Planet jupiter brief description. Atmosphere and internal structure of Jupiter. The magnetic field and rings on Jupiter Jupiter the presence of the atmosphere its composition
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Compound Jupiter's atmosphere is a gas giant in the solar system. Description of the structure, structure of the atmosphere, the Great Red Spot, photo, density, pressure.
In fact, it is foolish to determine the presence of the atmosphere of Jupiter, because this is the entire planet, since it does not have a solid crust. This is a continuous hydrogen and helium mass with impurities of other gases and air. Let's see what the atmosphere of Jupiter looks like and what chemical elements are represented.
Atmospheric composition of Jupiter
Before you is a huge accumulation of hydrogen (90%). The remaining 10% is helium, as well as small amounts of methane, ammonia, sulfur and water vapor. The atmospheric structure of Jupiter is shown in the photo.
If you move from the outer layers to the inner, you feel an increase in temperature and pressure. That is why gases are divided into layers. At depth, hydrogen transforms from a gas to a liquid, and can also become metallic.
Atmospheric layers of Jupiter
Scientists have calculated that on the atmospheric surface the pressure is equal to one bar, which corresponds to the situation on the earth's surface. Next comes the troposphere (50 km). It is represented by ammonia, ammonium hydrosulfide and water, forming attractive and noticeable red and white lines. White (colder) are called zones (gas rises), and red - belts (gases fall).
Most often, these areas are separated by wind currents, but sometimes frozen cloud structures are superimposed on the red bands and outshine them for a certain period. Scientists even managed to fix the periodic erasure of the southern strip, but the northern one does not change. Dense water clouds also affect the dynamics. If you go higher, you feel a sharp drop in temperature: from -160°C to -100°C.
Next comes the stratosphere (320 km), containing hydrocarbon haze. Here the temperature can be kept at -100°C. The stratosphere resembles the troposphere, as it is heated by the sun's rays and the internal heat of the planet. The higher the temperature, the faster the movement. The layer ends at a point where the pressure exceeds the earth's pressure by a thousand times.
Above it is the thermosphere (1000 km above the surface) with a temperature of 725°C. It is here at the poles that the auroras occur. In addition, the thermosphere is able to create a faint glow that prevents the night sky from completely plunging into darkness. The layer is heated by particles from the magnetosphere, as well as by the Sun.
At the very top is the exosphere, in which particles of gas propagate into outer space. She does not have a clear division.
Great Red Spot in Jupiter's atmosphere
Thanks to the red and white stripes, Jupiter is striking in its beauty. The outstanding feature is the Great Red Spot. It was discovered back in the 1600s. It represents the strongest storm located in the south side of the equatorial line. These hurricanes can be seen through telescopes.
The cyclone takes 6 days to rotate. It is so huge that two Earths can easily fit there. True, recent studies say that it can be reduced.
Since the Great Red Spot is colder than the band, it must be higher in the atmosphere of the planet Jupiter. While there is no exact data on the cause of the appearance of red light.
After a third of the way to the planet, hydrogen becomes metallic, which generates electrical charges. This helps to control the strong magnetic field. Jupiter rotates extremely quickly around its axis (once every 9.9 hours), so it easily feeds the field with electricity.
Jupiter's magnetic field is 20 times greater than Earth's. Moreover, radio amateurs can hear electromagnetic storms. Sometimes these signals are even stronger than solar ones.
Unlike Earth, Jupiter's atmosphere does not have a mesosphere. There is no solid surface on Jupiter, and the lowest level of the atmosphere - the troposphere - smoothly passes into the hydrogen ocean of the mantle. There are no clear boundaries between liquid and gas, because the temperature and pressure at this level are much higher than the critical points for hydrogen and helium. Hydrogen becomes a supercritical fluid at about 12 bar.
Troposphere - includes a complex system of clouds and fogs, with layers of ammonia, ammonium hydrosulfide and water. The upper ammonia clouds observed on Jupiter's "surface" are organized into numerous bands parallel to the equator and bounded by strong zonal atmospheric currents (winds) known as "jets". The stripes have different colors: darker stripes are commonly called “belts”, and light ones are called “zones”. Zones are areas of ascending flows that have a lower temperature than belts - areas of descending flows.
The origin of the stripe and jet structure is not known for certain; two models of this structure have been proposed. The surface model assumes that these are surface phenomena over stable interior regions. The deep model assumes that the bands and jets are surface manifestations of deep circulation occurring in the Jovian mantle, which consists of molecular hydrogen and is organized as a system of cylinders.
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The first attempts to explain the dynamics of Jupiter's atmosphere date back to the 1960s. They were partly based on terrestrial meteorology, well developed by that time. It was assumed that atmospheric flows on Jupiter arise due to turbulence, which in turn is supported by moist convection in the outer layer of the atmosphere (above the clouds). Wet convection is a phenomenon associated with the condensation and evaporation of water, it is one of the main phenomena that affect the formation of the earth's weather. The appearance of flows in this model is associated with the well-known property of two-dimensional turbulence - the so-called reverse cascade, in which small turbulent structures (vortices) merge and form larger vortices. Due to the finite size of the planet, such structures cannot grow beyond a certain characteristic scale, for Jupiter this is called the Rhines scale. This is due to the influence of Rossby waves. The mechanism is this: when the largest turbulent structure reaches a certain size, the energy begins to flow into Rossby waves, and not into a larger structure, the reverse cascade stops. On a spherical, rapidly rotating planet, the dispersion relation for Rossby waves is anisotropic, so the Reines scale in the direction of the parallels is larger than in the direction of the meridian. As a result, large-scale structures are formed, stretched parallel to the equator. Their meridional extent seems to be the same as the actual width of the streams. Thus, in near-surface models, vortices transfer energy to flows and therefore must disappear. |
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Surface Models of Jupiter's Atmosphere |
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The first depth model was proposed by Busse in 1976. It is based on the well-known Taylor-Prudman theorem in hydrodynamics, which is as follows: in any rapidly rotating barotropic ideal fluid, flows are organized into a series of cylinders parallel to the axis of rotation. The conditions of the theorem are probably met in the conditions of Jupiter's interior. Therefore Jupiter's hydrogen mantle may well be divided into many cylinders, in each of which the circulation is independent. At those latitudes where the outer and inner boundaries of the cylinders intersect with the visible surface of the planet, flows are formed, and the cylinders themselves are visible as zones and belts. |
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Depth Models of Jupiter's Atmosphere |
A variety of active phenomena occur in Jupiter's atmosphere, such as band instability, eddies (cyclones and anticyclones), storms, and lightning. Vortices look like large red, white and brown spots (ovals). The two largest spots, the Great Red Spot (GRS) and oval BA, are reddish in color. They, like most other large spots, are anticyclones. Small anticyclones are usually white. It is assumed that the depth of the eddies does not exceed several hundred kilometers.
Located in the southern hemisphere, the BKP is the largest known vortex in the solar system. This vortex could house several Earth-sized planets and has been around for at least 350 years. Oval BA, which is located south of the BKP and is three times smaller than the latter, is a red spot that formed in 2000 when three white ovals merged.
Strong storms with thunderstorms constantly rage on Jupiter. A storm is the result of moist convection in the atmosphere associated with the evaporation and condensation of water. These are areas of strong upward movement of air, which leads to the formation of bright and dense clouds. Storms form mainly in belt regions. Lightning discharges on Jupiter are much stronger than on Earth, but there are fewer of them, so the average level of lightning activity is close to that of the Earth.
Information about the state of the upper atmosphere was obtained by the Galileo probe during its descent into the atmosphere of Jupiter.
Since the lower boundary of the atmosphere is not exactly known, a pressure level of 10 bar, 90 km below the pressure of 1 bar, with a temperature of about 340 K, is considered to be the base of the troposphere. In the scientific literature, a pressure level of 1 bar is usually chosen as the zero point for Jupiter's "surface" heights. As on Earth, the upper level of the atmosphere - the exosphere - does not have a well-defined boundary. Its density gradually decreases, and the exosphere smoothly passes into interplanetary space approximately 5000 km from the "surface".
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Cloud layers lie deeper than expected, including heavy ammonia clouds, according to data from the Juno spacecraft. Rather than being confined to the upper layers of the clouds, ammonia appears to be concentrated much deeper, at depths of 350 kilometers. The signature of ammonia was recorded between the surface clouds (which start at a depth of 100 km) and the convective region (500 km). |
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Atmosphere of Jupiter |
Vertical temperature variations in the Jovian atmosphere are similar to those on Earth. The temperature of the troposphere decreases with height until it reaches a minimum called the tropopause, which is the boundary between the troposphere and stratosphere. On Jupiter, the tropopause is about 50 km above visible clouds (or the 1 bar level), where pressure and temperature are close to 0.1 bar and 110 K. about 320 km and 1 mbar. In the thermosphere, the temperature continues to rise, eventually reaching 1000 K at approximately 1000 km and at a pressure of 1 nanobar.
Jupiter's troposphere is characterized by a complex structure of clouds. The upper clouds, located at a pressure level of 0.6-0.9 bar, consist of ammonia ice. It is assumed that there is a lower layer of clouds, consisting of ammonium hydrosulfide (or ammonium sulfide) (between 1-2 bar) and water (3-7 bar). These are definitely not clouds of methane, since the temperature there is too high for it to condense. Water clouds form the densest layer of clouds and have a strong influence on atmospheric dynamics. This is the result of the high condensation heat of water and its higher content in the atmosphere compared to ammonia and hydrogen sulfide (oxygen is a more common chemical element than nitrogen or sulfur).
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An example of ammonia clouds on Jupiter
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Atmosphere of Jupiter |
Various tropospheric (200-500 mbar) and stratospheric (10-100 mbar) fog layers are located above the main cloud layer. The latter consist of condensed heavy polycyclic aromatic hydrocarbons or hydrazine, which are formed in the stratosphere (1-100 microbars) under the influence of solar ultraviolet radiation on methane or ammonia. The abundance of methane relative to molecular hydrogen in the stratosphere is 10 -4 , while the ratio of other hydrocarbons, such as ethane and acetylene, to molecular hydrogen is about 10 -6 .
Jupiter's thermosphere is located at a pressure level below 1 microbar and is characterized by phenomena such as atmospheric glow, aurora and x-rays. Within this level of the atmosphere, an increase in the density of electrons and ions forms the ionosphere. The reasons for the predominance of high temperatures (800-1000 K) in the atmosphere have not been fully explained; current models do not predict temperatures above 400 K. This may be due to adsorption of high-energy solar radiation (ultraviolet or X-ray), heating of charged particles from acceleration in Jupiter's magnetosphere, or scattering of upward propagating gravitational waves.
At low latitudes and poles, the thermosphere and exosphere are sources of X-rays, which was first observed by the Einstein Observatory in 1983. Energetic particles from Jupiter's magnetosphere are responsible for the bright auroral ovals that surround the poles. Unlike terrestrial counterparts, which appear only during magnetic storms, auroras in the atmosphere of Jupiter are observed constantly. Jupiter's thermosphere is the only place outside the Earth where a triatomic ion (H 3 +) has been found. This ion causes strong mid-infrared emission at wavelengths between 3 and 5 µm and acts as the main coolant of the thermosphere.
Chemical composition
The atmosphere of Jupiter has been studied most fully relative to other atmospheres of gas giants, since it was directly probed by the Galileo descent spacecraft, which was launched into the atmosphere of Jupiter on December 7, 1995. Also sources of information are the observations of the Infrared Space Observatory (ISO), interplanetary probes Galileo and Cassini, as well as data from ground-based observations.
The gaseous envelope surrounding Jupiter is predominantly composed of molecular hydrogen and helium. The relative amount of helium is 0.157 ± 0.0036 in relation to molecular hydrogen in terms of the number of molecules and its mass fraction, 0.234 ± 0.005, is not much lower than the primary value in the solar system. The reason for this is not entirely clear, but being denser than hydrogen, most helium can condense into Jupiter's core. The atmosphere also contains many simple compounds, such as water, methane (CH 4), hydrogen sulfide (H 2 S), ammonia (NH 3) and phosphine (PH 3). Their relative abundance in the deep (below 10 bar) troposphere implies that Jupiter's atmosphere is 3-4 times richer in carbon, nitrogen, sulfur and possibly oxygen than the Sun. The number of noble gases, such as argon, krypton and xenon, exceeds the number of those on the Sun (see table), while neon is clearly less. Other chemical compounds, arsine (AsH 3) and german (GeH 4), are present only in trace amounts. Jupiter's upper atmosphere contains small relative amounts of simple hydrocarbons: ethane, acetylene, and diacetylene, which are formed under the influence of solar ultraviolet radiation and charged particles arriving from Jupiter's magnetosphere. Carbon dioxide, carbon monoxide, and water in the upper atmosphere are thought to owe their presence to impacts on Jupiter's atmosphere from comets such as Comet Shoemaker-Levy 9. Water cannot come from the troposphere because the tropopause, acting as a cold trap, effectively prevents the rise of water to the level of the stratosphere.
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Element |
The sun |
Jupiter/Sun |
3.6 ± 0.5 (8 bar) |
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0.033 ± 0.015 (12 bar) |
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The prevalence of elements in the ratio |
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Attitude |
The sun |
Jupiter/Sun |
0.0108±0.0005 |
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2.3±0.3*10 -3 |
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1.5 ± 0.3*10 -4 |
1.66 ± 0.05*10 -4 |
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3.0±0.17*10 -5 |
2.25±0.35*10 -5 |
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Isotope ratio on Jupiter and the Sun |
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Ground-based observations, as well as observations from spacecraft, have led to improved knowledge of the isotope ratio in Jupiter's atmosphere. As of July 2003, the accepted value for the relative abundance of deuterium is (2.25 ± 0.35)*10 -5 , which is probably the original value for the protosolar nebula from which the solar system formed. The ratio of nitrogen isotopes 15 N and 14 N in the atmosphere of Jupiter is 2.3 * 10 -3, which is one third lower than in the earth's atmosphere (3.5 * 10 -3). The latter discovery is particularly significant, since previous theories of the formation of the solar system believed that terrestrial values for nitrogen isotopes were primordial.
Unlike Earth's clouds, which are all water, Jupiter's clouds contain various compounds of hydrogen, carbon, nitrogen, oxygen, sulfur, and phosphorus. Their composition is determined by pressure, temperature, illumination and atmospheric movements. It has long been known that ammonia (NH 3) and methane (CH 4) are present in the atmosphere of Jupiter, the molecules of which contain a lot of hydrogen. But ammonia, methane, water vapor, ammonium hydrosulfide (NH 3 H 2 S) are all small components of the part of Jupiter's atmosphere accessible to study. Note that the strong bands of ammonia vapor inherent in Jupiter are barely noticeable around Saturn, while Uranus and Neptune do not have them at all, since all ammonia is frozen deep under their cloud layers. On the other hand, the methane bands of these planets become very wide and occupy a significant part of the spectrum in its red-blue part, which gives these planets a blue-green color.
At the cloud level of Jupiter, the content of water vapor is 1.5*10 -3, methane 8.3*10 -3, ammonium hydrosulfide in the gas phase 2.8*10 -5, ammonia 1.7*10 -4. At the same time, the ammonia content is variable and depends on the height. It is he who forms the visible cloud cover; its condensation temperature depends on pressure and is 130-200 K, which on average coincides with what is observed at the level of clouds. At a temperature of 165 K, the pressure of ammonia above the crystals of ammonia ice is 1.9 mbar, and doubles at 170 K. To condense methane at the same pressures, a much lower temperature, 79 K, is needed. Therefore, methane in the atmosphere of Jupiter into a solid phase, apparently does not condense.
In the clouds, along with crystals, drops of liquid ammonia should be present. The color of clouds with such a mixture is white with a slight yellowish tinge, characteristic of the zones. However, some other coloring agent is needed to explain the red-brown hues of the belts. Apparently, phosphine (PH 3) - a gaseous compound of phosphorus with hydrogen, the content of which is about 6 * 10 -7, gives the belts some color shades. At temperatures from 290 to 600 K, it decomposes with the release of red phosphorus. Conversely, at low temperatures, phosphorus recombines with hydrogen. The color of the clouds can also be associated with hydrogen and ammonium polysulfides and sulfur. The list of gases present in Jupiter's atmosphere also includes ethane, acetylene, and a small amount of hydrocyanic acid (HCN).
It should be remembered that the visible surface of the clouds is a thin layer, only a few tens of kilometers. Under the clouds of crystalline ammonium there are other layers: from ammonium sulfite, an aqueous solution of ammonia, from crystals of water ice, and finally from drops of water.
Zones, belts and vortices
The visible surface of Jupiter is divided into many bands parallel to the equator. There are two types of bands: relatively light zones and dark bands. The wide equatorial zone (EZ) extends roughly between latitudes 7°S and 7°N. Above and below the EZ are the Northern and Southern Equatorial Belts (NEB and SEB) extending to 18°N and 18°S respectively. Farther from the equator lie the Northern and Southern Tropical Zones (NtrZ and STrZ). This constant alternation of belts and zones continues up to 50°S and N, where their visible manifestations become somewhat less noticeable. The belts probably continue up to about 80° north or south towards the poles.
The difference in coloration between the zones and belts lies in the differences between the opacity of the clouds. Ammonia concentrations are higher in the zones, resulting in denser clouds of ammonia ice at higher altitudes, which in turn makes the zones brighter. On the other hand, belt clouds are thinner and located at lower altitudes. The upper troposphere is colder in zones and warmer in belts. The exact nature of the substances that make Jupiter's zones and belts so "colourful" is unknown, but they may include complex compounds of sulfur, phosphorus and carbon.
The Jupiter belts are bordered by zonal atmospheric flows (winds), which are called "jets". Jets moving westward (retrograde motion) are usually observed when moving from zones to belts (farther from the equator), while those moving eastward (normal motion) are usually observed when moving from belts to zones. Models of Jupiter's atmosphere suggest that zonal winds decrease in belt speed and increase in zones from the equator to the poles. Therefore, the wind gradient in the belts is cyclonic, and in the zones it is anticyclonic. The equatorial zone is an exception to the rule, in which there is a strong movement of jets to the east, and the local minimum of wind speed is located exactly on the equator. The speed of the jets on Jupiter is very high, in some places it reaches 100 m/s. This speed corresponds to clouds of ammonia located in the pressure range of 0.7-1 bar. Jets circling in the same direction as Jupiter is stronger than those circling against (retrograde). The vertical dimensions of the jets are unknown. Zonal winds die out at a height equal to 2-3 altitude scales above the clouds. At the same time, the wind speed below the cloud level increases only slightly and remains constant up to a pressure level of 22 bar - the maximum depth reached by the Galileo lander.
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Schematic representation of the location of Jupiter's cloud bands, they are designated by their official abbreviations. The Great Red Spot and oval BA are located in the southern tropics and southern temperate zones, respectively. The Jupiterian atmosphere is divided into zones and belts, and each of them has its own name and has special distinctive characteristics. They start from the south and north polar regions, which extend from the poles to about 40-48° N/S. These bluish-gray areas are usually featureless. The texture of cloudiness, typical for belts and zones, is sometimes disturbed by atmospheric disturbances (perturbations). One of these particularly stable and long-lived disturbances in the Southern Tropical Zone is called " Southern tropical perturbation» (STD). The history of observation marks one of the longest periods of existence of the STD, when it could be clearly distinguished from 1901 to 1939. The perturbation was first noticed by Percy B. Molesworth on February 28, 1901. The perturbation resulted in a partial obscuration of the normally bright STZ. Since then, several similar perturbations have been observed in the South Tropical Zone. |
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Atmosphere of Jupiter |
The origin of the "ribbon structure" of Jupiter's clouds is not entirely clear, but the mechanisms that control it resemble the Earth's Hadley cell. The simplest interpretation is that zones are places of atmospheric upwelling, and belts are manifestations of downwelling. In the zones, the air, rising and enriched with ammonia, expands and cools, forming high and dense clouds. In the belts, the air sinks and heats up adiabatically, and the white ammonia clouds evaporate, revealing the darker clouds below. The location and width of the bands on Jupiter are stable and have rarely changed over the period from the 1980s to the 2000s. One example of a change is a slight decrease in the speed of a powerful eastward jet between the northern tropical zones and the northern temperate zones by 23°N. However, the stripes change in color and intensity of colors over time.
Atmospheric dynamics
Since 1966, it has been known that Jupiter radiates much more heat than it receives from the Sun. It is assumed that the ratio between the radiation power of the planet and the received solar radiation is approximately equal to 1.67 ± 0.09. Jupiter's internal heat flux is 5.44 ± 0.43 W/m 2 , while the total radiated power is 335 ± 26 PW. The latter value is approximately one billionth of the total power radiated by the Sun.
Measurement of heat fluxes emanating from Jupiter showed that there are practically no differences between the polar and equatorial regions, its day and night sides. A significant role in this is played by the heat supply due to advection - the transfer of gas in the horizontal movements of the atmosphere. Against the background of the ordered structure of belts and zones, eddies and plumes, fast gas flows are observed - winds with a speed of up to 120 m/s. If we take into account the large heat capacity of hydrogen, then the constancy of temperature in different regions of the planet will not be surprising.
The reason for the powerful circulation that delivers heat to the cloud layer is undoubtedly the heat flow emanating from the bowels of the planet. In many scientific papers, one can read that additional energy in the depths of Jupiter and other giant planets is released as a result of their very slow compression; moreover, calculations show that for this it is enough to compress the planet by millimeters per year. However, information about the structure of Jupiter does not support this hypothesis.
An analysis of the movement of spacecraft in the gravitational field of the planet makes it possible to judge the structure of its bowels and the state of matter. The movement of the vehicles shows that this is a gas-liquid planet, consisting of a mixture of hydrogen and helium, and that it does not have a solid surface. The figure of Jupiter is mathematically perfect, which can only be a liquid planet. The dimensionless moment of inertia has a very low value: 0.254. This indicates a high concentration of mass in the center of the planet. A significant part of its core is in a liquid state. A liquid core is practically incompressible. The source of the heat flow can be the heat released during the formation of the planet (4.5 billion years ago), stored in the core and shells of Jupiter.
There is evidence that in the early stages of evolution, Jupiter radiated huge streams of energy into space. The Galilean satellites of Jupiter, located incomparably closer to their planet than to the Sun, received more energy per unit area than Mercury from the Sun. Traces of these events are preserved on the surface of Ganymede. Calculations show that the peak luminosity of Jupiter could reach 1/10 of the luminosity of the Sun. In the rays of Jupiter, ice melted on the surface of all satellites, partially including Ganymede. The relict heat of the planet is preserved from that distant era. And at present, an important source of heat can be the slow immersion towards the center of the planet of helium, which is denser than hydrogen.
The circulation in Jupiter's atmosphere differs markedly from that on Earth. The surface of Jupiter is liquid, there is no solid surface. Therefore, convection can occur in any region of the outer gaseous envelope. There is as yet no comprehensive theory of the dynamics of Jupiter's atmosphere. Such a theory should explain the following facts: the existence of narrow stable bands and flows symmetrical about the equator, a powerful equatorial flow from west to east (in the direction of the planet's rotation), the difference between zones and belts, as well as the origin and stability of large eddies, such as the Great Red Spot .
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In the planet's warm regions near the ector, each convection cell in Jupiter's atmosphere lifts matter up where it cools and then dumps it closer to the poles. And this process is ongoing. As the mixture of gases rises, they first condense, and then, higher, clouds of ammonium hydrosulfide form. Clouds of ammonia, located in the bright zones of Jupiter, appear only at the highest point. The upper layers of the atmosphere are moving west, in the direction of the rotation of the planet itself. While the Coriolis forces push the ammonia clouds in the opposite direction. |
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Atmosphere of Jupiter |
There are practically no meridional currents in Jupiter's atmosphere. Zones and belts are areas of ascending and descending flows in the atmosphere, which have a global extent in the longitudinal direction. These atmospheric currents, parallel to the equator, bear some resemblance to the Earth's trade winds. The driving forces in this natural heat engine are heat flows coming from the depths of the planet, energy received from the Sun, as well as the rapid rotation of the planet. The visible surfaces of zones and belts in this case should be at different heights. This was confirmed by thermal measurements: the zones turned out to be colder than the belts. The difference in temperatures shows that the visible surface of the zones is located about 20 km higher. The BKP turned out to be higher and several degrees colder than the belts. Conversely, blue spots turned out to be sources of thermal radiation rising from the deep layers of the atmosphere. No significant temperature difference was found between the polar and equatorial regions of the planet. Indirectly, this allows us to draw the following conclusion: the internal heat of the planet plays a more important role in the dynamics of its atmosphere than the energy received from the Sun. The average temperature at the level of visible clouds is close to 130 K.
Based on ground-based observations, astronomers divided the belts and zones in the atmosphere of Jupiter into equatorial, tropical, temperate and polar. The heated masses of gases rising from the depths of the atmosphere in the zones under the action of significant Coriolis forces on Jupiter are stretched in the longitudinal direction, and the opposite edges of the zones move towards each other, along the parallels. Strong turbulence is visible at the boundaries of zones and belts (regions of downdrafts); movement speeds here reach the highest values, up to 100 m/s, and in the equatorial region even 150 m/s. To the north of the equator, flows in zones directed to the north are deflected by Coriolis forces to the east, and those directed to the south - to the west. In the southern hemisphere, the direction of deviations is reversed. It is this structure of movements on Earth that the trade winds form. The "roof" of clouds in belts and zones is located at different heights. Differences in their coloration are determined by the temperature and pressure of phase transitions of small gaseous components. Light zones are ascending columns of gas with a high content of ammonia, belts are descending streams depleted in ammonia. The bright color of the belts is probably associated with ammonium polysulfides and some other coloring components, for example, phosphine.
Vortices in Jupiter's atmosphere
Experimental data testify that the dynamics of Jupiter's cloud layer is only an external manifestation of powerful forces acting in the planet's subcloud atmosphere. It was possible to observe how a powerful vortex formation, a local hurricane, with a diameter of 1000 km or more, arises in the clouds. Such formations live for a long time, several years, and the largest of them - even several hundred years. Such vortices are formed, for example, as a result of the movement of large masses of rising heated gas in the atmosphere.
The resulting vortex brings heated masses of gas with vapors of small components to the surface of the clouds, which closes the circuit of their circulation in the atmosphere. The resulting crystals of ammonia snow, solutions and compounds of ammonia in the form of snow and drops, ordinary water snow and ice gradually descend in the atmosphere and reach a temperature level where they evaporate. In the gas phase, the matter returns to the cloud layer again.
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Changes on Jupiter in the visible range and IR |
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Atmosphere of Jupiter |
Jupiter's atmosphere is home to hundreds of vortices: circular, rotating structures that, like Earth's atmosphere, can be divided into two classes: cyclones and anticyclones. The former rotate in the direction of the planet's rotation (counterclockwise in the northern hemisphere and clockwise in the southern hemisphere); the second - in the opposite direction. However, unlike the Earth's atmosphere, in Jupiter's atmosphere, anticyclones prevail over cyclones: of the eddies whose diameter exceeds 2000 km, more than 90% are anticyclones. The "lifetime" of eddies varies from several days to centuries, depending on their size: for example, the average lifetime of anticyclones with diameters from 1000 to 6000 km is 1-3 years. Vortices have never been observed at Jupiter's equator (within 10° latitude), where they are unstable. As with any rapidly rotating planet, Jupiter's anticyclones are centers of high pressure, while cyclones are centers of low pressure.
Jupiter's anticyclones are always limited to areas where wind speeds increase from the equator to the poles. They are usually bright and appear as white ovals. They can move in longitude, but remain in the same latitude, unable to leave the zone that gave birth to them. The wind speed at their periphery can reach 100 m/s. Different anticyclones located in the same zone tend to unite when approaching each other. However, in the atmosphere of Jupiter, two anticyclones unlike the others were observed and are observed - this is the Great Red Spot (GRS) and the oval BA, which formed in 2000. Unlike white ovals, their structure is dominated by a red color - probably due to a reddish substance rising from the depths of the planet. On Jupiter, anticyclones usually form from the merging of smaller structures, including convective storms, although large ovals can also form from unstable jets. The last time this was seen was in 1938-1940, when several white ovals were generated by instability in the southern temperate zone; they later merged to form Oval BA.
In contrast to anticyclones, Jovian cyclones are compact dark structures with an irregular shape. The darkest and most regular cyclones are called brown ovals. However, the existence of several large long-lived cyclones is not excluded. In addition to compact cyclones, several irregularly shaped filamentous "chunks" can be observed on Jupiter, in which cyclonic rotation is observed. One of them is located west of the BKP in the southern equatorial belt. These "chunks" are called cyclonic regions (CR). Cyclones always form only in belts, and, like anticyclones, they merge when approaching.
The deep structure of eddies is not completely clear. They are thought to be relatively thin, as any thickness above about 500 km would lead to instability. Large anticyclones do not rise above several tens of kilometers relative to the observed cloudiness. One hypothesis suggests that eddies are deep convection "feathers" (or "convection columns"), but at the moment it has not gained popularity among planetary scientists.
Vortex formations like spots of blue and brown hues were observed not only in stable belts and zones, but also in the polar regions of Jupiter. Here, the characteristic appearance of the cloud layer is a light brown field with dark and light brown and bluish spots. Here, in the area of those latitudes where zonal circulation becomes unstable, belts and zones give way to meteorological formations such as "lace collars" and "plumes". Areas near the pole of the planet can only be seen from spacecraft. The apparent chaos of the spots nevertheless obeys the general regularity of circulation, and the determining role is played by movements in the depths of the atmosphere.
Taking a number of assumptions, theorists managed to obtain phenomena in a cylindrical model that resemble what is seen on Jupiter (and Saturn). The structure of the planet is a system of nested cylinders, the axis of which is the polar axis. The cylinders pass through the entire planet and come to the surface at, say, 40°N. sh. and at 40°S sh. What we see are sections of these cylinders rotating at different speeds. If you count from the equator, then the cylinders penetrate deep into half the radius of the planet. Spots or ovals are also through columns sandwiched between cylinders. By the way, some observers point out that symmetrically at the same latitude in the northern hemisphere, a spot of the same size, but less pronounced, is sometimes seen.
Child blue spots may be observed through breaks in the cloud layer. However, breaks are often unrelated to spots and lower cloud layers are visible through them. A series of similar breaks was observed along the boundary of the Northern equatorial belt. Gaps exist for quite a long time, for several years. The increased heat flow from these places testifies that these are breaks. Temperature increases rapidly with depth. Already at a pressure level of 2 bar, it is approximately 210 K. And radio emission coming from great depths indicates a higher temperature. According to calculations, at a depth of 300 km, the atmosphere of Jupiter is as hot as the atmosphere of Venus near its surface (about 730 K).
Thunderstorms on Jupiter
Lightning is also recorded in Jupiter's atmosphere. Images from the Voyagers showed that on the night side of Jupiter there are light flashes of colossal extent - up to 1000 km or more. These are super-lightnings, the energy in which is much greater than in the terrestrial ones. It turned out, however, that Jupiter's lightning is less numerous than Earth's. Interestingly, Jupiter's lightning was detected 3 months after the discovery of thunderstorms on Venus.
Thunderstorms on Jupiter are similar to those on Earth. They manifest themselves as bright and massive clouds approximately 1000 km in size, which appear from time to time in the cyclonic regions of the belts, especially within strong westerly directed jets. Unlike eddies, thunderstorms are short-lived phenomena, the most powerful of them can last several months, while the average duration of existence is 3-4 days. It is believed that they are a consequence of wet convection in the layers of the Jupiter troposphere. In fact, thunderstorms are "convection columns" (feathers) that raise moist air masses from the depths higher and higher until they condense into clouds. The typical height of Jovian thunderclouds is 100 km, which means they extend to a pressure level of about 5-7 bar, while hypothetical water clouds start at a pressure level of 0.2-0.5 bar.
Thunderstorms on Jupiter, of course, are not complete without lightning. Images of the night side of Jupiter obtained by the Galileo and Cassini spacecraft make it possible to distinguish regular flashes of light in the Jupiterian belts and near the westward jets, mainly at latitudes of 51°N, 56°S and 14°S. Lightning strikes on Jupiter are generally more powerful than on Earth. However, they occur much less frequently, and they create about the same amount of light with their flashes as earthly ones. Several lightning flashes have been recorded in Jupiter's polar regions, making Jupiter the second planet after Earth to see polar lightning.
Every 15-17 years, a particularly powerful period of thunderstorm activity begins on Jupiter. It mainly manifests itself at a latitude of 23°C, where the strongest eastward jet is located. The last time this happened was in June 2007. It is curious that two thunderstorms located separately at longitude 55 ° in the Northern temperate zone had a significant impact on the belt. Matter of dark color, created by thunderstorms, mixed with the cloudiness of the belt and changed its color. Thunderstorms moved at a speed of about 170 m/s, even slightly faster than the jet itself, which indirectly indicates the existence of even stronger winds in the deep layers of the atmosphere.
Jupiter's atmosphere is characterized by high-speed winds blowing within wide bands parallel to the planet's equator, with winds directed in opposite directions in adjacent bands on Jupiter. Winds on Jupiter reach speeds of 500 km/h. Jupiter's atmosphere creates a gigantic pressure that increases as you approach the center of the planet. The layer farthest from the core consists primarily of ordinary molecular hydrogen and helium, which are in a liquid state inside and gradually turn into a gaseous outside. On Jupiter there are bands limited in latitude, within which winds blow at very high speeds, and their directions are opposite in adjacent bands. The slight difference in chemical composition and temperature between these regions is enough for them to appear as colored bands. Light stripes are called zones, dark - belts. Jupiter's atmosphere is highly turbulent. The bright colors seen in Jupiter's clouds are the result of various chemical reactions between elements present in the atmosphere, possibly including sulfur, which can produce a wide range of colors, but details are not yet known.
Moons of Jupiter
By the beginning of the third millennium, Jupiter has 28 known satellites. Four of them are large and heavy. They move in almost circular orbits in the plane of the planet's equator. The 20 outer satellites are so far from the planet that they are invisible from its surface to the naked eye, and Jupiter in the sky of the most distant of them looks smaller than the Moon. A number of small satellites move in almost identical orbits. All of them are the remnants of Jupiter's larger satellites, destroyed by its gravity. The outer satellites of Jupiter could well be captured by the gravitational field of the planet: they all revolve around Jupiter in the opposite direction.
Satellite of Jupiter.io
Orbit = 422,000 km from Jupiter Diameter = 3630 km Mass = 8.93*1022 kg
Io is the third largest and closest moon of Jupiter. Io is slightly larger than the Moon Unlike most satellites in the outer solar system, Io and Europa are similar in composition to terrestrial planets, primarily in the presence of silicate rocks. Io has an iron core with a radius of 900 km. The surface of Io is radically different from the surface of any other body in the solar system. Very few craters have been found on Io, hence its surface is very young. The material erupting from Io's volcanoes is some form of sulfur or sulfur dioxide. Volcanic eruptions change rapidly. The energy for all this activity Io probably receives from tidal interactions with Europa, Ganymede and Jupiter. Io crosses Jupiter's magnetic field lines, generating an electrical current. Io may have its own magnetic field, like Ganymede. Io has a very rarefied atmosphere, consisting of sulfur dioxide and some other gases. Unlike other moons of Jupiter, Io has very little or no water. Io has a solid metal core surrounded by a rocky mantle, similar to Earth's. The shape of Io under the influence of Jupiter is greatly distorted. Io is permanently oval due to Jupiter's rotation and tidal influence.
Planet characteristics:
- Distance from the Sun: ~ 778.3 million km
- Planet Diameter: 143,000 km*
- Days on the planet: 9h 50min 30s**
- Year on the planet: 11.86 years old***
- t° on the surface: -150°C
- Atmosphere: 82% hydrogen; 18% helium and minor traces of other elements
- Satellites: 16
* diameter at the equator of the planet
** period of rotation around its own axis (in Earth days)
*** orbital period around the Sun (in Earth days)
Jupiter is the fifth planet from the Sun. It is located at a distance of 5.2 astronomical years from the Sun, which is approximately 775 million km. The planets of the solar system are divided by astronomers into two conditional groups: terrestrial planets and gas giants. Jupiter is the largest of the gas giants.
Presentation: planet Jupiter
The dimensions of Jupiter exceed the dimensions of the Earth by 318 times, and if it were even larger by about 60 times, it would have every chance of becoming a star due to a spontaneous thermonuclear reaction. The planet's atmosphere is about 85% hydrogen. The remaining 15% is mainly helium with impurities of ammonia and sulfur and phosphorus compounds. Jupiter also contains methane in its atmosphere.
With the help of spectral analysis, it was found that there is no oxygen on the planet, therefore, there is no water - the basis of life. According to another hypothesis, there is still ice in the atmosphere of Jupiter. Perhaps no planet in our system causes so much controversy in the scientific world. Especially many hypotheses are connected with the internal structure of Jupiter. Recent studies of the planet with the help of spacecraft have made it possible to create a model that makes it possible to judge its structure with a high degree of certainty.
Internal structure
The planet is a spheroid, quite strongly compressed from the poles. It has a strong magnetic field that extends millions of kilometers into orbit. The atmosphere is an alternation of layers with different physical properties. Scientists suggest that Jupiter has a solid core 1-1.5 times the diameter of the Earth, but much denser. Its existence has not yet been proven, but it has not been refuted either.
atmosphere and surface
The upper layer of Jupiter's atmosphere consists of a mixture of hydrogen and helium gases and has a thickness of 8 - 20 thousand km. In the next layer, the thickness of which is 50 - 60 thousand km, due to the increase in pressure, the gas mixture passes into a liquid state. In this layer, the temperature can reach 20,000 C. Even lower (at a depth of 60 - 65 thousand km.) Hydrogen passes into a metallic state. This process is accompanied by an increase in temperature to 200,000 C. At the same time, the pressure reaches fantastic values of 5,000,000 atmospheres. Metallic hydrogen is a hypothetical substance characterized by the presence of free electrons and conductive electric current, as is characteristic of metals.
Moons of the planet Jupiter
The largest planet in the solar system has 16 natural satellites. Four of them, which Galileo spoke about, have their own unique world. One of them, the satellite of Io, has amazing landscapes of rocky rocks with real volcanoes, on which the Galileo apparatus, which studied the satellites, captured the volcanic eruption. The largest satellite in the solar system, Ganymede, although inferior in diameter to the satellites of Saturn, Titan and Neptune, Triton, has an ice crust that covers the surface of the satellite with a thickness of 100 km. There is an assumption that there is water under a thick layer of ice. Also, the existence of an underground ocean is also hypothesized on the Europa satellite, which also consists of a thick layer of ice, faults are clearly visible in the images, as if from icebergs. And the most ancient inhabitant of the solar system can rightfully be considered a satellite of Jupiter Calisto, there are more craters on its surface than on any other surface of other objects in the solar system, and the surface has not changed much over the past billion years.
Atmosphere of Jupiter
When the pressure of Jupiter's atmosphere reaches the pressure of the Earth's atmosphere, we will stop and look around. the usual blue sky is visible above, thick white clouds of condensed ammonia swirl around. At this altitude, the air temperature reaches -100°C.
The reddish color of part of Jupiter's clouds indicates that there are many complex chemical compounds. A variety of chemical reactions in the atmosphere are initiated by solar ultraviolet radiation, powerful lightning discharges (a thunderstorm on Jupiter must be an impressive sight!), As well as heat coming from the interior of the planet.
Jupiter's atmosphere, in addition to hydrogen (87%) and helium (13%), contains small amounts of methane, ammonia, water vapor, phosphorine, propane, and many other substances. Here it is difficult to determine due to what substances the Jovian atmosphere acquired an orange color.
The next layer of clouds consists of red-brown crystals of ammonium hydrosulfide at a temperature of -10o C. Water vapor and water crystals form a lower layer of clouds at a temperature of 20o C and a pressure of several atmospheres - almost above the very surface of Jupiter's ocean.
The thickness of the atmospheric layer, in which all these amazing cloud structures arise, is 1000 km.
Dark stripes and light zones parallel to the equator correspond to atmospheric currents of different directions (some lag behind the rotation of the planet, others are ahead of it). The speeds of these currents are up to 100 m/s. Giant eddies are formed at the boundary of multidirectional currents.
Particularly impressive is the Great Red Spot - a colossal elliptical atmospheric vortex about 15 x 30 thousand kilometers in size. When it arose is unknown, but it has been observed in ground-based telescopes for 300 years. This anticyclone sometimes almost disappears and then reappears. Obviously, it is a relative of terrestrial anticyclones, but because of its size it is much longer-lived.
Voyagers sent to Jupiter conducted a thorough analysis of the clouds, which confirmed the already existing model of the internal structure of the planet. It became quite clear that Jupiter is a world of chaos: endless storms with thunder and lightning rage there, by the way, the Red Spot is part of this chaos. And on the night side of the planet, the Voyagers registered numerous lightnings.
jupiterian ocean
Jupiter's ocean consists of the main element on the planet - hydrogen. At a sufficiently high pressure, hydrogen turns into a liquid. The entire surface of Jupiter under the atmosphere is a huge ocean of liquefied molecular hydrogen.
What waves arise in the ocean of liquid hydrogen with a superdense wind at a speed of 100 m/s? It is unlikely that the surface of the hydrogen sea has a clear boundary: at high pressures, a gas-liquid hydrogen mixture is formed on it. It looks like a continuous “boiling” of the entire surface of the Jovian ocean. The fall of a comet into it in 1994 caused a gigantic tsunami many kilometers high.
As you dive into the ocean of Jupiter for 20 thousand kilometers, pressure and temperature rapidly increase. At a distance of 46 thousand km. from the center of Jupiter, the pressure reaches 3 million atmospheres, the temperature is 11 thousand degrees. Hydrogen cannot withstand high pressure and passes into a liquid metallic state.
Core. We will plunge another 30 thousand km into the second ocean of Jupiter. Closer to the center, the temperature reaches 30 thousand degrees, and the pressure is 100 million atmospheres: here is a small (“only” 15 Earth masses!) The core of the planet, which, unlike the ocean, consists of stone and metals. There is nothing surprising in this - after all, the Sun also contains impurities of heavy elements. The core was formed as a result of the adhesion of particles consisting of heavy chemical elements. It was with him that the formation of the planet began.
Jupiter's moons and ring
Information about Jupiter and its satellites has been significantly replenished thanks to the passage of several automatic spacecraft near the planet. The total number of known satellites jumped from 13 to 16. Two of them - Io and Europa - are the size of our Moon, and the other two - Ganymede and Callisto - surpassed it in diameter by one and a half times.
Jupiter's dominion is quite extensive: the eight outer moons are so distant from it that they could not be observed from the planet itself with the naked eye. The origin of the satellites is mysterious: half of them move around Jupiter in the opposite direction (compared to the circulation of the other 12 satellites and the direction of the daily rotation of the planet itself).
The satellites of Jupiter are the most interesting worlds, each with its own “face” and history, which were revealed to us only in the space age.
Thanks to the Pioneer space stations, the previous idea about the existence of a rarefied gas-dust ring around Jupiter, similar to the famous ring of Saturn, received direct confirmation.
Jupiter's main ring is one radius away from the planet and extends 6,000 km wide. and is 1 km thick. One of the satellites circulates along the outer edge of this ring. However, even closer to the planet, almost reaching its cloudy layer, there is a system of much less dense "inner" rings of Jupiter.
It is practically impossible to see Jupiter's ring from the Earth: it is very thin and constantly turned to the observer with an edge due to the small inclination of Jupiter's axis of rotation to the plane of its orbit.