[{"@context":"http:\/\/schema.org\/","@type":"BlogPosting","@id":"https:\/\/wiki.edu.vn\/all2en\/wiki32\/magnetosphere-di-giove-wikipedia\/#BlogPosting","mainEntityOfPage":"https:\/\/wiki.edu.vn\/all2en\/wiki32\/magnetosphere-di-giove-wikipedia\/","headline":"Magnetosphere di Giove – Wikipedia","name":"Magnetosphere di Giove – Wikipedia","description":"before-content-x4 The Magnetosphere di Giove It is the largest and most powerful of all the magnetospheres of the planets of","datePublished":"2018-01-01","dateModified":"2018-01-01","author":{"@type":"Person","@id":"https:\/\/wiki.edu.vn\/all2en\/wiki32\/author\/lordneo\/#Person","name":"lordneo","url":"https:\/\/wiki.edu.vn\/all2en\/wiki32\/author\/lordneo\/","image":{"@type":"ImageObject","@id":"https:\/\/secure.gravatar.com\/avatar\/44a4cee54c4c053e967fe3e7d054edd4?s=96&d=mm&r=g","url":"https:\/\/secure.gravatar.com\/avatar\/44a4cee54c4c053e967fe3e7d054edd4?s=96&d=mm&r=g","height":96,"width":96}},"publisher":{"@type":"Organization","name":"Enzyklop\u00e4die","logo":{"@type":"ImageObject","@id":"https:\/\/wiki.edu.vn\/wiki4\/wp-content\/uploads\/2023\/08\/download.jpg","url":"https:\/\/wiki.edu.vn\/wiki4\/wp-content\/uploads\/2023\/08\/download.jpg","width":600,"height":60}},"image":{"@type":"ImageObject","@id":"https:\/\/upload.wikimedia.org\/wikipedia\/commons\/thumb\/b\/b9\/PIA04433_Jupiter_Torus_Diagram.jpg\/260px-PIA04433_Jupiter_Torus_Diagram.jpg","url":"https:\/\/upload.wikimedia.org\/wikipedia\/commons\/thumb\/b\/b9\/PIA04433_Jupiter_Torus_Diagram.jpg\/260px-PIA04433_Jupiter_Torus_Diagram.jpg","height":"195","width":"260"},"url":"https:\/\/wiki.edu.vn\/all2en\/wiki32\/magnetosphere-di-giove-wikipedia\/","wordCount":15595,"articleBody":"     (adsbygoogle = window.adsbygoogle || []).push({});before-content-x4The Magnetosphere di Giove It is the largest and most powerful of all the magnetospheres of the planets of the Solar System, as well as the largest structure of the Solar System itself not belonging to the Sun: it extends in fact in the external sun system for many times the radius of Jupiter and reaches a maximum size which can exceed the orbit of Saturn. [first] If he were visible to the naked eye from the earth, he would have an apparent extension superior to the diameter of the full moon, [2] despite its great distance. Schematic representation of the surrounding space Jupiter. The red band consists of ions captured by the magnetic field; The green and blue bands are instead neutral gas bulls originated, respectively, from I and I and Europe.        (adsbygoogle = window.adsbygoogle || []).push({});after-content-x4The magnetic field of Jupiter preserves its atmosphere from the interactions with the sun wind, a plasma flow emitted by our star, deflecting it and creating a distinct region, called magnetosphere, consisting of a plasma of composition very different from that of the sun wind. [3] Although it has a more flat shape than the Earth’s magnetosphere, the Gioviana magnetosphere has an intensity of a higher order of magnitude; The field that feeds is generated by whirlwind motions inside the metal hydrogen layer which constitutes the internal cloak of the planet. [4] The Galileian satellite, known for its intense volcanic activity, contributes to fueling the magnetosphere Gioviana generating an important plasma bull, [5] which loads and strengthens the magnetic field forming the structure called Magnetodic ; [6] It follows that the Gioviana magnetosphere, in spite of the terrestrial one, is fueled by the planet itself and by a satellite rather than the sun wind. The strong currents circulating in the magnetosphere generate intense radiation bands similar to the Van Allen Terrestrial bands, but thousands of more powerful times; [7] These forces generate perennial auror around the planet’s poles and intense variable radio emissions that effectively make Jupiter a weak radio pulsar. [8] The interaction of the energy particles with the surface of the Galilean Lunes major considerably affects the chemical and physical properties of the magnetosphere, also influenced by the subtle system of rings that orbit around the planet. [9] The existence of the magnetosphere of Jupiter was hypothesized starting from the radio observations conducted in the 1950s and was studied for the first time in detail by the Pioneer 10 probe in 1973; Since then it has been analyzed seven times by as many probes. [3]        (adsbygoogle = window.adsbygoogle || []).push({});after-content-x4The first evidence of the existence of a magnetic field around Jupiter was in 1955 when the radio decametric emission (DAM) was discovered; [ten] Since the spectrum of the Dam extends up to 40 MHz, the astronomers concluded that the planet possessed a magnetic field with a force of about 0.001 Tesla (T), corresponding to 10 Gauss (G). [11] Later, in 1959, the observations of the part of the radio spectrum to the microwave led to the discovery of the decimetric radiation Gioviana (Dim), which is emitted by the relativistic electrons blocked in the radiation belts; [twelfth] These synchronous emissions were used to estimate the number and energy of the electron population around Jupiter and allowed an increase in the values \u200b\u200bof the strength of the magnetic field. [5] The modulation of the Dam Gioviane emissions by the satellite I (called I-Dam) was discovered in 1964; His observations allowed to precisely determine the rotational period of Jupiter. [13] The definitive discovery of the magnetic field Gioviano took place in 1973, when the Pioneer 10 spatial probe flew near the planet. [14] Table of ContentsMain features in comparison with the geomagnetic field [ change | Modifica Wikitesto ] Shape and size [ change | Modifica Wikitesto ] The role of me in food the Gioviana magnetosphere [ change | Modifica Wikitesto ] Forces and currents [ change | Modifica Wikitesto ] Plasma transfer [ change | Modifica Wikitesto ] Polar Aurore [ change | Modifica Wikitesto ] Radio emission and modulation of the issue [ change | Modifica Wikitesto ] Interactions with rings and natural satellites [ change | Modifica Wikitesto ] General titles [ change | Modifica Wikitesto ] Specific titles [ change | Modifica Wikitesto ] On the sun system [ change | Modifica Wikitesto ] On the planet [ change | Modifica Wikitesto ] Scientific publications (in English) [ change | Modifica Wikitesto ] Main features in comparison with the geomagnetic field [ change | Modifica Wikitesto ] Comparison between the main parameters of the Gioviana magnetosphere and the terrestrial one. [3] [4] [15] Parameter Jupiter Earth Ray of the planet (R p , in km) 71.398 6.371 Rotation period (in hours) 9.9 24 Field intensity to the equator (in microtesla – \u03bcT -) 428 thirty first Moment of the dipole (in terrestrial units) 18,000 first Inclination of the magnetic dipole (in \u00b0) ten 11.3 Distance from magnetopause (R p ) 50\u2013100 8\u201310 Potenza in Input (In Treatment – TW -) 100 about 1 Solar wind density (in cm \u22123 ) 0.4 ten Intensity of the Solar Magnetic Field (in Nanotesla – NT -) first 6 Dominant ionic species H + , O n+ , S n+ H + , O + Unlike the earth’s magnetic field, which is generated by currents, similar to a dynamo, iron and nickel fused in the external nucleus, the magnetic field of Jupiter is produced inside the metal hydrogen layer surrounding its nucleus. [4] Like the terrestrial one, the Gioviano magnetic field is a dipole, with a north and a magnetic south placed at the ends of a single magnetic axis; [16] However, unlike what happens for our planet, the magnetic North of Jupiter is located in the northern hemisphere and the south pole in the southern hemisphere. [N 1] [17] The Gioviana magnetosphere also presents a development in multipoli (quadrupolo, ottupolo etc.), which decrease in intensity of an order of magnitude from a level to the higher one. [16] While the geomagnetic field has a “drop” shape, the Gioviana magnetosphere is more crushed, more similar to a disc, and periodically oscillates on its axis. [18] The dipole axis is inclined by 10 \u00b0 compared to the rotation axis of the planet, as well as the magnetic axis of our planet is inclined by 11.3 \u00b0 compared to the rotation axis. [14] [16] The intensity of the field to Jupiter’s equator is about 420 \u03bcT (4.2 g), which corresponds to a moment of the dipole of about 1.5 \u00d7 10 20 T\u00b7m 3 ; The magnetic field of Jupiter is therefore 10 times more intense than the terrestrial one, and its moment of the magnetic dipole 18,000 times higher. [4] The magnetic field of Jupiter revolves at the same speed of the planet’s cloak, in 9 h 55 m, and is rather stable: in fact, consistent changes in intensity or structure have not been observed from the first measurements obtained thanks to the probes of the Pioneer program in the mid -years seventy. [16]        (adsbygoogle = window.adsbygoogle || []).push({});after-content-x4Shape and size [ change | Modifica Wikitesto ] The characteristic discoid form of the Gioviana magnetosphere that interacts with the sun wind. The magnetic field of Jupiter preserves its atmosphere from the interactions with the sun wind, a plasma flow emitted by our star, deflinging it and creating a distinct region, called magnetosphere, consisting of a plasma of composition very different from that of the sun wind; [3] The gap present between the plasma of the sun wind and the magnetospheric plasma takes the name of magnetopause and is located at a distance from the planet between 45 and 100 times its radius (the radius of Jupiter – R J – Vale 71,492 km) depending on the period of the solar cycle. [3] [19] Beyond magnetopause (at an average distance of 84 R J from the planet) is the bow shock, the point where the wind flow is deflected by the magnetic field; [20] [21] The region between bow shocks and magnetopause takes the name of magnetosheath. [3] The extension of the planet magnetosphere is such that, if it were visible to the naked eye from our planet, it would appear much larger than the full moon. [2] On the opposite side, the sun wind draws the magnetic field of the planet in a long coda magnetic, whose extension can arrive far beyond the orbit of Saturn. [first] Its structure is very similar to the terrestrial one; It is made up of two lobes, whose magnetic field focuses in opposite directions: the field of the northern lobe focuses away from the planet, while the southern lobe points towards it. The lobes are divided by a weak layer of plasma called widespread current. [first] The magnetic tail acts as a channel for the plasma particles of the solar wind that manage to penetrate the internal regions of the magnetosphere, which heat up forming radiation bands at a distance of less than 10 r J from the top of the clouds. [7] The magnetosphere of Jupiter is conventionally divided into three parts: the internal magnetosphere, intermediate and external. The internal magnetosphere is located at a distance of less than 10 r J from the planet; The magnetic field inside remains substantially dipolar, since every contribution from the currents that flow from the equatorial magnetosphere plasma is small. In the intermediate regions (between 10 and 40 r J ) and external (over 40 R J ) The magnetic field is no longer dipola and is seriously disturbed by its interactions with the sun -plasma. [3] The role of me in food the Gioviana magnetosphere [ change | Modifica Wikitesto ] Although overall the shape of the magnetosphere of Jupiter resembles the terrestrial one, near the planet its structure is very different. [19] The moon, characterized by an intense volcanic activity, is a powerful source of plasma that fills the magnetosphere of the mother planet of about 1,000 kg of new material every second. [5] The strong volcanic eruptions on the surface of the satellite emit a large amount of sulfur dioxide (I know 2 ), of which a small part dissociate itself in the constituent atoms which, ionizing itself due to the ultraviolet solar radiation, produce the cations S + , O + , S ++ and the ++ . [22] These ions manage to abandon the atmosphere of the satellite, going to constitute the planes, a plasma bull, which reaches a temperature of 100,000-1,000 king, far lower than the one reached in the radiation bands (100 million Kelvin). [5] The plasma in the bull is forced to a co-rotation with Jupiter, and therefore both share the same period of rotation. [23] The bull of I therefore changes the dynamics of the Gioviana magnetosphere in a conspicuous way. [24] The interaction of I with the magnetosphere of Jupiter; In yellow the plasma bull of Io is represented. The electrical conductivity of the plasma inside the bull is not infinite; Consequently, the plasma slowly tends to move away from the planet. The main escape mechanisms are the diffusion and instability between the offices. [23] While the plasma moves away from the planet, the radial currents that flow inside them increase their speed (keeping co-rotation), which involves an increase in the kinetic energy of the plasma due to the energy of the rotation of the planet. [3] The density of the plasma is significantly variable inside the magnetosphere: the number of plasma particles ranges from a maximum of 2,000 per cm\u00b3 in the bull of I up to about 0.2 per cm\u00b3 at a distance of 35 R J ; [25] In this sense, the Gioviana magnetosphere is enhanced by the rotation of the planet, while the Earth’s magnetosphere is mainly reinforced by the solar wind. [24] However, in the intermediate magnetosphere (at distances greater than 10 r J from the planet) the co-rotation gradually is stupid and the plasma begins to rotate more slowly than the planet; [3] at distances greater than 40 R J , in the external magnetosphere, this plasma flees from the magnetic field and leaves the magnetosphere along the magnetic tail, [26] probably in the form of an unpublished planetary wind . [22] The coldest and densest plasma in motion to the outside is replaced by a less dense and warmer plasma (200 million k or higher) coming from the external magnetosphere, [25] Which, as Jupiter approaches Jupiter, undergoes adiabatic heating giving rise to the radiation bands of the internal magnetosphere, which constitute the main source of radio emission of the planet. [5] The centrifugal force of co-coating plasma draws up the field lines forming, at a distance greater than 20 r J from the planet, a flattened structure known as magnetic disc or Magnetodic . [6] This magnetisk has a weak widespread current in correspondence with the magnetic equator; [22] The lines of the field point in the opposite direction to the planet above this floor and towards it below the floor. [19] The Gioviana magnetosphere, strongly fueled by the plasma of I, expands enormously in width, since the magnetisk creates an additional pressure that balances the pressure of the sun wind. [20] If I was not exactly in that position in the Jupiter system, the distance between the top of the clouds of the planet and the magnetopause would be enormously less: 42 r J against the royal 75 r J medium. [3] So, as abundantly seen, the magnetosphere of the gaseous giant is dominated by the heavy plasma of I and is enhanced by the rotation of the planet, while the sun wind constitutes only a secondary source of plasma and energy, [24] even if it supplies the high energy protons system. [5] Forces and currents [ change | Modifica Wikitesto ] The magnetic field of Jupiter and the reinforcement currents of the co-circulation. As already seen, the main activator of the Gioviana magnetosphere is the rotation of the planet; [27] When it rotates, its ionosphere moves relatively to the dipolar magnetic field of the planet. Since the moment of magnetic dipole focuses in the same direction as rotation, [17] Lorentz’s strength, which appears as a result of this bike, transports electrons, negatively loaded, towards the poles, while the cations are headed towards the equator; [28] Consequently, the poles accumulate negative charges while the regions close to the equator become positive. Although the magnetosphere of Jupiter is full of highly conductive plasma, the electrical circuit thus constituted closed closed; [28] Electric currents follow the trend of the lines of the magnetic field: they flow from the lower latitudes of the ionosphere towards the widespread plasma (Birkeland currents), then they move away from the planet through the plasma and then, finally, return to the planetary ionosphere after crossing the external magnetosphere. The radial current interacts with the planetary magnetic field and the power of Lorentz resulting accelerates the magnetic plasma in the direction of the rotation. This is the main mechanism that maintains magnetospheric plasma in co-rotation. [28] The current that comes from the ionosphere, called direct current , is more intense if the corresponding part of widespread plasma rotates more slowly than the planet. [28] As mentioned before, the co-rotation stops in the region between 20 and 40 r J from Jupiter; This region corresponds to magnetisk, in which the field lines appear very developed in width. [29] The current that pours into the magnetisk originates in an area of \u200b\u200bthe ionosphere between 15 \u00b0 and 17 \u00b0 by the magnetic poles; The almost circular area thus described corresponds to the main auroral regions [30] (look down). The return current coming from the most external regions of the magnetosphere (over 50 R J ), penetrates the ionosphere to the poles, closing the electrical circuit; The total radial current of the planet magnetosphere has an estimated intensity on 60-140 million amp (a). [28] [thirty first] Another important current present in the magnetosphere of Jupiter, which reaches intensity of 160 million a, [3] It is the azimutal ring current, [32] which flows through the equatorial plasma in the same direction as the rotation of the planet. The strength of Lorentz which results from the interaction of this current with the magnetic field prevents co-crop plasma from chairing away from the planet. [3] [thirty first] In the Gioviana magnetosphere there are other minor currents: the widespread neutral current, which passes inside the widespread plasma in the same direction as the rotation of the planet; the tail currents, proper to the lobes of the magnetic tail, which move in the opposite direction to the rotation; The currents of the magnetopause (also called Chapman-Ferraro currents), which flow along the side exposed to the sun in the opposite direction to the rotation. All these currents contribute to preserving the configuration of the Gioviana magnetosphere by interacting substantially with the sun wind. [17] Plasma transfer [ change | Modifica Wikitesto ] The magnetosphere of Jupiter seen from the North Pole; Note the process of formation of plasmoids and the movement of plasma currents. The main problem encountered in deciphering the dynamics of the Gioviana magnetosphere concerns the transfer of the heavy cold plasma from the bull of I (at 6 r J from the planet) up to distances greater than 100 r J , in Piena Magnetosphere Song. [29] The exact mechanism is not yet known, but it is assumed that it is a result of the spread of plasma for intercaric instability. The process taken into consideration is very similar to the instability of Rayleigh-Taylor in hydrodynamics: [23] In the case of the Gioviana magnetosphere, the centrifugal force plays the same role played in the instability of the force of gravity; The heavy liquid is the cold and dense plasma of the Toroid, while the light liquid is the hottest and least dense plasma of the external magnetosphere. [23] The instability causes an exchange between the plasma flows full of plasma of the internal regions and those of the external regions of the magnetosphere: the “lively” empty flow pipes move towards the planet, removing the heavy pipes full of the plasma of I and to confine them in the external areas. [23] The intercaric exchange of flow pipes is a form of magnetospheric turbulence. [33] This hypothetical model was partially confirmed by the data of the Galileo probe, which identified the regions in which the density of the plasma was markedly reduced and others, inside the magnetosphere, in which the intensity of the field was higher than in the rest of the magnetosphere ; [23] These low density regions could correspond to the empty flow pipes arriving from the external magnetosphere. In the intermediate magnetosphere, the probe has identified so -called Injection events , which take place whenever the hot plasma of the external magnetosphere suddenly penetrates the magnetisk, causing an intense flow of energy particles and locally reinforcing the magnetic field. [34] The cold plasma transport mechanisms to external regions are not yet well known; However, it is assumed that when the flow of flow of the cold plasma of Io reach the external magnetosphere, they meet a reconnection process, which separates the magnetic field from the plasma. [29] These then return to the internal magnetosphere stuffed with the warm and not very dense plasma of the external regions, while the cold plasma is probably ejourished along the magnetic tail in the form of plasmoids (vast plasma bubbles). The reconnection processes would correspond to the global reconfiguration events observed by Galileo, which take place regularly every 2\u20133 days. [35] These events usually include rapid and chaotic variations of the intensity and the direction of the magnetic field, together with sudden changes in the motorcycle of the plasma, which with a certain frequency ceases to co-strot and begins to flow outwards. These phenomena were observed mainly on the night part of the magnetosphere, in correspondence with the albeggiant regions. [35] The reconnection events are analogous to the magnetic subtemptste of the Earth’s magnetosphere, [29] But they differentiate them for the causes. The terrestrial subtemptste are caused by the release, through an event of reconnection in the neutral plasma, of the energy of the solar wind stored in the magnetic tail, accompanied by the creation of a plasmoid that moves along the tail. [36] On the contrary, in the magnetosphere of Jupiter, these storms originate when the rotational energy, stored in the magnetisk, is released through the formation of a plasmoid that separates from the disc. [35] Polar Aurore [ change | Modifica Wikitesto ] A northern lights on Jupiter; You can see the main auroral oval, the polar emissions and the spots generated by the interactions with the magnetosfers of the Planet moons. Jupiter shows brilliant and persistent aurors on both poles. Unlike the terrestrial bumps, which are temporary and which are manifested above all in the periods of maximum solar activity, Jupiter’s auror are permanent, although their intensity is not constant, but various day by day. There are three main characteristics: the main oval, narrow (less than 1000 km) but brilliant circular areas placed about 16 \u00b0 by the magnetic poles; [37] the auroral spots of the satellites, which correspond to the “footprints” left by the lines of the magnetic field that connect their ionosfers with the ionosphere of the mother planet; The transient polar emissions, located within the main ovals. [37] [38] Although they have been analyzed in almost all the wavelengths (\u03bb) of the electromagnetic spectrum, including X -rays (up to 3 Kev), the auroral emissions appear far more bright in the average infrared (at \u03bb 3\u20134 \u00b5m e 7\u201314 \u00b5m) and in the distant ultraviolet (\u03bb 80\u2013180 nm). [39] The main oval are the predominant formation in the Aurore Gioviane; they have a very stable form and location, [38] But their intensity is strongly modulated by the pressure exerted by the solar wind: in fact, the more intense the sun wind, the weaker the ear. [40] As already mentioned before, the main ovals are fueled by the strong influx of electrons accelerated by the electric potential that is established between the plasma of the magnetisk and the Gioviana Ionosphere; [41] This current maintains the plasma of the magnetisk magnetisk in co-rotation with the planet. [29] Electrons have energies of the order of the 10\u2013100 Kev and penetrate deeply in the Gioviana atmosphere, ionizing and exciting molecular hydrogen and giving rise to an intense ultraviolet emission. [42] L’ERGIA TOTOE ACCUMULATA DALLA IONOSFERA AMMONTA A 10-100 TREATMENT (TW); [43] In addition, the currents that penetrate the ionosphere heat it by joule effect, which frees a quantity of energy, equal to 300 Two Two, responsible for the strong infrared emission of the aurore and, in part, of the heating of the planetary thermosphere. [44] Power emitted by the polar poles in different gangs of the electromagnetic spectrum [45] Emission Jupiter Macchia of me Radio (come,  1 km) are called GIOVIANA MILOMETRIC RADIATION O Kom; those with frequencies between 0.3 and 3 MHz (100      (adsbygoogle = window.adsbygoogle || []).push({});after-content-x4"},{"@context":"http:\/\/schema.org\/","@type":"BreadcrumbList","itemListElement":[{"@type":"ListItem","position":1,"item":{"@id":"https:\/\/wiki.edu.vn\/all2en\/wiki32\/#breadcrumbitem","name":"Enzyklop\u00e4die"}},{"@type":"ListItem","position":2,"item":{"@id":"https:\/\/wiki.edu.vn\/all2en\/wiki32\/magnetosphere-di-giove-wikipedia\/#breadcrumbitem","name":"Magnetosphere di Giove – Wikipedia"}}]}]