Atmosphere of Jupiter

The atmosphere of Jupiter is the largest planetary atmosphere in the Solar System. It is mostly made of molecular hydrogen and helium in roughly solar proportions; other chemical compounds are present only in small amounts and include methane, ammonia, hydrogen sulfide and water. Although water is thought to reside deep in the atmosphere, its directly measured concentration is very low. The oxygen, nitrogen, sulfur, and noble gas abundances in Jupiter's atmosphere exceed solar values by a factor of about three.[1] The atmosphere of Jupiter lacks a clear lower boundary and gradually transitions into the fluid interior of the planet.[2] From lowest to highest, the atmospheric layers are the troposphere, stratosphere, thermosphere and exosphere. Each layer has characteristic temperature gradients.[3] The lowest layer, the troposphere, has a complicated system of clouds and hazes, comprising layers of ammonia, ammonium hydrosulfide and water.[4] The upper ammonia clouds visible at Jupiter's surface are organized in a dozen zonal bands parallel to the equator and are bounded by powerful zonal atmospheric flows (winds) known as jets. The bands alternate in color: the dark bands are called belts, while light ones are called zones. Zones, which are colder than belts, correspond to upwellings, while belts mark descending air.[5] The zones' lighter color is believed to result from ammonia ice; what gives the belts their darker colors is not known with certainty.[5] The origins of the banded structure and jets are not well understood, though two models exist. The shallow model holds that they are surface phenomena overlaying a stable interior. In the deep model, the bands and jets are just surface manifestations of deep circulation in Jupiter's mantle of molecular hydrogen, which is organized in a number of cylinders.[6]

Cloud pattern on Jupiter

The Jovian atmosphere shows a wide range of active phenomena, including band instabilities, vortices (cyclones and anticyclones), storms and lightning.[7] The vortices reveal themselves as large red, white or brown spots (ovals). The largest two spots are the Great Red Spot (GRS)[8] and Oval BA,[9] which is also red. These two and most of the other large spots are anticyclonic. Smaller anticyclones tend to be white. Vortices are thought to be relatively shallow structures with depths not exceeding several hundred kilometers. Located in the southern hemisphere, the GRS is the largest known vortex in the Solar System. It could engulf several Earths and has existed for at least three hundred years. Oval BA, south of GRS, is a red spot a third the size of GRS that formed in 2000 from the merging of three white ovals.[10]

Jupiter has powerful storms, always accompanied by lightning strikes. The storms are a result of moist convection in the atmosphere connected to the evaporation and condensation of water. They are sites of strong upward motion of the air, which leads to the formation of bright and dense clouds. The storms form mainly in belt regions. The lightning strikes on Jupiter are more powerful than those on Earth. However, there are fewer of them, and the average levels of lightning activity are comparable to those on Earth.[11]

Vertical structure

Vertical structure of the atmosphere of Jupiter (*). Note that the pressure drops together with altitude. The Galileo atmospheric probe stopped transmitting at a depth of 132 km.[3]

The atmosphere of Jupiter is classified into four layers, by increasing altitude: the troposphere, stratosphere, thermosphere and exosphere. Unlike the Earth's atmosphere, Jupiter's lacks a mesosphere.[12] Jupiter does not have a solid surface, and the lowest atmospheric layer, the troposphere, smoothly transitions into the planet's fluid interior.[2] This is a result of having temperatures and the pressures well above those of the critical points for hydrogen and helium, meaning that there is no sharp boundary between gas and liquid phases.[2]

Since the lower boundary of the atmosphere is ill-defined, the pressure level of 10 bars, at an altitude of about 90 km below the 1 bar with a temperature of around 340 K, is commonly treated as the base of the troposphere.[3] In scientific literature, the 1 bar pressure level is usually chosen as a zero point for altitudes—a "surface" of Jupiter.[2] As with Earth, the top atmospheric layer, the exosphere, does not have a well defined upper boundary.[13] The density gradually decreases until it smoothly transitions into the interplanetary medium approximately 5,000 km above the "surface".[14]

The vertical temperature variations in the Jovian atmosphere are similar to those of the atmosphere of Earth. The temperature of the troposphere decreases with height until it reaches a minimum at the tropopause,[15] which is the boundary between the troposphere and stratosphere. On Jupiter, the tropopause is approximately 50 km above the visible clouds (or 1 bar level), where the pressure and temperature are about 0.1 bar and 110 K.[3][16] In the stratosphere, the temperatures rise to about 200 K at the transition into the thermosphere, at an altitude and pressure of around 320 km and 1 μbar.[3] In the thermosphere, temperatures continue to rise, eventually reaching 1000 K at about 1000 km, where pressure is about 1 nbar.[17]

Jupiter's troposphere contains a complicated cloud structure. The visible clouds, located in the pressure range 0.5–1.0 bar, are made of ammonia ice.[18] Below these ammonia ice clouds, clouds made of ammonium hydrosulfide or ammonium sulfide (between 1.5–3 bar) and water (3–7 bar) are thought to exist.[4][19] There are no methane clouds as the temperatures are too high for it to condense.[4] The water clouds form the densest layer of clouds and have the strongest influence on the dynamics of the atmosphere. This is a result of the higher condensation heat of water and higher water abundance as compared to the ammonia and hydrogen sulfide (oxygen is a more abundant chemical element than either nitrogen or sulfur).[12] Various tropospheric (at 200–400 mbar) and stratospheric (at 10–100 mbar) haze layers reside above the main cloud layers.[20] The latter are made from condensed heavy polycyclic aromatic hydrocarbons or hydrazine, which are generated in the upper stratosphere (1–100 μbar) from methane under the influence of the solar ultraviolet radiation (UV).[21] The methane abundance relative to molecular hydrogen in the stratosphere is about 10−4,[14] while the abundance ratio of other light hydrocarbons, like ethane and acetylene, to molecular hydrogen is about 10−6.[14]

Jupiter's thermosphere is located at pressures lower than 1 μbar and demonstrates such phenomena as airglow, polar aurorae and X-ray emissions.[22] Within it lie layers of increased electron and ion density that form the ionosphere.[14] The high temperatures prevalent in the thermosphere (800–1000 K) have not been fully explained yet;[17] existing models predict a temperature no higher than about 400 K.[14] They may be caused by absorption of high-energy solar radiation (UV or X-ray), by heating from the charged particles precipitating from the Jovian magnetosphere, or by dissipation of upward-propagating gravity waves.[23] The thermosphere and exosphere at the poles and at low latitudes emit X-rays, which were first observed by the Einstein Observatory in 1983.[24] The energetic particles coming from Jupiter's magnetosphere create bright auroral ovals, which encircle the poles. Unlike their terrestrial analogs, which appear only during magnetic storms, aurorae are permanent features of Jupiter's atmosphere.[24] The thermosphere was the first place outside the Earth where the trihydrogen cation (H+3) was discovered.[14] This ion emits strongly in the mid-infrared part of the spectrum, at wavelengths between 3 and 5 μm; this is the main cooling mechanism of the thermosphere.[22]0.19–0.58 (19 bar)
P/H 3.73 × 10−7 0.82
S/H 1.62 × 10−45 2.5 ± 0.15

Elemental abundances relative to hydrogen
in Jupiter and Sun[1]
Element Sun Jupiter/Sun
He/H 0.0975 0.807 ± 0.02
Ne/H 1.23 × 10−4 0.10 ± 0.01
Ar/H 3.62 × 10−6 2.5 ± 0.5
Kr/H 1.61 × 10−9 2.7 ± 0.5
Xe/H 1.68 × 10−10 2.6 ± 0.5
C/H 3.62 × 10−4 2.9 ± 0.5
N/H 1.12 × 10−4 3.6 ± 0.5 (8 bar)

3.2 ± 1.4 (9–12 bar)

O/H 8.51 × 10−4 0.033 ± 0.015 (12 bar)

0.19–0.58 (19 bar)

P/H 3.73 × 10−7 0.82
S/H 1.62 × 10−45 2.5 ± 0.15

The composition of Jupiter's atmosphere is similar to that of the planet as a whole.[1] Jupiter's atmosphere is the most comprehensively understood of those of all the gas giants because it was observed directly by the Galileo atmospheric probe when it entered the Jovian atmosphere on December 7, 1995.[25] Other sources of information about Jupiter's atmospheric composition include the Infrared Space Observatory (ISO),[26] the Galileo and Cassini orbiters,[27] and Earth-based observations.[1]

The two main constituents of the Jovian atmosphere are molecular hydrogen (H2) and helium.[1] The helium abundance is 0.157 ± 0.0036 relative to molecular hydrogen by number of molecules, and its mass fraction is 0.234 ± 0.005, which is slightly lower than the solar system's primordial value.[1] The reason for this low abundance is not entirely understood, but, being denser than hydrogen, some of the helium may have condensed into the core of Jupiter.[18] The atmosphere contains various simple compounds such as water, methane (CH4), hydrogen sulfide (H2S), ammonia (NH3) and phosphine (PH3).[1] Their abundances in the deep (below 10 bar) troposphere imply that the atmosphere of Jupiter is enriched in the elements carbon, nitrogen, sulfur and possibly oxygen[b] by factor of 2–4 relative to the Sun.[c][1] The noble gases argon, krypton and xenon appear to be enriched relative to solar abundances as well (see table), while neon is scarcer.[1] Other chemical compounds such as arsine (AsH3) and germane (GeH4) are present only in trace amounts.[1] The upper atmosphere of Jupiter contains small amounts of simple hydrocarbons such as ethane, acetylene, and diacetylene, which form from methane under the influence of the solar ultraviolet radiation and charged particles coming from Jupiter's magnetosphere.[1] The carbon dioxide, carbon monoxide and water present in the upper atmosphere are thought to originate from impacting comets, such as Shoemaker-Levy 9. The water cannot come from the troposphere because the cold tropopause acts like a cold trap, effectively preventing water from rising to the stratosphere (see Vertical structure above).[1]

Isotopic ratios in Jupiter and Sun[1]
Ratio Sun Jupiter
13C/12C 0.011 0.0108 ± 0.0005
15N/14N <2.8 × 10−3 2.3 ± 0.3 × 10−3

(0.08–2.8 bar)

36Ar/38Ar 5.77 ± 0.08 5.6 ± 0.25
20Ne/22Ne 13.81 ± 0.08 13 ± 2
3He/4He 1.5 ± 0.3 × 10−4 1.66 ± 0.05 × 10−4
D/H 3.0 ± 0.17 × 10−5 2.25 ± 0.35 × 10−5

Earth- and spacecraft-based measurements have led to improved knowledge of the isotopic ratios in Jupiter's atmosphere. As of July 2003, the accepted value for the deuterium abundance is 2.25 ± 0.35 × 10−5,[1] which probably represents the primordial value in the protosolar nebula that gave birth to the Solar System.[26] The ratio of nitrogen isotopes in the Jovian atmosphere, 15N to 14N, is 2.3 × 10−3, a third lower than that in the Earth's atmosphere (3.5 × 10−3).[1] The latter discovery is especially significant since the previous theories of Solar System formation considered the terrestrial value for the ratio of nitrogen isotopes to be primordial.[26]

Zones, belts and jets

The most detailed map of Jupiter ever produced; taken by Cassini

The visible surface of Jupiter is divided in a number of bands parallel to the equator. There are two types of bands: lightly colored zones and relatively dark belts.[5] The wide Equatorial Zone (EZ) extends between latitudes of approximately 7°S to 7°N. Above and below the EZ, the North and South Equatorial belts (NEB and SEB) extend to 18°N and 18°S, respectively. Farther from the equator lie the North and South Tropical zones (NtrZ and STrZ).[5] The alternating pattern of belts and zones continues until the polar regions at approximately 50 degrees latitude, where their visible appearance becomes somewhat muted.[28] The basic belt-zone structure probably extends well towards the poles, reaching at least to 80° North or South.[5]

The difference in the appearance between zones and belts is caused by differences in the opacity of the clouds. Ammonia concentration is higher in zones, which leads to the appearance of denser clouds of ammonia ice at higher altitudes, which in turn leads to their lighter color.[15] On the other hand, in belts clouds are thinner and are located at lower altitudes.[15] The upper troposphere is colder in zones and warmer in belts.[5] The exact nature of chemicals that make Jovian zones and bands so colorful is not known, but they may include complicated compounds of sulfur, phosphorus and carbon.[5]

The Jovian bands are bounded by zonal atmospheric flows (winds), called jets. The westward (retrograde) jets are found at the transition from zones to belts (going away from the equator), whereas eastward (prograde) jets mark the transition from belts to zones.[5] Such flow velocity patterns mean that the zonal winds decrease in belts and increase in zones from the equator to the pole. Therefore wind shear in belts is cyclonic, while in zones it is anticyclonic.[19] The EZ is an exception to this rule, showing a strong eastward (prograde) jet and has a local minimum of the wind speed exactly at the equator. The jet speeds are high on Jupiter, reaching more than 100 m/s.[5] These speeds correspond to ammonia clouds located in the pressure range 0.7–1 bar. The prograde jets are generally more powerful than the retrograde jets.[5] The vertical extent of jets is not known. They decay over two to three scale heights[a] above the clouds, while below the cloud level, winds increase slightly and then remain constant down to at least 22 bar—the maximum operational depth reached by the Galileo probe.[16]
Zonal wind speeds in the atmosphere of Jupiter

The origin of Jupiter's banded structure is not completely clear, though it may be similar to that driving the Earth's Hadley cells. The simplest interpretation is that zones are sites of atmospheric upwelling, whereas belts are manifestations of downwelling.[29] When air enriched in ammonia rises in zones, it expands and cools, forming high and dense clouds. In belts, however, the air descends, warming adiabatically, and white ammonia clouds evaporate, revealing lower, darker clouds. The location and width of bands, speed and location of jets on Jupiter are remarkably stable, having changed only slightly between 1980 and 2000. One example of change is a decrease of the speed of the strongest eastward jet located at the boundary between the North Tropical zone and North Temperate belts at 23°N.[6][29] However bands vary in coloration and intensity over time (see below).

Specific bands

Idealized illustration of Jupiter's cloud bands, labeled with their official abbreviations. Lighter zones are indicated to the right, darker belts to the left. The Great Red Spot and Oval BA are shown in the South Tropical Zone and South Temperate Belt, respectively.

The belts and zones that divide Jupiter's atmosphere each have their own names and unique characteristics. They begin below the North and South Polar Regions, which extend from the poles to roughly 40–48° N/S. These bluish-gray regions are usually featureless.[28]

The North North Temperate Region rarely shows more detail than the polar regions, due to limb darkening, foreshortening, and the general diffuseness of features. That said, the North-North Temperate Belt (NNTB) is the northernmost distinct belt, though it occasionally "disappears". Disturbances tend to be minor and short-lived. The North-North Temperate Zone (NNTZ) is perhaps more prominent, but also generally quiet. Other minor belts and zones in the region are occasionally observed.[30]

The North Temperate Region is part of a latitudinal region easily observable from Earth, and thus has a superb record of observation.[31] It also features the strongest prograde jet stream on the planet—a westerly current that forms the southern boundary of the North Temperate Belt (NTB).[31] The NTB fades roughly once a decade (this was the case during the Voyager encounters), making the North Temperate Zone (NTZ) apparently merge into the North Tropical Zone (NTropZ).[31] Other times, the NTZ is divided by a narrow belt into northern and southern components.[31]

The North Tropical Region is composed of the NTropZ and the North Equatorial Belt (NEB). The NTropZ is generally stable in coloration, changing in tint only in tandem with activity on the NTB's southern jet stream. Like the NTZ, it too is sometimes divided by a narrow band, the NTropB. On rare occasions, the southern NTropZ plays host to "Little Red Spots". As the name suggests, these are northern equivalents of the Great Red Spot. Unlike the GRS, they tend to occur in pairs and are always short-lived, lasting a year on average; one was present during the Pioneer 10 encounter.[32]

The NEB is one of the most active belts on the planet. It is characterized by anticyclonic white ovals and cyclonic "barges" (also known as "brown ovals"), with the former usually forming farther north than the latter; as in the NTropZ, most of these features are relatively short-lived. Like the South Equatorial Belt (SEB), the NEB has sometimes dramatically faded and "revived". The timescale of these changes is about 25 years.[33]
Zones, belts and vortices on Jupiter. The wide equatorial zone is visible in the center surrounded by two dark equatorial belts (SEB and NEB). The large grayish-blue irregular "hot spots" at the northern edge of the white Equatorial Zone change over the course of time as they march eastward across the planet. The Great Red Spot is at the southern margin of the SEB. Strings of small storms rotate around northern-hemisphere ovals. Small, very bright features, possible lightning storms, appear quickly and randomly in turbulent regions. The smallest features visible at the equator are about 600 kilometers across. This 14-frame animation spans 24 Jovian days, or about 10 Earth days. The passage of time is accelerated by a factor of 600,000.

The Equatorial Region (EZ) is one of the more stable regions of the planet, in latitude and in activity. The northern edge of the EZ hosts spectacular plumes that trail southwest from the NEB, which are bounded by dark, warm (in infrared) features known as festoons (hot spots).[34] Though the southern boundary of the EZ is usually quiescent, observations from the late 19th into the early 20th century show that this pattern was then reversed relative to today. The EZ varies considerably in coloration, from pale to an ochre, or even coppery hue; it is occasionally divided by an Equatorial Band (EB).[35] Features in the EZ move roughly 390 km/h relative to the other latitudes.[36][37]

The South Tropical Region includes the South Equatorial Belt (SEB) and the South Tropical Zone. It is by far the most active region the planet, as it is home to its strongest retrograde jet stream. The SEB is usually the broadest, darkest belt on Jupiter; however, it is sometimes split by a zone (the SEBZ), and can fade entirely every 3 to 15 years before reappearing in what is known as an SEB Revival cycle. A period of weeks or months following the belt's disappearance, a white spot forms and erupts dark brownish material which is stretched into a new belt by Jupiter's winds. The belt most recently disappeared in May, 2010.[38] Another characteristic of the SEB is a long train of cyclonic disturbances following the Great Red Spot. Like the NTropZ, the STropZ is one of the most prominent zones on the planet; not only does it contain the GRS, but it is occasionally rent by a South Tropical Disturbance (STropD), a division of the zone that can be very long-lived; the most famous one lasted from 1901 to 1939.[39]

The South Temperate Region, or South Temperate Belt (STB), is yet another dark, prominent belt, more so than the NTB; until March 2000, its most famous features were the long-lived white ovals BC, DE, and FA, which have since merged to form Oval BA ("Red Jr."). The ovals actually were part of South Temperate Zone, but they extended into STB partially blocking it.[5] The STB has occasionally faded, apparently due to complex interactions between the white ovals and the GRS. The appearance of the South Temperate Zone (STZ)—the zone in which the white ovals originated—is highly variable.[40]

There are a number of other features on Jupiter that are either temporary or difficult to observe from Earth. The South South Temperate Region is harder to discern even than the NNTR; its detail is subtle and can only be studied well by large telescopes or spacecraft.[41] Many zones and belts are more transient in nature and are not always visible. These include the Equatorial band (EB),[42] North Equatorial belt zone (NEBZ, a white zone within the belt) and South Equatorial belt zone (SEBZ).[43] Belts are also occasionally split by a sudden disturbance. When a disturbance divides a normally singular belt or zone, an N or an S is added to indicate whether the component is the northern or southern one; e.g., NEB(N) and NEB(S).[44]


Circulation in Jupiter's atmosphere is markedly different from that in the atmosphere of Earth. The interior of Jupiter is fluid and lacks any solid surface. Therefore, convection may occur throughout the planet's outer molecular envelope. As of 2008, a comprehensive theory of the dynamics of the Jovian atmosphere has not been developed. Any such theory needs to explain the following facts: the existence of narrow stable bands and jets that are symmetric relative to Jupiter's equator, the strong prograde jet observed at the equator, the difference between zones and belts, and the origin and persistence of large vortices such as the Great Red Spot.[6]

The theories regarding the dynamics of the Jovian atmosphere can be broadly divided into two classes: shallow and deep. The former hold that the observed circulation is largely confined to a thin outer (weather) layer of the planet, which overlays the stable interior. The latter hypothesis postulates that the observed atmospheric flows are only a surface manifestation of deeply rooted circulation in the outer molecular envelope of Jupiter.[45] As both theories have their own successes and failures, many planetary scientists actually think that the true theory will include elements of both models.[46]

Shallow models

The first attempts to explain Jovian atmospheric dynamics date back to the 1960s.[45][47] They were partly based on terrestrial meteorology, which was well developed at that time. Those shallow models assumed that the jets on Jupiter are driven by small scale turbulence, which is in turn maintained by moist convection in the outer layer of the atmosphere (above the water clouds).[48][49] The moist convection is a phenomenon related to the condensation and evaporation of water and is one of the major drivers of terrestrial weather.[50] The production of the jets in this model is related to a well-known property of two dimensional turbulence—the so-called inverse cascade, in which small turbulent structures (vortices) merge to form larger ones.[48] The finite size of the planet means that the cascade can not produce structures larger than some characteristic scale, which for Jupiter is called the Rhines scale. Its existence is connected to production of Rossby waves. This process works as follows: when the largest turbulent structures reach a certain size, the energy begins to flow into Rossby waves instead of larger structures, and the inverse cascade stops.[51] Since on the spherical rapidly rotating planet the dispersion relation of the Rossby waves is anisotropic, the Rhines scale in the direction parallel to the equator is larger than in the direction orthogonal to it.[51] The ultimate result of the process described above is production of large scale elongated structures, which are parallel to the equator. The meridional extent of them appears to match the actual width of jets.[48] Therefore in shallow models vortices actually feed the jets and should disappear by merging into them.

While these weather–layer models can successfully explain the existence of a dozen narrow jets, they have serious problems.[48] A glaring failure of the model is the prograde (super-rotating) equatorial jet: with some rare exceptions shallow models produce a strong retrograde (subrotating) jet, contrary to observations. In addition, the jets tend to be unstable and can disappear over time.[48] Shallow models cannot explain how the observed atmospheric flows on Jupiter violate stability criteria.[52] More elaborated multilayer versions of weather–layer models produce more stable circulation, but many problems persist.[53] Meanwhile, the Galileo probe found that the winds on Jupiter extend well below the water clouds at 5–7 bar and do not show any evidence of decay down to 22 bar pressure level, which implies that circulation in the Jovian atmosphere may in fact be deep.[16]

Deep models

The deep model was first proposed by Busse in 1976.[54][55] His model was based on another well-known feature of fluid mechanics, the Taylor-Proudman theorem. It holds that in any fast-rotating barotropic ideal liquid, the flows are organized in a series of cylinders parallel to the rotational axis. The conditions of the theorem are probably met in the fluid Jovian interior. Therefore the planet's molecular hydrogen mantle may be divided into a number of cylinders, each cylinder having a circulation independent of the others.[56] Those latitudes where the cylinders' outer and inner boundaries intersect with the visible surface of the planet correspond to the jets; the cylinders themselves are observed as zones and belts.
Thermal image of Jupiter obtained by NASA Infrared Telescope Facility

The deep model easily explains the strong prograde jet observed at the equator of Jupiter; the jets it produces are stable and do not obey the 2D stability criterion.[56] However it has major difficulties; it produces a very small number of broad jets, and realistic simulations of 3D flows are not possible as of 2008, meaning that the simplified models used to justify deep circulation may fail to catch important aspects of the fluid dynamics within Jupiter.[56] One model published in 2004 successfully reproduced the Jovian band-jet structure.[46] It assumed that the molecular hydrogen mantle is thinner than in all other models; occupying only the outer 10% of Jupiter's radius. In standard models of the Jovian interior, the mantle comprises the outer 20–30%.[57] The driving of deep circulation is another problem. In fact, the deep flows can be caused both by shallow forces (moist convection, for instance) or by deep planet-wide convection that transports heat out of the Jovian interior.[48] Which of these mechanisms is more important is not clear yet.

Internal heat

As has been known since 1966,[58] Jupiter radiates much more heat than it receives from the Sun. It is estimated that the ratio between the power emitted by the planet and that absorbed from the Sun is 1.67 ± 0.09. The internal heat flux from Jupiter is 5.44 ± 0.43 W/m2, whereas the total emitted power is 335 ± 26 petawatts. The latter value is approximately equal to one billionth of the total power radiated by the Sun. This excess heat is mainly the primordial heat from the early phases of Jupiter's formation, but may result in part from the precipitation of helium into the core.[59]

The internal heat may be important for the dynamics of the Jovian atmosphere. While Jupiter has a small obliquity of about 3°, and its poles receive much less solar radiation than its equator, the tropospheric temperatures do not change appreciably from the equator to poles. One explanation is that Jupiter's convective interior acts like a thermostat, releasing more heat near the poles than in the equatorial region. This leads to a uniform temperature in the troposphere. While heat is transported from the equator to the poles mainly via the atmosphere on Earth, on Jupiter deep convection equilibrates heat. The convection in the Jovian interior is thought to be driven mainly by the internal heat.[60]

Discrete features


The atmosphere of Jupiter is home to hundreds of vortices—circular rotating structures that, as in the Earth’s atmosphere, can be divided into two classes: cyclones and anticyclones.[7] The former rotate in the direction similar to the rotation of the planet (counterclockwise in the northern hemisphere and clockwise in the southern); the latter rotate in the reverse direction. However a major difference from the terrestrial atmosphere is that, in the Jovian atmosphere, anticyclones dominate over cyclones, as more than 90% of vortices larger than 2000 km in diameter are anticyclones.[61] The lifetime of vortices varies from several days to hundreds of years depending on their size. For instance, the average lifetime of anticyclones with diameters from 1000 to 6000 km is 1–3 years.[62] Vortices have never been observed in the equatorial region of Jupiter (within 10° of latitude), where they are unstable.[10] As on any rapidly rotating planet, Jupiter's anticyclones are high pressure centers, while cyclones are low pressure.[34]
New Horizons IR view of Jupiter's atmosphere

The anticyclones in Jupiter's atmosphere are always confined within zones, where the wind speed increases in direction from the equator to the poles.[62] They are usually bright and appear as white ovals.[7] They can move in longitude, but stay at approximately the same latitude as they are unable to escape from the confining zone.[10] The wind speeds at their periphery are about 100 m/s.[9] Different anticyclones located in one zone tend to merge, when they approach each other.[63] However Jupiter has two anticyclones that are somewhat different from all others. They are the Great Red Spot (GRS)[8] and the Oval BA;[9] the latter formed only in 2000. In contrast to white ovals, these structures are red, arguably due to dredging up of red material from the planet's depths.[8] On Jupiter the anticyclones usually form through merges of smaller structures including convective storms (see below),[62] although large ovals can result from the instability of jets. The latter was observed in 1938–1940, when a few white ovals appeared as a result of instability of the southern temperate zone; they later merged to form Oval BA.[9][62]

In contrast to anticyclones, the Jovian cyclones tend to be small, dark and irregular structures. Some of the darker and more regular features are known as brown ovals (or badges).[61] However the existence of a few long–lived large cyclones has been suggested. In addition to compact cyclones, Jupiter has several large irregular filamentary patches, which demonstrate cyclonic rotation.[7] One of them is located to the west of the GRS (in its wake region) in the southern equatorial belt.[64] These patches are called cyclonic regions (CR). The cyclones are always located in the belts and tend to merge when they encounter each other, much like anticyclones.[62]

The deep structure of vortices is not completely clear. They are thought to be relatively thin, as any thickness greater than about 500 km will lead to instability. The large anticyclones are known to extend only a few tens of kilometers above the visible clouds. The early hypothesis that the vortices are deep convective plumes (or convective columns) as of 2008 is not shared by the majority of planetary scientists.[10]

Great Red Spot

The Great Red Spot (GRS) is a persistent anticyclonic storm, 22° south of Jupiter's equator, which has lasted for at least 180 years and possibly as long as 345 years or more.[65][66] The storm is large enough to be visible through Earth-based telescopes.
An infrared image of GRS (top) showing its warm center, taken by the ground based Very Large Telescope. An image made by the Hubble Space Telescope (bottom) is shown for comparison.

The GRS rotates counterclockwise, with a period of about six Earth days[67] or 14 Jovian days. Its dimensions are 24–40,000 km west–to–east and 12–14,000 km south–to–north. The spot is large enough to contain two or three planets the size of Earth. At the start of 2004, the Great Red Spot had approximately half the longitudinal extent it had a century ago, when it was 40,000 km in diameter. At the present rate of reduction it could potentially become circular by 2040, although this is unlikely because of the distortion effect of the neighboring jet streams.[68] It is not known how long the spot will last, or whether the change is a result of normal fluctuations.[69]

According to a study by scientists at the University of California, Berkeley, between 1996 and 2006 the spot lost 15 percent of its diameter along its major axis. Xylar Asay-Davis, who was on the team that conducted the study, noted that the spot is not in danger of disappearing because "[v]elocity is a more robust measurement because the clouds associated with the Red Spot are also strongly influenced by numerous other phenomena in the surrounding atmosphere."[70]

Infrared data have long indicated that the Great Red Spot is colder (and thus, higher in altitude) than most of the other clouds on the planet;[71] the cloudtops of the GRS are about 8 km above the surrounding clouds. Furthermore, careful tracking of atmospheric features revealed the spot's counterclockwise circulation as far back as 1966—observations dramatically confirmed by the first time-lapse movies from the Voyager flybys.[72] The spot is spatially confined by a modest eastward jet stream (prograde) to its south and a very strong westward (retrograde) one to its north.[73] Though winds around the edge of the spot peak at about 120 m/s (432 km/h), currents inside it seem stagnant, with little inflow or outflow.[74] The rotation period of the spot has decreased with time, perhaps as a direct result of its steady reduction in size.[75] In 2010, astronomers imaged the GRS in the far infrared (from 8.5 to 24 μm) with a spatial resolution higher than ever before and found that its central, reddest region is warmer than its surroundings by between 3–4 K. The warm airmass is located in the upper troposphere in the pressure range of 200–500 mbar. This warm central spot slowly counter-rotates and may be caused by a weak subsidence of air in the center of GRS.[76]
Approximate size comparison of Earth and the GRS

The Great Red Spot's latitude has been stable for the duration of good observational records, typically varying by about a degree. Its longitude, however, is subject to constant variation.[77][78] Because Jupiter does not rotate uniformly at all latitudes, astronomers have defined three different systems for defining the longitude. System II is used for latitudes of more than 10°, and was originally based on the average rotation rate of the Great Red Spot of 9h 55m 42s.[79][80] Despite this, the spot has "lapped" the planet in System II at least 10 times since the early nineteenth century. Its drift rate has changed dramatically over the years and has been linked to the brightness of the South Equatorial Belt, and the presence or absence of a South Tropical Disturbance.[81]

It is not known exactly what causes the Great Red Spot's reddish color. Theories supported by laboratory experiments suppose that the color may be caused by complex organic molecules, red phosphorus, or yet another sulfur compound. The GRS varies greatly in hue, from almost brick-red to pale salmon, or even white. The reddest central region is slightly warmer than the surroundings, which is the first evidence that the Spot's color is affected by environmental factors.[76] The spot occasionally disappears from the visible spectrum, becoming evident only through the Red Spot Hollow, which is its niche in the South Equatorial Belt. The visibility of GRS is apparently coupled to the appearance of the SEB; when the belt is bright white, the spot tends to be dark, and when it is dark, the spot is usually light. The periods when the spot is dark or light occur at irregular intervals; as of 1997, during the preceding 50 years, the spot was darkest in the periods 1961–66, 1968–75, 1989–90, and 1992–93.[82]

The Great Red Spot should not be confused with the Great Dark Spot, a feature observed near the northern pole of Jupiter in 2000 by the Cassini–Huygens spacecraft.[83] Note that a feature in the atmosphere of Neptune was also called the Great Dark Spot. The latter feature was imaged by Voyager 2 in 1989, and may have been an atmospheric hole rather than a storm and it was no longer present in 1994 (although a similar spot had appeared farther to the north).[84]

Oval BA
Oval BA (left)

Oval BA is the official name for a red storm in Jupiter's southern hemisphere similar in form to, though smaller than, the Great Red Spot. Accordingly, it is often affectionately referred to as "Red Spot Jr.", "Red Jr." or "The Little Red Spot". A feature in the South Temperate Belt, Oval BA was first seen in 2000 after the collision of three small white storms, and has intensified since then.[85]

The formation of the three white oval storms that later merged into Oval BA can be traced to 1939, when the South Temperate Zone was rent by dark features that effectively split the zone into three long sections. Jovian observer Elmer J. Reese labeled the dark sections AB, CD, and EF. The rifts expanded, shrinking the remaining segments of the STZ into the white ovals FA, BC, and DE.[86] Ovals BC and DE merged in 1998, forming Oval BE. Then, in March 2000, BE and FA joined together, forming Oval BA.[85] (see White ovals, below)
Formation of Oval BA from three white ovals
Oval BA (bottom), Great Red Spot (top) and "Baby Red Spot" (middle) during a brief encounter in June, 2008

Oval BA slowly began to turn red in August 2005.[87] On February 24, 2006, Filipino amateur astronomer Christopher Go discovered the color change, noting that it had reached the same shade as the GRS.[87] As a result, NASA writer Dr. Tony Phillips suggested it be called "Red Spot Jr." or "Red Jr."[88]

In April 2006, a team of astronomers, believing that Oval BA might converge with the GRS that year, observed the storms through the Hubble Space Telescope.[89] The storms pass each other about every two years, but the passings of 2002 and 2004 did not produce anything exciting. Dr. Amy Simon-Miller, of the Goddard Space Flight Center, predicted the storms would have their closest passing on July 4, 2006.[89] On July 20, the two storms were photographed passing each other by the Gemini Observatory without converging.[90]

Why Oval BA turned red is not understood. According to a 2008 study by Dr. Santiago Pérez-Hoyos of the University of the Basque Country, the most likely mechanism is "an upward and inward diffusion of either a colored compound or a coating vapor that may interact later with high energy solar photons at the upper levels of Oval BA."[91] Some believe that small storms (and their corresponding white spots) on Jupiter turn red when the winds become powerful enough to draw certain gases from deeper within the atmosphere which change color when those gases are exposed to sunlight.[92]

Oval BA is getting stronger according to observations made with the Hubble Space Telescope in 2007. The wind speeds have reached 618 km/h; about the same as in the Great Red Spot and far stronger than any of the progenitor storms.[93][94] As of July 2008, its size is about the diameter of Earth—approximately half the size of the Great Red Spot.[91]

Oval BA should not be confused with another major storm on Jupiter, the South Tropical Little Red Spot (LRS) (nicknamed "the Baby Red Spot" by NASA[95]), which was destroyed by the GRS.[92] The new storm, previously a white spot in Hubble images, turned red in May 2008. The observations were led by Imke de Pater of the University of California, at Berkeley, US.[96] The Baby Red Spot encountered the GRS in late June to early July 2008, and in the course of a collision, the smaller red spot was shredded into pieces. The remnants of the Baby Red Spot first orbited, then were later consumed by the GRS. The last of the remnants with a reddish color to have been identified by astronomers had disappeared by mid-July, and the remaining pieces again collided with the GRS, then finally merged with the bigger storm. The remaining pieces of the Baby Red Spot had completely disappeared by August, 2008.[95] During this encounter Oval BA was present nearby, but played no apparent role in destruction of the Baby Red Spot.[95]

Storms and lightning
Lightning on Jupiter's night side, imaged by the Galileo orbiter in 1997

The storms on Jupiter are similar to thunderstorms on Earth. They reveal themselves via bright clumpy clouds about 1000 km in size, which appear from time to time in the belts' cyclonic regions, especially within the strong westward (retrograde) jets.[11] In contrast to vortices, storms are short-lived phenomena; the strongest of them may exist for several months, while the average lifetime is only 3–4 days.[11] They are believed to be due mainly to moist convection within Jupiter's troposphere. Storms are actually tall convective columns (plumes), which bring the wet air from the depths to the upper part of the troposphere, where it condenses in clouds. A typical vertical extent of Jovian storms is about 100 km; as they extend from a pressure level of about 5–7 bar, where the base of a hypothetical water cloud layer is located, to as high as 0.2–0.5 bar.[97]

Storms on Jupiter are always associated with lightning. The imaging of the night–side hemisphere of Jupiter by Galileo and Cassini spacecrafts revealed regular light flashes particularly at 51°N, 56°S and 23°N latitudes; higher latitude flashes concentrated near the locations of the westward jets.[98] The lightning strikes on Jupiter are on average more powerful than those on Earth. However, they are less frequent; the light power emitted from a given area is similar to that on Earth.[98] A few flashes have been detected in polar regions, making Jupiter the second planet after Earth to exhibit polar lightning.[99]

Every 15–17 years Jupiter is rattled by especially powerful storms. They appear at 23°N latitude, where the strongest eastward jet is located. The last such an event was observed in March–June 2007.[97] Two storms appeared in the northern temperate belt 55° apart in longitude. They significantly disturbed the belt. The dark material that was shed by the storms mixed with clouds and changed the belt’s color. The storms moved with a speed as high as 170 m/s, slightly faster than the jet itself, hinting at the existence of strong winds deep in the atmosphere.[97]
False color image of an equatorial hot spot


The normal pattern of bands and zones is sometimes disrupted for periods of time. One particular class of disruption are long-lived darkenings of the South Tropical Zone, normally referred to as "South Tropical Disturbances" (STD). The longest lived STD in recorded history was followed from 1901 until 1939, having been first seen by Percy B. Molesworth on February 28, 1901. It took the form of darkening over part of the normally bright South Tropical zone. Several similar disturbances in the South Tropical Zone have been recorded since then.[100]

Hot spots

One of the most mysterious features in the atmosphere of Jupiter are hot spots. In them the air is relatively free of clouds and the heat can escape from the depth without much absorption. The spots look like bright spots in the infrared images obtained at the wavelength of about 5 μm.[34] They are preferentially located in the belts, although there is a train of prominent hot spots at the northern edge of the Equatorial Zone. Galileo probe descended into one of those equatorial spots. Each equatorial spot is associated with a bright cloudy plume located to the west of it and reaching up to 10,000 km in size.[5] Hot spots generally have round shape, although they do not resemble vortexes.[34]

The origin of hot spots is not clear. They can be either downdrafts, where the descending air is adiabatically heated and dried or, alternatively, they can be a manifestation of a planetary scale waves. The latter hypotheses explains the periodical pattern of the equatorial spots.[34][5]

Observational history
Main article: Exploration of Jupiter
Time-lapse sequence from the approach of Voyager 1 to Jupiter

Early astronomers, using small telescopes with their eyes as detectors, recorded the changing appearance of Jupiter’s atmosphere.[20] Their descriptive terms—belts and zones, brown spots and red spots, plumes, barges, festoons, and streamers—are still used.[20] Other terms such as vorticity, vertical motion, cloud heights have entered in use later, in the 20th century.[20]

The first observations of the Jovian atmosphere at higher resolution than possible with Earth-based telescopes were taken by the Pioneer 10 and 11 spacecraft. The first truly detailed images of Jupiter's atmosphere were provided by the Voyagers.[20] The two spacecraft were able to image details at a resolution as low as 5 km in size in various spectra, and also able to create "approach movies" of the atmosphere in motion.[20] The Galileo probe saw less of Jupiter's atmosphere, but at a better average resolution and a wider spectral bandwidth.[20]

Today, astronomers have access to a continuous record of Jupiter's atmospheric activity thanks to telescopes such as Hubble. These show that the atmosphere is occasionally wracked by massive disturbances, but that, overall, it is remarkably stable.[20] The vertical motion of Jupiter's atmosphere was largely determined by the identification of trace gases by ground-based telescopes.[20] Spectroscopic studies after the collision of comet Shoemaker-Levy 9 gave a glimpse of the Jupiter's composition beneath the cloud tops. The presence of diatomic sulfur (S2) and carbon disulfide (CS2) was recorded—the first detection of either in Jupiter, and only the second detection of S2 in any astronomical object— together with other molecules such as ammonia (NH3) and hydrogen sulfide (H2S), while oxygen-bearing molecules such as sulfur dioxide were not detected, to the surprise of astronomers.[101]

The Galileo atmospheric probe, as it plunged into Jupiter, measured the wind, temperature, composition, clouds, and radiation levels down to 22 bar. However, below 1 bar there is uncertainty in the results.[20]

Great Red Spot studies
A wider view of Jupiter and the Great Red Spot as seen from Voyager 1 in 1979

The first sighting of the GRS is often credited to Robert Hooke, who described a spot on the planet in May 1664; however, it is likely that Hooke's spot was in the wrong belt altogether (the North Equatorial Belt, versus the current location in the South Equatorial Belt). Much more convincing is Giovanni Cassini's description of a "permanent spot" in the following year.[102] With fluctuations in visibility, Cassini's spot was observed from 1665 to 1713.[95]

A minor mystery concerns a Jovian spot depicted around 1700 on a canvas by Donato Creti, which is exhibited in the Vatican.[103][104] It is a part of a series of panels in which different (magnified) heavenly bodies serve as backdrops for various Italian scenes, the creation of all of them overseen by the astronomer Eustachio Manfredi for accuracy. Creti's painting is the first known to depict the GRS as red. No Jovian feature was officially described as red before the late 1800s.[104]

The present GRS was first seen only after 1830 and well-studied only after a prominent apparition in 1879. A long 118-year gap separates the observations made after 1830 from its seventeenth-century discovery; whether the original spot dissipated and re-formed, whether it faded, or even if the observational record was simply poor are unknown.[82] The older spots had a short observational history and slower motion than that of the modern spot, which make their identity unlikely.[103]

On February 25, 1979, when the Voyager 1 spacecraft was 9.2 million kilometers from Jupiter it transmitted the first detailed image of the Great Red Spot back to Earth. Cloud details as small as 160 km across were visible. The colorful, wavy cloud pattern seen to the west (left) of the GRS is the spot's wake region, where extraordinarily complex and variable cloud motions are observed.[105]

White ovals
The white ovals that later formed Oval BA, imaged by the Galileo orbiter in 1997

The white ovals that were to become Oval BA formed in 1939. They covered almost 90 degrees of longitude shortly after their formation, but contracted rapidly during their first decade; their length stabilized at 10 degrees or less after 1965.[106] Although they originated as segments of the STZ, they evolved to become completely embedded in the South Temperate Belt, suggesting that they moved north, "digging" a niche into the STB.[107] Indeed, much like the GRS, their circulations were confined by two opposing jet streams on their northern and southern boundaries, with an eastward jet to their north and a retrograde westward one to the south.[106]

The longitudinal movement of the ovals seemed to be influenced by two factors: Jupiter's position in its orbit (they became faster at aphelion), and their proximity to the GRS (they accelerated when within 50 degrees of the Spot).[108] The overall trend of the white oval drift rate was deceleration, with a decrease by half between 1940 and 1990.[109]

During the Voyager fly-bys, the ovals extended roughly 9000 km from east to west, 5000 km from north to south, and rotated every five days (compared to six for the GRS at the time).[110]

See also

* Extrasolar planet (Many are larger than Jupiter.)
* Galileo atmospheric probe
* Juno probe


1. ^ The scale height sh is defined as sh = RT/(Mgj), where R = 8.31 J/mol/K is the gas constant, M ≈ 0.0023 kg/mol is the average molar mass in the Jovian atmosphere,[3] T is temperature and gj ≈ 25 m/s2 is the gravitational acceleration at the surface of Jupiter. As the temperature varies from 110 K in the tropopause up to 1000 K in the thermosphere,[3] the scale height can assume values from 15 to 150 km.
2. ^ The Galileo atmospheric probe failed to measure the deep abundance of oxygen, because the water concentration continued to increase down to the pressure level of 22 bar, when it ceased operating. While the actually measured oxygen abundances are much lower than the solar value, the observed rapid increase of water content of the atmosphere with depth makes it highly likely that the deep abundance of oxygen indeed exceeds the solar value by a factor of about 3—much like other elements.[1]
3. ^ Various explanations of the overabundance of carbon, oxygen, nitrogen and other elements have been proposed. The leading one is that Jupiter captured a large number of icy planetesimals during the later stages of its accretion. The volatiles like noble gases are thought to have been trapped as clathrate hydrates in water ice.[1]


1. ^ a b c d e f g h i j k l m n o p q Atreya et al. (2003)
2. ^ a b c d Guillot (1999)
3. ^ a b c d e f g Sieff et al. (1998)
4. ^ a b c Atreya et al. (2005)
5. ^ a b c d e f g h i j k l m Ingersoll (2004), pp. 2–5
6. ^ a b c Vasavada (2005), p. 1942
7. ^ a b c d Vasavada (2005), p. 1974
8. ^ a b c Vasavada (2005), pp. 1978–1980
9. ^ a b c d Vasavada (2005), pp. 1980–1982
10. ^ a b c d Vasavada (2005), p. 1976
11. ^ a b c Vasavada (2005), pp. 1982, 1985–1987
12. ^ a b Ingersoll (2004), pp. 13–14
13. ^ Yelle (2004), p. 1
14. ^ a b c d e f Miller et al. (2005)
15. ^ a b c Ingersoll (2004), pp. 5–7
16. ^ a b c Ingersoll (2004), p. 12
17. ^ a b Yelle (2004), pp. 15–16
18. ^ a b Atreya et al. (1999)
19. ^ a b Vasavada (2005), p. 1937
20. ^ a b c d e f g h i j Ingersoll (2004), p. 8
21. ^ Atreya et al. (2005)
22. ^ a b Yelle (2004), pp. 1–12
23. ^ Yelle (2004), pp. 22–27
24. ^ a b Bhardwaj and Gladstone (2000), pp. 299–302
25. ^ McDowell, Jonathan (1995-12-08). "Jonathan's Space Report, No. 267". Harvard-Smithsonian Center for Astrophysics. Retrieved 2007-05-06.
26. ^ a b c Encrenaz (2003)
27. ^ Kunde et al. (2004)
28. ^ a b Rogers (1995), p. 81.
29. ^ a b Ingersoll (2004), p. 5
30. ^ Rogers (1995), pp. 85, 91–4.
31. ^ a b c d Rogers (1995), pp. 101–105.
32. ^ Rogers (1995), pp.113–117.
33. ^ Rogers (1995), pp. 125–130.
34. ^ a b c d e Vasavada (2005), pp. 1987–1989
35. ^ Rogers (1995), pp. 133, 145–147.
36. ^ Rogers (1995), p. 133.
37. ^ Beebe (1997), p. 24.
38. ^ Nancy Atkinson (2010). "Jupiter, It Is A-Changing". Universe Today. Retrieved 2010-05-14.
39. ^ Rogers (1995), pp. 159–160
40. ^ Rogers (1995), pp. 219–221, 223, 228–229.
41. ^ Rogers (1995), p. 235.
42. ^ Rogers et al. (2003)
43. ^ Rogers and Metig (2001)
44. ^ Ridpath (1998)
45. ^ a b Vasavada (2005), pp. 1943–1945
46. ^ a b Hiempel et al. (2005)
47. ^ See, e. g., Ingersoll et al. (1969)
48. ^ a b c d e f Vasavada (2005), pp. 1947–1958
49. ^ Ingersoll (2004), pp. 16–17
50. ^ Ingersoll (2004), pp. 14–15
51. ^ a b Vasavada (2005), p. 1949
52. ^ Vasavada (2005), pp. 1945–1947
53. ^ Vasavada (2005), pp. 1962–1966
54. ^ Vasavada (2005), p. 1966
55. ^ Busse (1976)
56. ^ a b c Vasavada (2005), pp. 1966–1972
57. ^ Vasavada (2005), p. 1970
58. ^ Low (1966)
59. ^ Pearl, 1990, pp. 12, 26.
60. ^ Ingersoll (2004), pp. 11, 17–18
61. ^ a b Vasavada (2005), p. 1978
62. ^ a b c d e Vasavada (2005), p. 1977
63. ^ Vasavada (2005), p. 1975
64. ^ Vasavada (2005), p. 1979
65. ^ Staff (2007). "Jupiter Data Sheet –". Imaginova. Retrieved 2008-06-03.
66. ^ Anonymous (August 10, 2000). "The Solar System - The Planet Jupiter – The Great Red Spot". Dept. Physics & Astronomy – University of Tennessee. Retrieved 2008-06-03.
67. ^ Smith et al. (1979), p. 954.
68. ^ Irwin, 2003, p. 171
69. ^ Beatty (2002)
70. ^ Britt, Robert Roy (2009-03-09). "Jupiter's Great Red Spot Is Shrinking". Retrieved 2009-02-04.
71. ^ Rogers (1995), p. 191.
72. ^ Rogers (1995), pp. 194–196.
73. ^ Beebe (1997), p. 35.
74. ^ Rogers (1995), p. 195.
75. ^ Rogers, John (July 30, 2006). "Interim reports on STB (Oval BA passing GRS), STropB, GRS (internal rotation measured), EZ(S. Eq. Disturbance; dramatic darkening; NEB interactions), & NNTB". British Astronomical Association. Retrieved 2007-06-15.
76. ^ a b Fletcher, Leigh N.; Orton,, G.S.; Mousis et. al, O. (2010). "Thermal structure and composition of Jupiter’s Great Red Spot from high-resolution thermal imaging" (pdf). Icarus 208: 306–328. doi:10.1016/j.icarus.2010.01.005.
77. ^ Reese and Gordon (1966)
78. ^ Rogers (1995), 192–193.
79. ^ Stone (1974)
80. ^ Rogers (1995), pp. 48, 193.
81. ^ Rogers (1995), p. 193.
82. ^ a b Beebe (1997), pp. 38–41.
83. ^ Phillips, Tony (March 12, 2003). "The Great Dark Spot". Science at NASA. Retrieved 2007-06-20.
84. ^ Hammel et al. (1995)
85. ^ a b Sanchez-Lavega et al. (2001)
86. ^ Rogers (1995), p. 223.
87. ^ a b Go et al. (2006)
88. ^ Phillips, Tony (March 3, 2006). "Jupiter's New Red Spot". NASA. Retrieved 2008-10-16.
89. ^ a b Phillips, Tony (June 5, 2006). "Huge Storms Converge". Science@NASA. Retrieved 2007-01-08.
90. ^ Michaud, Peter (July 20, 2006). "Gemini Captures Close Encounter of Jupiter's Red Spots". Gemini Observatory. Retrieved 2007-06-15.
91. ^ a b "Diffusion Caused Jupiter's Red Spot Junior To Color Up". ScienceDaily. September 26, 2008. Retrieved 2008-10-16.
92. ^ a b Fountain, Henry (July 22, 2008). "On Jupiter, a Battle of the Red Spots, With the Baby Losing". The New York Times. Retrieved 2010-06-18.
93. ^ Buckley, M. (May 20, 2008). "Storm Winds Blow in Jupiter’s Little Red Spot". Johns Hopkins Applied Physics Laboratory. Retrieved 2008-10-16.
94. ^ Steigerwald , Bill (October 10, 2006). "Jupiter's Little Red Spot Growing Stronger". NASA Goddard Space Center. Retrieved 2008-10-16.
95. ^ a b c d Rogers, John H. (August 8, 2008). "The collision of the Little Red Spot and Great Red Spot: Part 2". British Astronomical Association. Retrieved 2008-11-29.
96. ^ Shiga, David (May 22, 2008). "Third red spot erupts on Jupiter". New Scientist. Retrieved 2008-05-23.
97. ^ a b c Sanchez-Lavega et al. (2008)
98. ^ a b Vasavada (2005), pp. 1983–1985
99. ^ Baines et al. (2007)
100. ^ McKim (1997)
101. ^ Noll, K.S.; McGrath, M.A.; Weaver, H.A.; Yelle, R.V.; Trafton, L.M.; Atreya, S.K.; Caldwell, J.J.; Barnet, C.; Edgington, S. (March 1995). "HST Spectroscopic Observations of Jupiter Following the Impact of Comet Shoemaker-Levy 9". Science 267 (5202): 1307–1313. doi:10.1126/science.7871428. PMID 7871428. Retrieved 2008-08-24.
102. ^ Rogers (1995), p. 6.
103. ^ a b Rogers (1995), p. 188
104. ^ a b Hockey, 1999, pp. 40–41.
105. ^ Smith et al. (1979), pp. 951–972.
106. ^ a b Rogers (1995), pp. 224–5.
107. ^ Rogers (1995), p. 226–227.
108. ^ Rogers (1995), p. 226.
109. ^ Rogers (1995), p. 225.
110. ^ Beebe (1997), p. 43.

Cited sources

* Atreya, S.K.; Wong, M.H.; Owen, T.C. et al. (1999). "A comparison of the atmospheres of Jupiter and Saturn: deep atmospheric composition, cloud structure, vertical mixing, and origin". Planetary and Space Science 47: 1243–1262. doi:10.1016/S0032-0633(99)00047-1. Bibcode: 1999P%26SS...47.1243A.
* Atreya, S.K.; Mahaffy, P.R.; Niemann, H.B. et al. (2003). "Composition and origin of the atmosphere of Jupiter—an update, and implications for the extrasolar giant planets". Planetary and Space Science 51: 105–112. doi:10.1016/S0032-0633(02)00144-7. Bibcode: 2003P%26SS...51..105A.
* Atreya, S.K.; Wong, A.S. (2005). "Coupled Clouds and Chemistry of the Giant Planets – a Case for Multiprobes". Space Science Reviews 116: 121–136. doi:10.1007/s11214-005-1951-5.
* Atreya, S.K.; Wong, A.S.; Baines, K.H. et al. (2005). "Jupiter’s ammonia clouds—localized or ubiquitous?". Planetary and Space Science 53: 498–507. doi:10.1016/j.pss.2004.04.002.
* Baines, K.H; Simon-Miller, A.A.; Orton, G.S. et al. (2007). "Polar Lightning and Decadal-Scale Cloud Variability on Jupiter". Science 318 (5848): 226–229. doi:10.1126/science.1147912. PMID 17932285. Bibcode: 2007Sci...318..226B.
* Beatty, J.K. (2002). "Jupiter's Shrinking Red Spot". Sky and Telescope 103 (4): 24.
* Beebe, R. (1997). Jupiter the Giant Planet (2nd ed.). Washington: Smithsonian Books. ISBN 1560986859. OCLC 224014042.
* Bhardwaj, A.; Gladstone, G.R. (2000). "Auroral emissions of the giant planets". Reviews of Geophysics 38 (3): 295–353. doi:10.1029/1998RG000046.
* Busse, F.H. (1976). "A simple model of convection in the Jovian atmosphere". Icarus 29: 255–260. doi:10.1016/0019-1035(76)90053-1. Bibcode: 1976Icar...29..255B.
* Encrenaz, T. (2003). "ISO observations of the giant planets and Titan: what have we learnt?". Planetary and Space Science 51: 89–103. doi:10.1016/S0032-0633(02)00145-9. Bibcode: 2003P%26SS...51...89E.
* Go, C.Y.; de Pater, I.; Wong M. et al. (2006). "Evolution Of The Oval Ba During 2004–2005". Bulletin of the American Astronomical Society 38: 495. Bibcode: 2006DPS....38.1102G.
* Guillot, T. (1999). "A comparison of the interiors of Jupiter and Saturn". Planetary and Space Science 47: 1183–1200. doi:10.1016/S0032-0633(99)00043-4. Bibcode: 1999P%26SS...47.1183G.
* Hammel, H.B.; Lockwood, G.W.; Mills, J.R.; Barnet, C.D. (1995). "Hubble Space Telescope Imaging of Neptune's Cloud Structure in 1994". Science 268 (5218): 1740–1742. doi:10.1126/science.268.5218.1740. PMID 17834994. Bibcode: 1995Sci...268.1740H.
* Heimpel, M.; Aurnou, J.; Wicht, J. (2005). "Simulation of equatorial and high-latitude jets on Jupiter in a deep convection model" (pdf). Nature 438 (7065): 193–196. doi:10.1038/nature04208. PMID 16281029.
* Hockey, T. (1999). Galileo's Planet: Observing Jupiter Before Photography. Bristol, Philadelphia: Institute of Physics Publishing. ISBN 0750304480. OCLC 39733730.
* Ingersoll, A.P.; Dowling, T.E.; Gierasch, P.J. et al (2004). "Dynamics of Jupiter’s Atmosphere". in Bagenal, F.; Dowling, T.E.; McKinnon, W.B.. Jupiter: The Planet, Satellites and Magnetosphere. Cambridge: Cambridge University Press.
* Ingersoll, A.P.; Cuzzi, J.N. (1969). "Dynamics of Jupiter's cloud bands". Journal of the Atmospheric Sciences 26: 981–985. doi:10.1175/1520-0469(1969)026<0981:DOJCB>2.0.CO;2. Bibcode: 1969JAtS...26..981I.
* Irwin, P. (2003). Giant Planets of Our Solar System. Atmospheres, Composition, and Structure. Springer and Praxis. ISBN 9783540006817.
* Kunde, V.G.; Flasar, F.M.; Jennings, D.E. et al. (2004). "Jupiter’s Atmospheric Composition from the Cassini Thermal Infrared Spectroscopy Experiment". Science 305 (5690): 1582–1586. doi:10.1126/science.1100240. PMID 15319491. Bibcode: 2004Sci...305.1582K.
* Low, F.J. (1966). "Observations of Venus, Jupiter, and Saturn at λ20 μ". Astronomical Journal 71: 391. doi:10.1086/110110. Bibcode: 1966AJ.....71R.391L.
* McKim, R.J. (1997). "P. B. Molesworth's discovery of the great South Tropical Disturbance on Jupiter, 1901". Journal of the British Astronomical Association 107 (5): 239–245. Bibcode: 1997JBAA..107..239M.
* Miller, S.; Aylword, A.; Milliword, G. (2005). "Giant Planet Ionospheres and Thermospheres: the Importance of Ion-Neutral Coupling". Space Science Reviews 116: 319–343. doi:10.1007/s11214-005-1960-4. Bibcode: 2005SSRv..116..319M.
* Pearl, J.C.; Conrath, B.J.; Hanel, R.A.; Pirraglia, J.A. (1990). "The Albedo, Effective Temperature, and Energy Balance of Uranus as Determined from Voyager IRIS Data". Icarus 84: 12–28. doi:10.1016/0019-1035(90)90155-3. Bibcode: 1990Icar...84...12P.
* Reese, E.J.; Solberg, H.G. (1966). "Recent measures of the latitude and longitude of Jupiter's red spot". Icarus 5 (1–6): 266–273. doi:10.1016/0019-1035(66)90036-4. Bibcode: 1966Icar....5..266R.
* Ridpath, I. (1998). Norton's Star Atlas and Reference Handbook (19th ed.). Harlow: Addison Wesley Longman. p. 107.
* Rogers, J.H. (1995). The Giant Planet Jupiter. Cambridge: Cambridge University Press. ISBN 0521410088. OCLC 219591510.
* Rogers, J.H.; Metig, H.J. (2001). "Jupiter in 1998/99". Journal of the British Astronomical Association 111 (6): 321–332.
* Rogers, J.H. (2003). "Jupiter in 1999/2000. II: Infrared wavelengths". Journal of the British Astronomical Association 113 (3): 136–140.
* Rogers, J.H. (2008). "The accelerating circulation of Jupiter’s Great Red Spot". Journal of the British Astronomical Association 118 (1): 14–20.
* Sanchez-Lavega, A.; Orton, G.S.; Morales R. et al. (2001). "The Merger of Two Giant Anticyclones in the Atmosphere of Jupiter". Icarus 149 (2): 491–495. doi:10.1006/icar.2000.6548.
* Sanchez-Lavega, A.; Orton, G.S.; Hueso, S. et al. (2008). "Depth of the strong Jovian jet from a planetary scale disturbance driven by storms". Nature 451 (7177): 437–440. doi:10.1038/nature06533. PMID 18216848. Bibcode: 2008Natur.451..437S.
* Seiff, A.; Kirk, D.B.; Knight, T.C.D. et al. (1998). "Thermal structure of Jupiter's atmosphere near the edge of a 5-μm hot spot in the north equatorial belt". Journal of Geophysical Research 103: 22857–22889. doi:10.1029/98JE01766. Bibcode: 1998JGR...10322857S.
* Smith, B.A.; Soderblom, L.A.; Johnson, T.V. et al. (1979). "The Jupiter system through the eyes of Voyager 1". Science 204 (4396): 951–957, 960–972. doi:10.1126/science.204.4396.951. PMID 17800430. Bibcode: 1979Sci...204..951S.
* Stone, P.H. (1974). "On Jupiter's Rate of Rotation" (pdf). Journal of Atmospheric Sciences 31: 1471–1472. doi:10.1175/1520-0469(1974)031<1471:OJROR>2.0.CO;2.
* Vasavada, A.R.; Showman, A. (2005). "Jovian atmospheric dynamics: An update after Galileo and Cassini". Reports on Progress in Physics 68: 1935–1996. doi:10.1088/0034-4885/68/8/R06. Bibcode: 2005RPPh...68.1935V.
* Yelle, R.V.; Miller, S. (2004). "Jupiter’s Thermosphere and Ionosphere". in Bagenal, F.; Dowling, T.E.; McKinnon, W.B.. Jupiter: The Planet, Satellites and Magnetosphere. Cambridge: Cambridge University Press.

Further reading

* [Numerous authors] (1999). Beatty, Kelly J.; Peterson, Carolyn Collins; Chaiki, Andrew. ed. The New Solar System (4th ed.). Massachusetts: Sky Publishing Corporation. ISBN 0933346867. OCLC 39464951.
* Peek, Bertrand M. (1981). The Planet Jupiter: The Observer's Handbook (Revised ed.). London: Faber and Faber Limited. ISBN 0571180264. OCLC 8318939.
* Yang, Sarah (April 21, 2004). "Researcher predicts global climate change on Jupiter as giant planet's spots disappear". UC Berkeley News. Retrieved 2007-06-14.
* Youssef, Ashraf; Marcus, Philip S. (2003). "The dynamics of jovian white ovals from formation to merger". Icarus 162 (1): 74–93. doi:10.1016/S0019-1035(02)00060-X. Retrieved 2007-06-15.
* Williams, Gareth P. (1975). "Jupiter's atmospheric circulation.". Nature 257 (5529): 778. doi:10.1038/257778a0.
* Williams, Gareth P. (1978). "Planetary Circulations: 1. Barotropic representation of Jovian and terrestrial turbulence". Journal of the Atmospheric Sciences 35: 1399–1426. doi:10.1175/1520-0469(1978)035<1399:PCBROJ>2.0.CO;2.
* Williams, Gareth P. (1985). "Jovian and comparative atmospheric modeling". Advances in Geophysics 28A: 381–429.
* Williams, Gareth P. (1997). "Planetary vortices and Jupiter's vertical structure". Journal of Geophysical Research 102 (E4): 9303–9308. doi:10.1029/97JE00520.
* Williams, Gareth P. (1996). "Jovian Dynamics. Part I: Vortex stability, structure, and genesis". Journal of the Atmospheric Sciences, 53 (18): 2685–2734.. doi:10.1175/1520-0469(1996)053<2685:JDPVSS>2.0.CO;2.
* Williams, Gareth P. (2002). "Jovian Dynamics.Part II: The genesis and equilibration of vortex sets". Journal of the Atmospheric Sciences, 59: 1356–1370. doi:10.1175/1520-0469(2002)059<1356:JDPITG>2.0.CO;2.
* Williams, Gareth P. (2003). "Jovian Dynamics, Part III: Multiple, migrating, and equatorial jets". Journal of the Atmospheric Sciences, 60 (10): 1270–1296. doi:10.1175/1520-0469(2003)60<1270:JDPIMM>2.0.CO;2.
* Williams, Gareth P. (2003). "Super Circulations". Bulletin of the American Meteorological Society 84 (9): 1190.
* Williams, Gareth P. (2003). "Barotropic instability and equatorial superrotation". Journal of the Atmospheric Sciences 60 (17): 2136–2152. doi:10.1175/1520-0469(2003)060<2136:BIAES>2.0.CO;2.
* Williams, Gareth P. (2003). "Jet sets". Journal of the Meteorological Society of Japan 81 (3): 439–476. doi:10.2151/jmsj.81.439.
* Williams, Gareth P. (2006). "Equatorial Superrotation and Barotropic Instability: Static Stability Variants.". Journal of the Atmospheric Sciences 63 (5): 1548–1557. doi:10.1175/JAS3711.1.

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