Science. Archived from the original on April 24, 2019. Retrieved December 20, 2022.
8. Seidelmann, P. Kenneth; Archinal, Brent A.; A'Hearn, Michael F.; Conrad, Albert R.; Consolmagno, Guy J.; Hestroffer, Daniel; Hilton, James L.; Krasinsky, Georgij A.; Neumann, Gregory A.; Oberst, Jürgen; Stooke, Philip J.; Tedesco, Edward F.; Tholen, David J.; Thomas, Peter C.; Williams, Iwan P. (2007). "Report of the IAU/IAG Working Group on cartographic coordinates and rotational elements: 2006". Celestial Mechanics and Dynamical Astronomy. 98 (3): 155–180. Bibcode:2007CeMDA..98..155S. doi:10.1007/s10569-007-9072-y. ISSN 0923-2958.
9. de Pater, Imke; Lissauer, Jack J. (2015). Planetary Sciences (2nd updated ed.). New York: Cambridge University Press. p. 250. ISBN 978-0-521-85371-2. Retrieved August 17, 2016.
10. "Astrodynamic Constants". JPL Solar System Dynamics. February 27, 2009. Archived from the original on March 21, 2019. Retrieved August 8, 2007.
11. "NASA: Solar System Exploration: Planets: Jupiter: Facts & Figures". solarsystem.nasa.gov. June 2, 2011. Archived from the original on September 5, 2011. Retrieved October 15, 2024.
12. Ni, D. (2018). "Empirical models of Jupiter's interior from Juno data". Astronomy & Astrophysics. 613: A32. Bibcode:2018A&A...613A..32N. doi:10.1051/0004-6361/201732183.
13. Archinal, B. A.; Acton, C. H.; A'Hearn, M. F.; Conrad, A.; Consolmagno, G. J.; Duxbury, T.; Hestroffer, D.; Hilton, J. L.; Kirk, R. L.; Klioner, S. A.; McCarthy, D.; Meech, K.; Oberst, J.; Ping, J.; Seidelmann, P. K. (2018). "Report of the IAU Working Group on Cartographic Coordinates and Rotational Elements: 2015". Celestial Mechanics and Dynamical Astronomy. 130 (3): 22. Bibcode:2018CeMDA.130...22A. doi:10.1007/s10569-017-9805-5. ISSN 0923-2958.
14. Li, Liming; Jiang, X.; West, R. A.; Gierasch, P. J.; Perez-Hoyos, S.; Sanchez-Lavega, A.; Fletcher, L. N.; Fortney, J. J.; Knowles, B.; Porco, C. C.; Baines, K. H.; Fry, P. M.; Mallama, A.; Achterberg, R. K.; Simon, A. A.; Nixon, C. A.; Orton, G. S.; Dyudina, U. A.; Ewald, S. P.; Schmude, R. W. (2018). "Less absorbed solar energy and more internal heat for Jupiter". Nature Communications. 9 (1): 3709. Bibcode:2018NatCo...9.3709L. doi:10.1038/s41467-018-06107-2. PMC 6137063. PMID 30213944.
15. Mallama, Anthony; Krobusek, Bruce; Pavlov, Hristo (2017). "Comprehensive wide-band magnitudes and albedos for the planets, with applications to exo-planets and Planet Nine". Icarus. 282: 19–33. arXiv:1609.05048. Bibcode:2017Icar..282...19M. doi:10.1016/j.icarus.2016.09.023. S2CID 119307693.
16. Mallama, A.; Hilton, J. L. (2018). "Computing Apparent Planetary Magnitudes for The Astronomical Almanac". Astronomy and Computing. 25: 10–24. arXiv:1808.01973. Bibcode:2018A&C....25...10M. doi:10.1016/j.ascom.2018.08.002. S2CID 69912809.
17. "Encyclopedia - the brightest bodies". IMCCE. Archived from the original on July 24, 2023. Retrieved May 29, 2023.
18. Bjoraker, G. L.; Wong, M. H.; de Pater, I.; Ádámkovics, M. (September 2015). "Jupiter's Deep Cloud Structure Revealed Using Keck Observations of Spectrally Resolved Line Shapes". The Astrophysical Journal. 810 (2): 10. arXiv:1508.04795. Bibcode:2015ApJ...810..122B. doi:10.1088/0004-637X/810/2/122. S2CID 55592285. 122.
19. Rachel Alexander (2015). Myths, Symbols and Legends of Solar System Bodies. The Patrick Moore Practical Astronomy Series. Vol. 177. New York, NY: Springer. pp. 141–159. Bibcode:2015msls.book.....A. doi:10.1007/978-1-4614-7067-0. ISBN 978-1-4614-7066-3.
20. "Naming of Astronomical Objects". International Astronomical Union. Archived from the original on October 31, 2013. Retrieved March 23, 2022.
21. Jones, Alexander (1999). Astronomical papyri from Oxyrhynchus. American Philosophical Society. pp. 62–63. ISBN 978-0-87169-233-7. It is now possible to trace the medieval symbols for at least four of the five planets to forms that occur in some of the latest papyrus horoscopes ([ P.Oxy. ] 4272, 4274, 4275 [...]). That for Jupiter is an obvious monogram derived from the initial letter of the Greek name.
22. Maunder, A. S. D. (August 1934). "The origin of the symbols of the planets". The Observatory. 57: 238–247. Bibcode:1934Obs....57..238M.
23. Harper, Douglas. "Jove". Online Etymology Dictionary. Archived from the original on March 23, 2022. Retrieved March 22, 2022.
24. "Jovial". Dictionary.com. Archived from the original on February 16, 2012. Retrieved July 29, 2007.
25. Kruijer, Thomas S.; Burkhardt, Christoph; Budde, Gerrit; Kleine, Thorsten (June 2017). "Age of Jupiter inferred from the distinct genetics and formation times of meteorites". Proceedings of the National Academy of Sciences. 114 (26): 6712–6716. Bibcode:2017PNAS..114.6712K. doi:10.1073/pnas.1704461114. PMC 5495263. PMID 28607079.
26. Bosman, A. D.; Cridland, A. J.; Miguel, Y. (December 2019). "Jupiter formed as a pebble pile around the N2 ice line". Astronomy & Astrophysics. 632: 5. arXiv:1911.11154. Bibcode:2019A&A...632L..11B. doi:10.1051/0004-6361/201936827. S2CID 208291392. L11.
27. D'Angelo, G.; Weidenschilling, S. J.; Lissauer, J. J.; Bodenheimer, P. (2021). "Growth of Jupiter: Formation in disks of gas and solids and evolution to the present epoch". Icarus. 355: 114087. arXiv:2009.05575. Bibcode:2021Icar..35514087D. doi:10.1016/j.icarus.2020.114087. S2CID 221654962.
28. Bodenheimer, Peter; D'Angelo, Gennaro; Lissauer, Jack J.; Fortney, Jonathan J.; Saumon, Didier (June 3, 2013). "Deuterium Burning In Massive Giant Planets And Low-mass Brown Dwarfs Formed By Core-nucleated Accretion". The Astrophysical Journal. 770 (2): 120. arXiv:1305.0980. Bibcode:2013ApJ...770..120B. doi:10.1088/0004-637X/770/2/120. ISSN 0004-637X.
29. Drobyshevski, E. M. (1974). "Was Jupiter the protosun's core?". Nature. 250 (5461). Springer Science and Business Media LLC: 35–36. Bibcode:1974Natur.250...35D. doi:10.1038/250035a0. ISSN 0028-0836. S2CID 4290185.
30. Walsh, K. J.; Morbidelli, A.; Raymond, S. N.; O'Brien, D. P.; Mandell, A. M. (2011). "A low mass for Mars from Jupiter's early gas-driven migration". Nature. 475 (7355): 206–209. arXiv:1201.5177. Bibcode:2011Natur.475..206W. doi:10.1038/nature10201. PMID 21642961. S2CID 4431823.
31. Batygin, Konstantin (2015). "Jupiter's decisive role in the inner Solar System's early evolution". Proceedings of the National Academy of Sciences. 112 (14): 4214–4217. arXiv:1503.06945. Bibcode:2015PNAS..112.4214B. doi:10.1073/pnas.1423252112. PMC 4394287. PMID 25831540.
32. Raúl O Chametla; Gennaro D’Angelo; Mauricio Reyes-Ruiz; F Javier Sánchez-Salcedo (March 2020). "Capture and migration of Jupiter and Saturn in mean motion resonance in a gaseous protoplanetary disc". Monthly Notices of the Royal Astronomical Society. 492 (4): 6007–6018. arXiv:2001.09235. doi:10.1093/mnras/staa260.
33. Haisch Jr., K. E.; Lada, E. A.; Lada, C. J. (2001). "Disc Frequencies and Lifetimes in Young Clusters". The Astrophysical Journal. 553 (2): 153–156. arXiv:astro-ph/0104347. Bibcode:2001ApJ...553L.153H. doi:10.1086/320685. S2CID 16480998.
34. Fazekas, Andrew (March 24, 2015). "Observe: Jupiter, Wrecking Ball of Early Solar System". National Geographic. Archived from the original on March 14, 2017. Retrieved April 18, 2021.
35. Zube, N.; Nimmo, F.; Fischer, R.; Jacobson, S. (2019). "Constraints on terrestrial planet formation timescales and equilibration processes in the Grand Tack scenario from Hf-W isotopic evolution". Earth and Planetary Science Letters. 522 (1): 210–218. arXiv:1910.00645. Bibcode:2019E&PSL.522..210Z. doi:10.1016/j.epsl.2019.07.001. PMC 7339907. PMID 32636530. S2CID 199100280.
36. D'Angelo, G.; Marzari, F. (2012). "Outward Migration of Jupiter and Saturn in Evolved Gaseous Disks". The Astrophysical Journal. 757 (1): 50 (23 pp.). arXiv:1207.2737. Bibcode:2012ApJ...757...50D. doi:10.1088/0004-637X/757/1/50. S2CID 118587166.
37. Pirani, S.; Johansen, A.; Bitsch, B.; Mustill, A.J.; Turrini, D. (March 2019). "Consequences of planetary migration on the minor bodies of the early solar system". Astronomy & Astrophysics. 623: A169. arXiv:1902.04591. Bibcode:2019A&A...623A.169P. doi:10.1051/0004-6361/201833713.
38. "Jupiter's Unknown Journey Revealed". ScienceDaily. Lund University. March 22, 2019. Archived from the original on March 22, 2019. Retrieved March 25, 2019.
39. Levison, Harold F.; Morbidelli, Alessandro; Van Laerhoven, Christa; Gomes, R. (2008). "Origin of the structure of the Kuiper belt during a dynamical instability in the orbits of Uranus and Neptune". Icarus. 196 (1): 258–273. arXiv:0712.0553. Bibcode:2008Icar..196..258L. doi:10.1016/j.icarus.2007.11.035. S2CID 7035885.
40. Öberg, K.I.; Wordsworth, R. (2019). "Jupiter's Composition Suggests its Core Assembled Exterior to the N_{2} Snowline". The Astronomical Journal. 158 (5). arXiv:1909.11246. doi:10.3847/1538-3881/ab46a8. S2CID 202749962.
41. Öberg, K.I.; Wordsworth, R. (2020). "Erratum: "Jupiter's Composition Suggests Its Core Assembled Exterior to the N2 Snowline"". The Astronomical Journal. 159 (2): 78. doi:10.3847/1538-3881/ab6172. S2CID 214576608.
42. Denecke, Edward J. (January 7, 2020). Regents Exams and Answers: Earth Science—Physical Setting 2020. Barrons Educational Series. p. 419. ISBN 978-1-5062-5399-2.
43. Swarbrick, James (2013). Encyclopedia of Pharmaceutical Technology. Vol. 6. CRC Press. p. 3601. ISBN 978-1-4398-0823-8. Archived from the original on March 26, 2023. Retrieved March 19, 2023. Syrup USP (1.31 g/cm³)
44. Allen, Clabon Walter; Cox, Arthur N. (2000). Allen's Astrophysical Quantities. Springer. pp. 295–296. ISBN 978-0-387-98746-0. Archived from the original on February 21, 2023. Retrieved March 18, 2022.
45. Polyanin, Andrei D.; Chernoutsan, Alexei (October 18, 2010). A Concise Handbook of Mathematics, Physics, and Engineering Sciences. CRC Press. p. 1041. ISBN 978-1-4398-0640-1.
46. Guillot, Tristan; Gautier, Daniel; Hubbard, William B. (December 1997). "NOTE: New Constraints on the Composition of Jupiter from Galileo Measurements and Interior Models". Icarus. 130 (2): 534–539. arXiv:astro-ph/9707210. Bibcode:1997Icar..130..534G. doi:10.1006/icar.1997.5812. S2CID 5466469.
47. Bagenal, Fran; Dowling, Timothy E.; McKinnon, William B., eds. (2006). Jupiter: The Planet, Satellites and Magnetosphere. Cambridge University Press. pp. 59–75. ISBN 0521035457.
48. Kim, S. J.; Caldwell, J.; Rivolo, A. R.; Wagner, R. (1985). "Infrared Polar Brightening on Jupiter III. Spectrometry from the Voyager 1 IRIS Experiment". Icarus. 64 (2): 233–248. Bibcode:1985Icar...64..233K. doi:10.1016/0019-1035(85)90201-5.
49. Vdovichenko, V. D.; Karimov, A. M.; Kirienko, G. A.; Lysenko, P. G.; Tejfel’, V. G.; Filippov, V. A.; Kharitonova, G. A.; Khozhenets, A. P. (2021). "Zonal Features in the Behavior of Weak Molecular Absorption Bands on Jupiter". Solar System Research. 55 (1): 35–46. Bibcode:2021SoSyR..55...35V. doi:10.1134/S003809462101010X. S2CID 255069821.
50. Gautier, D.; Conrath, B.; Flasar, M.; Hanel, R.; Kunde, V.; Chedin, A.; Scott, N. (1981). "The helium abundance of Jupiter from Voyager". Journal of Geophysical Research. 86 (A10): 8713–8720. Bibcode:1981JGR....86.8713G. doi:10.1029/JA086iA10p08713. hdl:2060/19810016480. S2CID 122314894.
51. Kunde, V. G.; Flasar, F. M.; Jennings, D. E.; Bézard, B.; Strobel, D. F.; et al. (September 10, 2004). "Jupiter's Atmospheric Composition from the Cassini Thermal Infrared Spectroscopy Experiment". Science. 305 (5690): 1582–1586. Bibcode:2004Sci...305.1582K. doi:10.1126/science.1100240. PMID 15319491. S2CID 45296656.
52. "Solar Nebula Supermarket" (PDF). nasa.gov. Archived (PDF) from the original on July 17, 2023. Retrieved July 10, 2023.
53. Niemann, H. B.; Atreya, S. K.; Carignan, G. R.; Donahue, T. M.; Haberman, J. A.; et al. (1996). "The Galileo Probe Mass Spectrometer: Composition of Jupiter's Atmosphere". Science. 272 (5263): 846–849. Bibcode:1996Sci...272..846N. doi:10.1126/science.272.5263.846. PMID 8629016. S2CID 3242002.
54. von Zahn, U.; Hunten, D. M.; Lehmacher, G. (1998). "Helium in Jupiter's atmosphere: Results from the Galileo probe Helium Interferometer Experiment". Journal of Geophysical Research. 103 (E10): 22815–22829. Bibcode:1998JGR...10322815V. doi:10.1029/98JE00695.
55. Stevenson, David J. (May 2020). "Jupiter's Interior as Revealed by Juno". Annual Review of Earth and Planetary Sciences. 48: 465–489. Bibcode:2020AREPS..48..465S. doi:10.1146/annurev-earth-081619-052855. S2CID 212832169.
56. Ingersoll, A. P.; Hammel, H. B.; Spilker, T. R.; Young, R. E. (June 1, 2005). "Outer Planets: The Ice Giants" (PDF). Lunar & Planetary Institute. Archived (PDF) from the original on October 9, 2022. Retrieved February 1, 2007.
57. Hofstadter, Mark (2011), "The Atmospheres of the Ice Giants, Uranus and Neptune" (PDF), White Paper for the Planetary Science Decadal Survey, US National Research Council, pp. 1–2, archived (PDF) from the original on July 17, 2023, retrieved January 18, 2015
58. MacDougal, Douglas W. (2012). "A Binary System Close to Home: How the Moon and Earth Orbit Each Other". Newton's Gravity. Undergraduate Lecture Notes in Physics. Springer New York. pp. 193–211. doi:10.1007/978-1-4614-5444-1_10. ISBN 978-1-4614-5443-4. the barycentre is 743,000 km from the centre of the Sun. The Sun's radius is 696,000 km, so it is 47,000 km above the surface.
59. Burgess, Eric (1982). By Jupiter: Odysseys to a Giant. New York: Columbia University Press. ISBN 978-0-231-05176-7.
60. Shu, Frank H. (1982). The physical universe: an introduction to astronomy. Series of books in astronomy (12th ed.). University Science Books. p. 426. ISBN 978-0-935702-05-7.
61. Davis, Andrew M.; Turekian, Karl K. (2005). Meteorites, comets, and planets. Treatise on geochemistry. Vol. 1. Elsevier. p. 624. ISBN 978-0-08-044720-9.
62. Schneider, Jean (2009). "The Extrasolar Planets Encyclopedia: Interactive Catalogue". Extrasolar Planets Encyclopaedia. Archived from the original on October 28, 2023. Retrieved August 9, 2014.
63. Feng, Fabo; Butler, R. Paul; et al. (August 2022). "3D Selection of 167 Substellar Companions to Nearby Stars". The Astrophysical Journal Supplement Series. 262 (21): 21. arXiv:2208.12720. Bibcode:2022ApJS..262...21F. doi:10.3847/1538-4365/ac7e57. S2CID 251864022.
64. Seager, S.; Kuchner, M.; Hier-Majumder, C. A.; Militzer, B. (2007). "Mass-Radius Relationships for Solid Exoplanets". The Astrophysical Journal. 669 (2): 1279–1297. arXiv:0707.2895. Bibcode:2007ApJ...669.1279S. doi:10.1086/521346. S2CID 8369390.
65. How the Universe Works 3. Vol. Jupiter: Destroyer or Savior?. Discovery Channel. 2014.
66. Guillot, Tristan (1999). "Interiors of Giant Planets Inside and Outside the Solar System" (PDF). Science. 286 (5437): 72–77. Bibcode:1999Sci...286...72G. doi:10.1126/science.286.5437.72. PMID 10506563. Archived (PDF) from the original on October 9, 2022. Retrieved April 24, 2022.
67. Burrows, Adam; Hubbard, W. B.; Lunine, J. I.; Liebert, James (July 2001). "The theory of brown dwarfs and extrasolar giant planets". Reviews of Modern Physics. 73 (3): 719–765. arXiv:astro-ph/0103383. Bibcode:2001RvMP...73..719B. doi:10.1103/RevModPhys.73.719. S2CID 204927572. Hence the HBMM at solar metallicity and Y_α = 50.25 is 0.07 – 0.074 M_☉, ... while the HBMM at zero metallicity is 0.092 M_☉
68. von Boetticher, Alexander; Triaud, Amaury H. M. J.; Queloz, Didier; Gill, Sam; Lendl, Monika; Delrez, Laetitia; Anderson, David R.; Collier Cameron, Andrew; Faedi, Francesca; Gillon, Michaël; Gómez Maqueo Chew, Yilen; Hebb, Leslie; Hellier, Coel; Jehin, Emmanuël; Maxted, Pierre F. L.; Martin, David V.; Pepe, Francesco; Pollacco, Don; Ségransan, Damien; Smalley, Barry; Udry, Stéphane; West, Richard (August 2017). "The EBLM project. III. A Saturn-size low-mass star at the hydrogen-burning limit". Astronomy & Astrophysics. 604: 6. arXiv:1706.08781. Bibcode:2017A&A...604L...6V. doi:10.1051/0004-6361/201731107. S2CID 54610182. L6.
69. Elkins-Tanton, Linda T. (2011). Jupiter and Saturn (revised ed.). New York: Chelsea House. ISBN 978-0-8160-7698-7.
70. Irwin, Patrick (2003). Giant Planets of Our Solar System: Atmospheres, Composition, and Structure. Springer Science & Business Media. p. 62. ISBN 978-3-540-00681-7. Archived from the original on June 19, 2024. Retrieved April 23, 2022.
71. Irwin, Patrick G. J. (2009) [2003]. Giant Planets of Our Solar System: Atmospheres, Composition, and Structure (Second ed.). Springer. p. 4. ISBN 978-3-642-09888-8. Archived from the original on June 19, 2024. Retrieved March 6, 2021. the radius of Jupiter is estimated to be currently shrinking by approximately 1 mm/yr.
72. Guillot, Tristan; Stevenson, David J.; Hubbard, William B.; Saumon, Didier (2004). "Chapter 3: The Interior of Jupiter". In Bagenal, Fran; Dowling, Timothy E.; McKinnon, William B. (eds.). Jupiter: The Planet, Satellites and Magnetosphere. Cambridge University Press. ISBN 978-0-521-81808-7.
73. Bodenheimer, P. (1974). "Calculations of the early evolution of Jupiter". Icarus. 23. 23 (3): 319–325. Bibcode:1974Icar...23..319B. doi:10.1016/0019-1035(74)90050-5.
74. Smoluchowski, R. (1971). "Metallic interiors and magnetic fields of Jupiter and Saturn". The Astrophysical Journal. 166: 435. Bibcode:1971ApJ...166..435S. doi:10.1086/150971.
75. Wahl, S. M.; Hubbard, William B.; Militzer, B.; Guillot, Tristan; Miguel, Y.; Movshovitz, N.; Kaspi, Y.; Helled, R.; Reese, D.; Galanti, E.; Levin, S.; Connerney, J. E.; Bolton, S. J. (2017). "Comparing Jupiter interior structure models to Juno gravity measurements and the role of a dilute core". Geophysical Research Letters. 44 (10): 4649–4659. arXiv:1707.01997. Bibcode:2017GeoRL..44.4649W. doi:10.1002/2017GL073160.
76. Shang-Fei Liu; et al. (August 15, 2019). "The Formation of Jupiter's Diluted Core by a Giant Impact". Nature. 572 (7769): 355–357. arXiv:2007.08338. Bibcode:2019Natur.572..355L. doi:10.1038/s41586-019-1470-2. PMID 31413376. S2CID 199576704.
77. Chang, Kenneth (July 5, 2016). "NASA's Juno Spacecraft Enters Jupiter's Orbit". The New York Times. Archived from the original on May 2, 2019. Retrieved July 5, 2016.
78. Stevenson, D. J.; Bodenheimer, P.; Lissauer, J. J.; D'Angelo, G. (2022). "Mixing of Condensable Constituents with H-He during the Formation and Evolution of Jupiter". The Planetary Science Journal. 3 (4): id.74. arXiv:2202.09476. Bibcode:2022PSJ.....3...74S. doi:10.3847/PSJ/ac5c44. S2CID 247011195.
79. Guillot, T. (2019). "Signs that Jupiter was mixed by a giant impact". Nature. 572 (7769): 315–317. Bibcode:2019Natur.572..315G. doi:10.1038/d41586-019-02401-1. PMID 31413374.
80. Trachenko, K.; Brazhkin, V. V.; Bolmatov, D. (March 2014). "Dynamic transition of supercritical hydrogen: Defining the boundary between interior and atmosphere in gas giants". Physical Review E. 89 (3): 032126. arXiv:1309.6500. Bibcode:2014PhRvE..89c2126T. doi:10.1103/PhysRevE.89.032126. PMID 24730809. S2CID 42559818. 032126.
81. Coulter, Dauna. "A Freaky Fluid inside Jupiter?". NASA. Archived from the original on December 9, 2021. Retrieved December 8, 2021.
82. "NASA System Exploration Jupiter". NASA. Archived from the original on November 4, 2021. Retrieved December 8, 2021.
83. Guillot, T. (1999). "A comparison of the interiors of Jupiter and Saturn". Planetary and Space Science. 47 (10–11): 1183–1200. arXiv:astro-ph/9907402. Bibcode:1999P&SS...47.1183G. doi:10.1016/S0032-0633(99)00043-4. S2CID 19024073. Archived from the original on May 19, 2021. Retrieved June 21, 2023.
84. Lang, Kenneth R. (2003). "Jupiter: a giant primitive planet". NASA. Archived from the original on May 14, 2011. Retrieved January 10, 2007.
85. Lodders, Katharina (2004). "Jupiter Formed with More Tar than Ice" (PDF). The Astrophysical Journal. 611 (1): 587–597. Bibcode:2004ApJ...611..587L. doi:10.1086/421970. S2CID 59361587. Archived from the original (PDF) on April 12, 2020.
86. Brygoo, S.; Loubeyre, P.; Millot, M.; Rygg, J. R.; Celliers, P. M.; Eggert, J. H.; Jeanloz, R.; Collins, G. W. (2021). "Evidence of hydrogen−helium immiscibility at Jupiter-interior conditions". Nature. 593 (7860): 517–521. Bibcode:2021Natur.593..517B. doi:10.1038/s41586-021-03516-0. OSTI 1820549. PMID 34040210. S2CID 235217898.
87. Kramer, Miriam (October 9, 2013). "Diamond Rain May Fill Skies of Jupiter and Saturn". Space.com. Archived from the original on August 27, 2017. Retrieved August 27, 2017.
88. Kaplan, Sarah (August 25, 2017). "It rains solid diamonds on Uranus and Neptune". The Washington Post. Archived from the original on August 27, 2017. Retrieved August 27, 2017.
89. Guillot, Tristan; Stevenson, David J.; Hubbard, William B.; Saumon, Didier (2004). "The interior of Jupiter". In Bagenal, Fran; Dowling, Timothy E.; McKinnon, William B. (eds.). Jupiter. The planet, satellites and magnetosphere. Cambridge planetary science. Vol. 1. Cambridge, UK: Cambridge University Press. p. 45. Bibcode:2004jpsm.book...35G. ISBN 0-521-81808-7. Archived from the original on March 26, 2023. Retrieved March 19, 2023.
90. Atreya, Sushil K.; Mahaffy, P. R.; Niemann, H. B.; Wong, M. H.; Owen, T. C. (February 2003). "Composition and origin of the atmosphere of Jupiter—an update, and implications for the extrasolar giant planets". Planetary and Space Science. 51 (2): 105–112. Bibcode:2003P&SS...51..105A. doi:10.1016/S0032-0633(02)00144-7.
91. Loeffler, Mark J.; Hudson, Reggie L. (March 2018). "Coloring Jupiter's clouds: Radiolysis of ammonium hydrosulfide (NH4SH)" (PDF). Icarus. 302: 418–425. Bibcode:2018Icar..302..418L. doi:10.1016/j.icarus.2017.10.041. Archived (PDF) from the original on October 9, 2022. Retrieved April 25, 2022.
92. Ingersoll, Andrew P.; Dowling, Timothy E.; Gierasch, Peter J.; Orton, Glenn S.; Read, Peter L.; Sánchez-Lavega, Agustin; Showman, Adam P.; Simon-Miller, Amy A.; Vasavada, Ashwin R. (2004). Bagenal, Fran; Dowling, Timothy E.; McKinnon, William B. (eds.). "Dynamics of Jupiter's Atmosphere" (PDF). Jupiter. The Planet, Satellites and Magnetosphere. Cambridge planetary science. 1. Cambridge, UK: Cambridge University Press: 105–128. ISBN 0-521-81808-7. Archived (PDF) from the original on October 9, 2022. Retrieved March 8, 2022.
93. Aglyamov, Yury S.; Lunine, Jonathan; Becker, Heidi N.; Guillot, Tristan; Gibbard, Seran G.; Atreya, Sushil; Bolton, Scott J.; Levin, Steven; Brown, Shannon T.; Wong, Michael H. (February 2021). "Lightning Generation in Moist Convective Clouds and Constraints on the Water Abundance in Jupiter". Journal of Geophysical Research: Planets. 126 (2). arXiv:2101.12361. Bibcode:2021JGRE..12606504A. doi:10.1029/2020JE006504. S2CID 231728590. e06504.
94. Watanabe, Susan, ed. (February 25, 2006). "Surprising Jupiter: Busy Galileo spacecraft showed jovian system is full of surprises". NASA. Archived from the original on October 8, 2011. Retrieved February 20, 2007.
95. Kerr, Richard A. (2000). "Deep, Moist Heat Drives Jovian Weather". Science. 287 (5455): 946–947. doi:10.1126/science.287.5455.946b. S2CID 129284864. Archived from the original on February 3, 2023. Retrieved April 26, 2022.
96. Becker, Heidi N.; Alexander, James W.; Atreya, Sushil K.; Bolton, Scott J.; Brennan, Martin J.; Brown, Shannon T.; Guillaume, Alexandre; Guillot, Tristan; Ingersoll, Andrew P.; Levin, Steven M.; Lunine, Jonathan I.; Aglyamov, Yury S.; Steffes, Paul G. (2020). "Small lightning flashes from shallow electrical storms on Jupiter". Nature. 584 (7819): 55–58. Bibcode:2020Natur.584...55B. doi:10.1038/s41586-020-2532-1. ISSN 0028-0836. PMID 32760043. S2CID 220980694. Archived from the original on September 29, 2021. Retrieved March 6, 2021.
97. Guillot, Tristan; Stevenson, David J.; Atreya, Sushil K.; Bolton, Scott J.; Becker, Heidi N. (2020). "Storms and the Depletion of Ammonia in Jupiter: I. Microphysics of "Mushballs"". Journal of Geophysical Research: Planets. 125 (8): e2020JE006403. arXiv:2012.14316. Bibcode:2020JGRE..12506403G. doi:10.1029/2020JE006404. S2CID 226194362.
98. Giles, Rohini S.; Greathouse, Thomas K.; Bonfond, Bertrand; Gladstone, G. Randall; Kammer, Joshua A.; Hue, Vincent; Grodent, Denis C.; Gérard, Jean-Claude; Versteeg, Maarten H.; Wong, Michael H.; Bolton, Scott J.; Connerney, John E. P.; Levin, Steven M. (2020). "Possible Transient Luminous Events Observed in Jupiter's Upper Atmosphere". Journal of Geophysical Research: Planets. 125 (11): e06659. arXiv:2010.13740. Bibcode:2020JGRE..12506659G. doi:10.1029/2020JE006659. S2CID 225075904. e06659.
99. Greicius, Tony, ed. (October 27, 2020). "Juno Data Indicates 'Sprites' or 'Elves' Frolic in Jupiter's Atmosphere". NASA. Archived from the original on January 27, 2021. Retrieved December 30, 2020.
100. Strycker, P. D.; Chanover, N.; Sussman, M.; Simon-Miller, A. (2006). A Spectroscopic Search for Jupiter's Chromophores. DPS meeting No. 38, #11.15. American Astronomical Society. Bibcode:2006DPS....38.1115S.
101. Gierasch, Peter J.; Nicholson, Philip D. (2004). "Jupiter". World Book @ NASA. Archived from the original on January 5, 2005. Retrieved August 10, 2006.
102. Chang, Kenneth (December 13, 2017). "The Great Red Spot Descends Deep into Jupiter". The New York Times. Archived from the original on December 15, 2017. Retrieved December 15, 2017.
103. Denning, William F. (1899). "Jupiter, early history of the great red spot on". Monthly Notices of the Royal Astronomical Society. 59 (10): 574–584. Bibcode:1899MNRAS..59..574D. doi:10.1093/mnras/59.10.574.
104. Kyrala, A. (1982). "An explanation of the persistence of the Great Red Spot of Jupiter". Moon and the Planets. 26 (1): 105–107. Bibcode:1982M&P....26..105K. doi:10.1007/BF00941374. S2CID 121637752.
105. Oldenburg, Henry, ed. (1665–1666). "Philosophical Transactions of the Royal Society". Project Gutenberg. Archived from the original on March 4, 2016. Retrieved December 22, 2011.
106. Wong, M.; de Pater, I. (May 22, 2008). "New Red Spot Appears on Jupiter". HubbleSite. NASA. Archived from the original on December 16, 2013. Retrieved December 12, 2013.
107. Simon-Miller, A.; Chanover, N.; Orton, G. (July 17, 2008). "Three Red Spots Mix It Up on Jupiter". HubbleSite. NASA. Archived from the original on May 1, 2015. Retrieved April 26, 2015.
108. Covington, Michael A. (2002). Celestial Objects for Modern Telescopes. Cambridge University Press. p. 53. ISBN 978-0-521-52419-3.
109. Cardall, C. Y.; Daunt, S. J. "The Great Red Spot". University of Tennessee. Archived from the original on March 31, 2010. Retrieved February 2, 2007.
110. Jupiter, the Giant of the Solar System. NASA. 1979. p. 5. Archived from the original on March 26, 2023. Retrieved March 19, 2023.
111. Sromovsky, L. A.; Baines, K. H.; Fry, P. M.; Carlson, R. W. (July 2017). "A possibly universal red chromophore for modeling colour variations on Jupiter". Icarus. 291: 232–244. arXiv:1706.02779. Bibcode:2017Icar..291..232S. doi:10.1016/j.icarus.2016.12.014. S2CID 119036239.
112. White, Greg (November 25, 2015). "Is Jupiter's Great Red Spot nearing its twilight?". Space.news. Archived from the original on April 14, 2017. Retrieved April 13, 2017.
113. Sommeria, Jöel; Meyers, Steven D.; Swinney, Harry L. (February 25, 1988). "Laboratory simulation of Jupiter's Great Red Spot". Nature. 331 (6158): 689–693. Bibcode:1988Natur.331..689S. doi:10.1038/331689a0. S2CID 39201626.
114. Simon, Amy A.; Wong, M. H.; Rogers, J. H.; Orton, G. S.; de Pater, I.; Asay-Davis, X.; Carlson, R. W.; Marcus, P. S. (March 2015). Dramatic Change in Jupiter's Great Red Spot. 46th Lunar and Planetary Science Conference. March 16–20, 2015. The Woodlands, Texas. Bibcode:2015LPI....46.1010S.
115. Doctor, Rina Marie (October 21, 2015). "Jupiter's Superstorm Is Shrinking: Is Changing Red Spot Evidence Of Climate Change?". Tech Times. Archived from the original on April 14, 2017. Retrieved April 13, 2017.
116. Grush, Loren (October 28, 2021). "NASA's Juno spacecraft finds just how deep Jupiter's Great Red Spot goes". The Verge. Archived from the original on October 28, 2021. Retrieved October 28, 2021.
117. Adriani, Alberto; Mura, A.; Orton, G.; Hansen, C.; Altieri, F.; et al. (March 2018). "Clusters of cyclones encircling Jupiter's poles". Nature. 555 (7695): 216–219. Bibcode:2018Natur.555..216A. doi:10.1038/nature25491. PMID 29516997. S2CID 4438233.
118. Starr, Michelle (December 13, 2017). "NASA Just Watched a Mass of Cyclones on Jupiter Evolve Into a Mesmerising Hexagon". Science Alert. Archived from the original on May 26, 2021. Retrieved May 26, 2021.
119. Steigerwald, Bill (October 14, 2006). "Jupiter's Little Red Spot Growing Stronger". NASA. Archived from the original on April 5, 2012. Retrieved February 2, 2007.
120. Wong, Michael H.; de Pater, Imke; Asay-Davis, Xylar; Marcus, Philip S.; Go, Christopher Y. (September 2011). "Vertical structure of Jupiter's Oval BA before and after it reddened: What changed?" (PDF). Icarus. 215 (1): 211–225. Bibcode:2011Icar..215..211W. doi:10.1016/j.icarus.2011.06.032. Archived (PDF) from the original on October 9, 2022. Retrieved April 27, 2022.
121. Stallard, Tom S.; Melin, Henrik; Miller, Steve; Moore, Luke; O'Donoghue, James; Connerney, John E. P.; Satoh, Takehiko; West, Robert A.; Thayer, Jeffrey P.; Hsu, Vicki W.; Johnson, Rosie E. (April 10, 2017). "The Great Cold Spot in Jupiter's upper atmosphere". Geophysical Research Letters. 44 (7): 3000–3008. Bibcode:2017GeoRL..44.3000S. doi:10.1002/2016GL071956. PMC 5439487. PMID 28603321.
122. Connerney, J. E. P.; Kotsiaros, S.; Oliversen, R. J.; Espley, J. R.; Joergensen, J. L.; Joergensen, P. S.; Merayo, J. M. G.; Herceg, M.; Bloxham, J.; Moore, K. M.; Bolton, S. J.; Levin, S. M. (May 26, 2017). "A New Model of Jupiter's Magnetic Field From Juno's First Nine Orbits" (PDF). Geophysical Research Letters. 45 (6): 2590–2596. Bibcode:2018GeoRL..45.2590C. doi:10.1002/2018GL077312. Archived (PDF) from the original on October 9, 2022.
123. Brainerd, Jim (November 22, 2004). "Jupiter's Magnetosphere". The Astrophysics Spectator. Archived from the original on January 25, 2021. Retrieved August 10, 2008.
124. "Receivers for Radio JOVE". NASA. March 1, 2017. Archived from the original on January 26, 2021. Retrieved September 9, 2020.
125. Phillips, Tony; Horack, John M. (February 20, 2004). "Radio Storms on Jupiter". NASA. Archived from the original on February 13, 2007. Retrieved February 1, 2007.
126. Ringwald, Frederick A. (February 29, 2000). "SPS 1020 (Introduction to Space Sciences)". California State University, Fresno. Archived from the original on July 25, 2008. Retrieved January 5, 2014.
127. Showalter, M. A.; Burns, J. A.; Cuzzi, J. N.; Pollack, J. B. (1987). "Jupiter's ring system: New results on structure and particle properties". Icarus. 69 (3): 458–498. Bibcode:1987Icar...69..458S. doi:10.1016/0019-1035(87)90018-2.
128. Burns, J. A.; Showalter, M. R.; Hamilton, D. P.; Nicholson, P. D.; de Pater, I.; Ockert-Bell, M. E.; Thomas, P. C. (1999). "The Formation of Jupiter's Faint Rings". Science. 284 (5417): 1146–1150. Bibcode:1999Sci...284.1146B. doi:10.1126/science.284.5417.1146. PMID 10325220. S2CID 21272762.
129. Fieseler, P. D.; Adams, O. W.; Vandermey, N.; Theilig, E. E.; Schimmels, K. A.; Lewis, G. D.; Ardalan, S. M.; Alexander, C. J. (2004). "The Galileo Star Scanner Observations at Amalthea". Icarus. 169 (2): 390–401. Bibcode:2004Icar..169..390F. doi:10.1016/j.icarus.2004.01.012.
130. Herbst, T. M.; Rix, H.-W. (1999). "Star Formation and Extrasolar Planet Studies with Near-Infrared Interferometry on the LBT". In Guenther, Eike; Stecklum, Bringfried; Klose, Sylvio (eds.). Optical and Infrared Spectroscopy of Circumstellar Matter. ASP Conference Series. Vol. 188. San Francisco, Calif.: Astronomical Society of the Pacific. pp. 341–350. Bibcode:1999ASPC..188..341H. ISBN 978-1-58381-014-9. – See section 3.4.
131. MacDougal, Douglas W. (December 16, 2012). Newton's Gravity: An Introductory Guide to the Mechanics of the Universe. Springer New York. p. 199. ISBN 978-1-4614-5444-1.
132. Michtchenko, T. A.; Ferraz-Mello, S. (February 2001). "Modeling the 5:2 Mean-Motion Resonance in the Jupiter–Saturn Planetary System". Icarus. 149 (2): 77–115. Bibcode:2001Icar..149..357M. doi:10.1006/icar.2000.6539.
133. "Simulations explain giant exoplanets with eccentric, close-in orbits". ScienceDaily. October 30, 2019. Archived from the original on July 17, 2023. Retrieved July 17, 2023.
134. "Interplanetary Seasons". Science@NASA. Archived from the original on October 16, 2007. Retrieved February 20, 2007.
135. Ridpath, Ian (1998). Norton's Star Atlas (19th ed.). Prentice Hall. ISBN 978-0-582-35655-9.^{[page needed]}
136. Hide, R. (January 1981). "On the rotation of Jupiter". Geophysical Journal. 64: 283–289. Bibcode:1981GeoJ...64..283H. doi:10.1111/j.1365-246X.1981.tb02668.x.
137. Russell, C. T.; Yu, Z. J.; Kivelson, M. G. (2001). "The rotation period of Jupiter" (PDF). Geophysical Research Letters. 28 (10): 1911–1912. Bibcode:2001GeoRL..28.1911R. doi:10.1029/2001GL012917. S2CID 119706637. Archived (PDF) from the original on October 9, 2022. Retrieved April 28, 2022.
138. Rogers, John H. (July 20, 1995). "Appendix 3". The giant planet Jupiter. Cambridge University Press. ISBN 978-0-521-41008-3.
139. Price, Fred W. (October 26, 2000). The Planet Observer's Handbook. Cambridge University Press. p. 140. ISBN 978-0-521-78981-3. Archived from the original on March 26, 2023. Retrieved March 19, 2023.
140. Fimmel, Richard O.; Swindell, William; Burgess, Eric (1974). "8. Encounter with the Giant". Pioneer Odyssey (Revised ed.). NASA History Office. Archived from the original on December 25, 2017. Retrieved February 17, 2007.
141. Chaple, Glenn F. (2009). Jones, Lauren V.; Slater, Timothy F. (eds.). Outer Planets. Greenwood Guides to the Universe. ABC-CLIO. p. 47. ISBN 978-0-313-36571-3. Archived from the original on March 26, 2023. Retrieved March 19, 2023.
142. North, Chris; Abel, Paul (October 31, 2013). The Sky at Night: How to Read the Solar System. Ebury Publishing. p. 183. ISBN 978-1-4481-4130-2.
143. Sachs, A. (May 2, 1974). "Babylonian Observational Astronomy". Philosophical Transactions of the Royal Society of London. 276 (1257): 43–50 (see p. 44). Bibcode:1974RSPTA.276...43S. doi:10.1098/rsta.1974.0008. JSTOR 74273. S2CID 121539390.
144. Dubs, Homer H. (1958). "The Beginnings of Chinese Astronomy". Journal of the American Oriental Society. 78 (4): 295–300. doi:10.2307/595793. JSTOR 595793.
145. Chen, James L.; Chen, Adam (2015). A Guide to Hubble Space Telescope Objects: Their Selection, Location, and Significance. Springer International Publishing. p. 195. ISBN 978-3-319-18872-0. Archived from the original on March 26, 2023. Retrieved March 19, 2023.
146. Seargent, David A. J. (September 24, 2010). "Facts, Fallacies, Unusual Observations, and Other Miscellaneous Gleanings". Weird Astronomy: Tales of Unusual, Bizarre, and Other Hard to Explain Observations. Astronomers' Universe. pp. 221–282. ISBN 978-1-4419-6424-3.
147. Xi, Z. Z. (1981). "The Discovery of Jupiter's Satellite Made by Gan-De 2000 Years Before Galileo". Acta Astrophysica Sinica. 1 (2): 87. Bibcode:1981AcApS...1...85X.
148. Dong, Paul (2002). China's Major Mysteries: Paranormal Phenomena and the Unexplained in the People's Republic. China Books. ISBN 978-0-8351-2676-2.
149. Ossendrijver, Mathieu (January 29, 2016). "Ancient Babylonian astronomers calculated Jupiter's position from the area under a time-velocity graph". Science. 351 (6272): 482–484. Bibcode:2016Sci...351..482O. doi:10.1126/science.aad8085. PMID 26823423. S2CID 206644971. Archived from the original on August 1, 2022. Retrieved June 30, 2022.
150. Pedersen, Olaf (1974). A Survey of the Almagest. Odense University Press. pp. 423, 428. ISBN 9788774920878.
151. Pasachoff, Jay M. (2015). "Simon Marius's Mundus Iovialis: 400th Anniversary in Galileo's Shadow". Journal for the History of Astronomy. 46 (2): 218–234. Bibcode:2015AAS...22521505P. doi:10.1177/0021828615585493. S2CID 120470649.
152. Westfall, Richard S. "Galilei, Galileo". The Galileo Project. Rice University. Archived from the original on January 23, 2022. Retrieved January 10, 2007.
153. Del Santo, Paolo; Olschki, Leo S. (2009). "On an Unpublished Letter of Francesco Fontana to the Grand-Duke of Tuscany Ferdinand II de' Medici". Galilæana: Journal of Galilean Studies. VI: 1000–1017. Archived from the original on November 15, 2023. Retrieved November 14, 2023. Alternate URL
154. O'Connor, J. J.; Robertson, E. F. (April 2003). "Giovanni Domenico Cassini". University of St. Andrews. Archived from the original on July 7, 2015. Retrieved February 14, 2007.
155. Atkinson, David H.; Pollack, James B.; Seiff, Alvin (September 1998). "The Galileo probe Doppler wind experiment: Measurement of the deep zonal winds on Jupiter". Journal of Geophysical Research. 103 (E10): 22911–22928. Bibcode:1998JGR...10322911A. doi:10.1029/98JE00060.
156. Murdin, Paul (2000). Encyclopedia of Astronomy and Astrophysics. Bristol: Institute of Physics Publishing. ISBN 978-0-12-226690-4.
157. Rogers, John H. (1995). The giant planet Jupiter. Cambridge University Press. pp. 188–189. ISBN 978-0-521-41008-3. Archived from the original on March 26, 2023. Retrieved March 19, 2023.
158. Fimmel, Richard O.; Swindell, William; Burgess, Eric (August 1974). "Jupiter, Giant of the Solar System". Pioneer Odyssey (Revised ed.). NASA History Office. Archived from the original on August 23, 2006. Retrieved August 10, 2006.
159. Brown, Kevin (2004). "Roemer's Hypothesis". MathPages. Archived from the original on September 6, 2012. Retrieved January 12, 2007.
160. Bobis, Laurence; Lequeux, James (July 2008). "Cassini, Rømer, and the velocity of light". Journal of Astronomical History and Heritage. 11 (2): 97–105. Bibcode:2008JAHH...11...97B. doi:10.3724/SP.J.1440-2807.2008.02.02. S2CID 115455540.
161. Tenn, Joe (March 10, 2006). "Edward Emerson Barnard". Sonoma State University. Archived from the original on September 17, 2011. Retrieved January 10, 2007.
162. "Amalthea Fact Sheet". NASA/JPL. October 1, 2001. Archived from the original on November 24, 2001. Retrieved February 21, 2007.
163. Dunham Jr., Theodore (1933). "Note on the Spectra of Jupiter and Saturn". Publications of the Astronomical Society of the Pacific. 45 (263): 42–44. Bibcode:1933PASP...45...42D. doi:10.1086/124297.
164. Youssef, A.; Marcus, P. S. (2003). "The dynamics of jovian white ovals from formation to merger". Icarus. 162 (1): 74–93. Bibcode:2003Icar..162...74Y. doi:10.1016/S0019-1035(02)00060-X.
165. Weintraub, Rachel A. (September 26, 2005). "How One Night in a Field Changed Astronomy". NASA. Archived from the original on July 3, 2011. Retrieved February 18, 2007.
166. Garcia, Leonard N. "The Jovian Decametric Radio Emission". NASA. Archived from the original on March 2, 2012. Retrieved February 18, 2007.
167. Klein, M. J.; Gulkis, S.; Bolton, S. J. (1996). "Jupiter's Synchrotron Radiation: Observed Variations Before, During and After the Impacts of Comet SL9". Conference at University of Graz. NASA: 217. Bibcode:1997pre4.conf..217K. Archived from the original on November 17, 2015. Retrieved February 18, 2007.
168. "The Pioneer Missions". NASA. March 26, 2007. Archived from the original on December 23, 2018. Retrieved February 26, 2021.
169. "NASA Glenn Pioneer Launch History". NASA – Glenn Research Center. March 7, 2003. Archived from the original on July 13, 2017. Retrieved December 22, 2011.
170. Fortescue, Peter W.; Stark, John; Swinerd, Graham (2003). Spacecraft systems engineering (3rd ed.). John Wiley and Sons. p. 150. ISBN 978-0-470-85102-9.
171. Hirata, Chris. "Delta-V in the Solar System". California Institute of Technology. Archived from the original on July 15, 2006. Retrieved November 28, 2006.
172. Wong, Al (May 28, 1998). "Galileo FAQ: Navigation". NASA. Archived from the original on January 5, 1997. Retrieved November 28, 2006.
173. Chan, K.; Paredes, E. S.; Ryne, M. S. (2004). "Ulysses Attitude and Orbit Operations: 13+ Years of International Cooperation". Space OPS 2004 Conference. American Institute of Aeronautics and Astronautics. doi:10.2514/6.2004-650-447.
174. Lasher, Lawrence (August 1, 2006). "Pioneer Project Home Page". NASA Space Projects Division. Archived from the original on January 1, 2006. Retrieved November 28, 2006.
175. "Jupiter". NASA/JPL. January 14, 2003. Archived from the original on June 28, 2012. Retrieved November 28, 2006.
176. Hansen, C. J.; Bolton, S. J.; Matson, D. L.; Spilker, L. J.; Lebreton, J.-P. (2004). "The Cassini–Huygens flyby of Jupiter". Icarus. 172 (1): 1–8. Bibcode:2004Icar..172....1H. doi:10.1016/j.icarus.2004.06.018.
177. "Pluto-Bound New Horizons Sees Changes in Jupiter System". NASA. October 9, 2007. Archived from the original on November 27, 2020. Retrieved February 26, 2021.
178. "Pluto-Bound New Horizons Provides New Look at Jupiter System". NASA. May 1, 2007. Archived from the original on December 12, 2010. Retrieved July 27, 2007.
179. McConnell, Shannon (April 14, 2003). "Galileo: Journey to Jupiter". NASA/JPL. Archived from the original on November 3, 2004. Retrieved November 28, 2006.
180. Magalhães, Julio (December 10, 1996). "Galileo Probe Mission Events". NASA Space Projects Division. Archived from the original on January 2, 2007. Retrieved February 2, 2007.
181. Goodeill, Anthony (March 31, 2008). "New Frontiers – Missions – Juno". NASA. Archived from the original on February 3, 2007. Retrieved January 2, 2007.
182. "Juno, NASA's Jupiter probe". The Planetary Society. Archived from the original on May 12, 2022. Retrieved April 27, 2022.
183. Jet Propulsion Laboratory (June 17, 2016). "NASA's Juno spacecraft to risk Jupiter's fireworks for science". phys.org. Archived from the original on August 9, 2022. Retrieved April 10, 2022.
184. Firth, Niall (September 5, 2016). "NASA's Juno probe snaps first images of Jupiter's north pole". New Scientist. Archived from the original on September 6, 2016. Retrieved September 5, 2016.
185. Clark, Stephen (February 21, 2017). "NASA's Juno spacecraft to remain in current orbit around Jupiter". Spaceflight Now. Archived from the original on February 26, 2017. Retrieved April 26, 2017.
186. Agle, D. C.; Wendel, JoAnna; Schmid, Deb (June 6, 2018). "NASA Re-plans Juno's Jupiter Mission". NASA/JPL. Archived from the original on July 24, 2020. Retrieved January 5, 2019.
187. Talbert, Tricia (January 8, 2021). "NASA Extends Exploration for Two Planetary Science Missions". NASA. Archived from the original on January 11, 2021. Retrieved January 11, 2021.
188. Dickinson, David (February 21, 2017). "Juno Will Stay in Current Orbit Around Jupiter". Sky & Telescope. Archived from the original on January 8, 2018. Retrieved January 7, 2018.
189. Bartels, Meghan (July 5, 2016). "To protect potential alien life, NASA will destroy its $1 billion Jupiter spacecraft on purpose". Business Insider. Archived from the original on January 8, 2018. Retrieved January 7, 2018.
190. Sori, Mike (April 10, 2023). "Jupiter's moons hide giant subsurface oceans – two missions are sending spacecraft to see if these moons could support life". The Conversation. Archived from the original on May 12, 2023. Retrieved May 12, 2023.
191. Berger, Brian (February 7, 2005). "White House scales back space plans". MSNBC. Archived from the original on October 29, 2013. Retrieved January 2, 2007.
192. "Laplace: A mission to Europa & Jupiter system". European Space Agency. Archived from the original on July 14, 2012. Retrieved January 23, 2009.
193. Favata, Fabio (April 19, 2011). "New approach for L-class mission candidates". European Space Agency. Archived from the original on April 2, 2013. Retrieved May 2, 2012.
194. "European Space Agency: Blast off for Jupiter icy moons mission". BBC News. April 14, 2023. Archived from the original on April 14, 2023. Retrieved April 14, 2023.
195. Foust, Jeff (July 10, 2020). "Cost growth prompts changes to Europa Clipper instruments". Space News. Archived from the original on September 29, 2021. Retrieved July 10, 2020.
196. Jones, Andrew (January 12, 2021). "Jupiter Mission by China Could Include Callisto Landing". The Planetary Society. Archived from the original on April 27, 2021. Retrieved April 27, 2020.
197. Jones, Andrew (April 16, 2021). "China to launch a pair of spacecraft towards the edge of the solar system". Space News. Archived from the original on May 15, 2021. Retrieved April 27, 2020.
198. Billings, Lee (November 12, 2019). "Proposed Interstellar Mission Reaches for the Stars, One Generation at a Time". Scientific American. Archived from the original on July 25, 2021. Retrieved April 27, 2020.
199. Hecht, Jeff (January 31, 2023). "Astronomers Find a Dozen More Moons for Jupiter". Sky & Telescope. Archived from the original on January 31, 2023. Retrieved February 1, 2023.
200. Greenfieldboyce, Nell (February 9, 2023). "Here's why Jupiter's tally of moons keeps going up and up". NPR. Archived from the original on March 5, 2023. Retrieved March 29, 2023.
201. Carter, Jamie (2015). A Stargazing Program for Beginners. Springer International Publishing. p. 104. ISBN 978-3-319-22072-7.
202. Musotto, S.; Varadi, F.; Moore, W. B.; Schubert, G. (2002). "Numerical simulations of the orbits of the Galilean satellites". Icarus. 159 (2): 500–504. Bibcode:2002Icar..159..500M. doi:10.1006/icar.2002.6939. Archived from the original on August 10, 2011. Retrieved February 19, 2007.
203. Lang, Kenneth R. (March 3, 2011). The Cambridge Guide to the Solar System. Cambridge University Press. p. 304. ISBN 978-1-139-49417-5.
204. McFadden, Lucy-Ann; Weissmann, Paul; Johnson, Torrence (2006). Encyclopedia of the Solar System. Elsevier Science. p. 446. ISBN 978-0-08-047498-4.
205. Kessler, Donald J. (October 1981). "Derivation of the collision probability between orbiting objects: the lifetimes of jupiter's outer moons". Icarus. 48 (1): 39–48. Bibcode:1981Icar...48...39K. doi:10.1016/0019-1035(81)90151-2. S2CID 122395249. Archived from the original on September 29, 2021. Retrieved December 30, 2020.
206. Hamilton, Thomas W. M. (2013). Moons of the Solar System. SPBRA. p. 14. ISBN 978-1-62516-175-8.
207. Jewitt, D. C.; Sheppard, S.; Porco, C. (2004). Bagenal, F.; Dowling, T.; McKinnon, W. (eds.). Jupiter: The Planet, Satellites and Magnetosphere (PDF). Cambridge University Press. ISBN 978-0-521-81808-7. Archived from the original (PDF) on March 26, 2009.
208. Nesvorný, D.; Alvarellos, J. L. A.; Dones, L.; Levison, H. F. (2003). "Orbital and Collisional Evolution of the Irregular Satellites" (PDF). The Astronomical Journal. 126 (1): 398–429. Bibcode:2003AJ....126..398N. doi:10.1086/375461. S2CID 8502734. Archived (PDF) from the original on August 1, 2020. Retrieved August 25, 2019.
209. "Planetary Satellite Mean Orbital Parameters". JPL, NASA. August 23, 2013. Archived from the original on November 3, 2013. Retrieved February 1, 2016., and references therein.
210. Showman, A. P.; Malhotra, R. (1999). "The Galilean Satellites". Science. 286 (5437): 77–84. Bibcode:1999Sci...296...77S. doi:10.1126/science.286.5437.77. PMID 10506564. S2CID 9492520.
211. Sheppard, Scott S.; Jewitt, David C. (May 2003). "An abundant population of small irregular satellites around Jupiter" (PDF). Nature. 423 (6937): 261–263. Bibcode:2003Natur.423..261S. doi:10.1038/nature01584. PMID 12748634. S2CID 4424447. Archived from the original (PDF) on August 13, 2006.
212. Nesvorný, David; Beaugé, Cristian; Dones, Luke; Levison, Harold F. (July 2003). "Collisional Origin of Families of Irregular Satellites" (PDF). The Astronomical Journal. 127 (3): 1768–1783. Bibcode:2004AJ....127.1768N. doi:10.1086/382099. S2CID 27293848. Archived (PDF) from the original on October 9, 2022.
213. Ferraz-Mello, S. (1994). Milani, Andrea; Di Martino, Michel; Cellino, A. (eds.). Kirkwood Gaps and Resonant Groups. Asteroids, Comets, Meteors 1993: Proceedings of the 160th Symposium of the International Astronomical Union, held in Belgirate, Italy, June 14–18, 1993, International Astronomical Union. Symposium no. 160. Dordrecht: Kluwer Academic Publishers. p. 175. Bibcode:1994IAUS..160..175F.
214. Kerr, Richard A. (2004). "Did Jupiter and Saturn Team Up to Pummel the Inner Solar System?". Science. 306 (5702): 1676. doi:10.1126/science.306.5702.1676a. PMID 15576586. S2CID 129180312.
215. "List Of Jupiter Trojans". IAU Minor Planet Center. Archived from the original on July 25, 2011. Retrieved October 24, 2010.
216. Cruikshank, D. P.; Dalle Ore, C. M.; Geballe, T. R.; Roush, T. L.; Owen, T. C.; Cash, Michele; de Bergh, C.; Hartmann, W. K. (October 2000). "Trojan Asteroid 624 Hektor: Constraints on Surface Composition". Bulletin of the American Astronomical Society. 32: 1027. Bibcode:2000DPS....32.1901C.
217. Quinn, T.; Tremaine, S.; Duncan, M. (1990). "Planetary perturbations and the origins of short-period comets". Astrophysical Journal, Part 1. 355: 667–679. Bibcode:1990ApJ...355..667Q. doi:10.1086/168800.
218. "Caught in the act: Fireballs light up Jupiter". ScienceDaily. September 10, 2010. Archived from the original on April 27, 2022. Retrieved April 26, 2022.
219. Nakamura, T.; Kurahashi, H. (1998). "Collisional Probability of Periodic Comets with the Terrestrial Planets: An Invalid Case of Analytic Formulation". Astronomical Journal. 115 (2): 848–854. Bibcode:1998AJ....115..848N. doi:10.1086/300206.
220. Horner, J.; Jones, B. W. (2008). "Jupiter – friend or foe? I: the asteroids". International Journal of Astrobiology. 7 (3–4): 251–261. arXiv:0806.2795. Bibcode:2008IJAsB...7..251H. doi:10.1017/S1473550408004187. S2CID 8870726.
221. Overbye, Dennis (July 25, 2009). "Jupiter: Our Cosmic Protector?". The New York Times. Archived from the original on April 24, 2012. Retrieved July 27, 2009.
222. "In Depth | P/Shoemaker-Levy 9". NASA Solar System Exploration. Archived from the original on February 2, 2022. Retrieved December 3, 2021.
223. Howell, Elizabeth (January 24, 2018). "Shoemaker-Levy 9: Comet's Impact Left Its Mark on Jupiter". Space.com. Archived from the original on December 6, 2021. Retrieved December 3, 2021.
224. [e-mail]. "The Big Comet Crash of 1994 – Intensive Observational Campaign at ESO". www.eso.org. Archived from the original on December 3, 2021. Retrieved December 3, 2021.
225. "Top 20 Comet Shoemaker-Levy Images". www2.jpl.nasa.gov. Archived from the original on November 27, 2021. Retrieved December 3, 2021.
226. Savage, Donald; Elliott, Jim; Villard, Ray (December 30, 2004). "Hubble Observations Shed New Light on Jupiter Collision". nssdc.gsfc.nasa.gov. Archived from the original on November 12, 2021. Retrieved December 3, 2021.
227. "NASA TV Coverage on Comet Shoemaker-Levy". www2.jpl.nasa.gov. Archived from the original on September 8, 2021. Retrieved December 3, 2021.
228. Tabe, Isshi; Watanabe, Jun-ichi; Jimbo, Michiwo (February 1997). "Discovery of a Possible Impact SPOT on Jupiter Recorded in 1690". Publications of the Astronomical Society of Japan. 49: L1–L5. Bibcode:1997PASJ...49L...1T. doi:10.1093/pasj/49.1.l1.
229. "Stargazers prepare for daylight view of Jupiter". ABC News. June 16, 2005. Archived from the original on May 12, 2011. Retrieved February 28, 2008.
230. Rogers, J. H. (1998). "Origins of the ancient constellations: I. The Mesopotamian traditions". Journal of the British Astronomical Association. 108: 9–28. Bibcode:1998JBAA..108....9R.
231. Waerden, B. L. (1974). "Old-Babylonian Astronomy" (PDF). Science Awakening II. Dordrecht: Springer. pp. 46–59. doi:10.1007/978-94-017-2952-9_3. ISBN 978-90-481-8247-3. Archived (PDF) from the original on March 21, 2022. Retrieved March 21, 2022.
232. "Greek Names of the Planets". April 25, 2010. Archived from the original on May 9, 2010. Retrieved July 14, 2012. In Greek the name of the planet Jupiter is Dias, the Greek name of god Zeus. See also the Greek article about the planet.
233. Cicero, Marcus Tullius (1888). Cicero's Tusculan Disputations; also, Treatises on The Nature of the Gods, and on The Commonwealth. Translated by Yonge, Charles Duke. New York, NY: Harper & Brothers. p. 274 – via Internet Archive.
234. Cicero, Marcus Tullus (1967) [1933]. Warmington, E. H. (ed.). De Natura Deorum [On The Nature of the Gods]. Cicero. Vol. 19. Translated by Rackham, H. Cambridge, MA: Cambridge University Press. p. 175 – via Internet Archive.
235. Zolotnikova, O. (2019). "Mythologies in contact: Syro-Phoenician traits in Homeric Zeus". The Scientific Heritage. 41 (5): 16–24. Archived from the original on August 9, 2022. Retrieved April 26, 2022.
236. Tarnas, R. (2009). "The planets". Archai: The Journal of Archetypal Cosmology. 1 (1): 36–49. CiteSeerX 10.1.1.456.5030.
237. Harper, Douglas (November 2001). "Jupiter". Online Etymology Dictionary. Archived from the original on September 28, 2008. Retrieved February 23, 2007.
238. Vytautas Tumėnas (2016). "The Common Attributes Between The Baltic Thunder God Perkunas And His Antique Equivalents Jupiter And Zeus" (PDF). Mediterranean Archaeology and Archaeometry. 16 (4): 359–367. Archived (PDF) from the original on July 19, 2023. Retrieved July 19, 2023.
239. "Guru". Indian Divinity.com. Archived from the original on September 16, 2008. Retrieved February 14, 2007.
240. Sanathana, Y. S.; Manjil, Hazarika (November 27, 2020). "Astrolatry in the Brahmaputra Valley: Reflecting upon the Navagraha Sculptural Depiction" (PDF). Heritage: Journal of Multidisciplinary Studies in Archaeology. 8 (2): 157–174. Archived (PDF) from the original on October 9, 2022. Retrieved July 4, 2022.^{[dead link‍]}
241. "Türk Astrolojisi-2" (in Turkish). NTV. Archived from the original on January 4, 2013. Retrieved April 23, 2010.
242. De Groot, Jan Jakob Maria (1912). Religion in China: universism. a key to the study of Taoism and Confucianism. American lectures on the history of religions. Vol. 10. G.P. Putnam's Sons. p. 300. Archived from the original on February 26, 2024. Retrieved January 8, 2010.
243. Crump, Thomas (1992). The Japanese numbers game: the use and understanding of numbers in modern Japan. Nissan Institute/Routledge Japanese studies series. Routledge. pp. 39–40. ISBN 978-0-415-05609-0.
244. Hulbert, Homer Bezaleel (1909). The passing of Korea. Doubleday, Page & Company. p. 426. Retrieved January 8, 2010.

Further reading

• Bagenal, Fran; Dowling, Timothy E.; McKinnon, William B. (2006). Jupiter: The Planet, Satellites and Magnetosphere. Cambridge University Press. ISBN 978-0-52-103545-3 – via Google Books.
• Lohninger, Hans; et al. (November 2, 2005). "Jupiter, As Seen By Voyager 1". A Trip into Space. Virtual Institute of Applied Science.

External links

• Jupiter overview by NASA's Science Mission Directorate
• Simulation of the 62 moons of Jupiter from Tony Dunn's Gravity Simulator website.
• Photographs of Jupiter circa 1920s from the Lick Observatory Records Digital Archive, at the University of California, Santa Cruz Library's Digital Collections.
• Interactive 3D gravity simulation of the Jovian system.
• Video on YouTube of the 2010 Jupiter impact event by an amateur astronomer.
• Animation on YouTube of the Juno spacecraft's flyby of Ganymede and Jupiter by NASA.