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Magnetotail

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Magnetotail

File:Rattling Earth's Force Field.ogv

A magnetosphere is the area of space near an astronomical object in which charged particles are controlled by that object's magnetic field.[1][2] Near the surface of the object, the magnetic field lines resemble those of a magnetic dipole. Farther away from the surface, the field lines are significantly distorted by electric currents flowing in the plasma (e.g. in ionosphere or solar wind).[3][4] When speaking about the Earth, magnetosphere is typically used to refer to the outer layer of the ionosphere,[3] although some sources consider the ionosphere and magnetosphere to be separate.[2]

History

Study of the Earth's magnetosphere began in 1600, when William Gilbert discovered that the magnetic field on the surface of the earth was similar to that on a terrella, a small, magnetized sphere. In the 1940s, Walter M. Elsasser proposed the model of dynamo theory, which attributes the Earth's magnetic field to the motion of the Earth's iron outer core. Through the use of magnetometers, scientists were able to study the variations in the Earth's magnetic field as functions of both time and latitude and longitude. Beginning in the late 1940s, rockets were used to study cosmic rays. In 1958, Explorer 1, the first of the Explorer series of space missions, was launched to study the intensity of cosmic rays above the atmosphere and measure the fluctuations in this activity. This mission observed the existence of the Van Allen radiation belt (located in the inner region of the Earth's magnetosphere), with the Explorer 3 mission later that year definitively proving its existence. Also in 1958, Eugene Parker proposed the idea of the solar wind. In 1959, the term magnetosphere was proposed by Thomas Gold. The Explorer 12 mission in 1961 led to the observation by Cahill and Amazeen in 1963 of a sudden decrease in the strength of the magnetic field near the noon meridian, later named the magnetopause. In 1983, the International Cometary Explorer observed the magnetotail, or the distant magnetic field.[4]

Types of magnetospheres

The structure and behavior of magnetospheres is dependent on several variables: the type of astronomical object, the nature of sources of plasma and momentum, the period of the object's spin, the nature of the axis on which the object spins, the axis of the magnetic dipole, and the magnitude and direction of the velocity of the flow of solar wind.

The distance at which a planet can withstand the solar wind pressure is called the Chapman–Ferraro distance. This is modeled by a formula in which R_P represents the radius of the planet, B_{surf} represents the magnetic field on the surface of the planet at the equator, and V_{SW} represents the velocity of the solar wind.

R_{CF}=R_{P} \left( \frac{B_{surf}^2}{\mu_{0} \rho V_{SW}^2} \right) ^{\frac{1}{6}}

A magnetosphere is classified as "intrinsic" when R_{CF} \gg R_{P}, or when the primary opposition to the flow of solar wind is the magnetic field of the object. Mercury, Earth, Jupiter, Saturn, Uranus, and Neptune exhibit intrinsic magnetospheres. A magnetosphere is classified as "induced" when R_{CF} \ll R_P, or when the solar wind is not opposed by the object's magnetic field. In this case, the solar wind interacts with the atmosphere or ionosphere of the planet (or surface of the planet, if the planet has no atmosphere). Venus has an induced magnetic field. What this means is that since Venus appears to have no internal dynamo effect, the only magnetic field present is the one which is formed by the wrapping of the solar wind around the physical obstacle of Venus (see also Venus' Induced Magnetosphere). When R{CF} \approx R_P, the planet itself and its magnetic field both contribute. It is possible that Mars is of this type.[5]

Structure


Bow shock

Main article: Bow shock

The bow shock forms the outermost layer of the magnetosphere: the boundary between the magnetosphere and the ambient medium. For stars, this is usually the boundary between the stellar wind and interstellar medium; for planets, this is the boundary at which the speed of the solar wind drops abruptly as it approaches the magnetopause.[6]

Magnetosheath

Main article: Magnetosheath

The magnetosheath is the region of the magnetosphere between the bow shock and the magnetopause. It is formed mainly from shocked solar wind, though it contains a small amount of plasma from the magnetosphere.[7] It is an area exhibiting high particle energy flux, where the direction and magnitude of the magnetic field varies erratically. This is caused by the collection of solar wind gas that has effectively undergone thermalization. It acts as a cushion that transmits the pressure from the flow of the solar wind and the barrier of the magnetic field from the object.[4]

Magnetopause

Main article: Magnetopause

The magnetopause is the area of the magnetosphere in which the pressure from the planetary magnetic field is balanced with the pressure from the solar wind.[3] It is the convergence of the shocked solar wind from the magnetosheath with the magnetic field of the object and plasma from the magnetosphere. Because both sides of this convergence contain magnetized plasma, the interactions between them are very complex. The structure of the magnetopause depends upon the Mach number and beta of the plasma, as well as the magnetic field.[8] The magnetopause changes size and shape as the pressure from the solar wind fluctuates.[9]

Magnetotail

Opposite the compressed magnetic field is the magnetotail, where the magnetosphere extends far beyond the astronomical object. It contains two lobes, referred to as the northern and southern tail lobes. The northern tail lobe points towards the object and the southern tail lobe points away. The tail lobes are almost empty, with very few charged particles able to oppose the flow of the solar wind. The two lobes are separated by a plasma sheet, an area where the magnetic field is weaker and the density of charged particles is higher.[10]

Earth's magnetosphere


Over the Earth's equator, the magnetic field lines become almost horizontal, then return to connect back again at high latitudes. However, at high altitudes, the magnetic field is significantly distorted by the solar wind and its solar magnetic field. On the dayside of the Earth, the magnetic field is significantly compressed by the solar wind to a distance of approximately 65,000 kilometers (40,000 mi). The Earth's bow shock is about 17 kilometers (11 mi) thick[11] and located about 90,000 kilometers (56,000 mi) from the Earth.[12] The magnetopause exists at a distance of several hundred kilometers off the surface of the earth. The Earth's magnetopause has been compared to a sieve, as it allows particles from the solar wind to enter. Kelvin–Helmholtz instabilities occur when large swirls of plasma travel along the edge of the magnetosphere at a different velocity from the magnetosphere, causing the plasma to slip past. This results in magnetic reconnection, and as the magnetic field lines break and reconnect, solar wind particles are able to enter the magnetosphere.[13] On the nightside of the earth, the magnetic field extends in the magnetotail, which is over 6,300,000 kilometers (3,900,000 mi) in length.[3] The Earth's magnetotail is the primary source of the polar aurora.[10] Also, NASA scientists have suggested or "speculated" that the Earth's magnetotail can cause "dust storms" on the moon by creating a potential difference between the day side and the night side.[14]

Other objects

The magnetosphere of Jupiter is the largest planetary magnetosphere in the Solar System, extending up to 7,000,000 kilometers (4,300,000 mi) on the dayside and almost to the orbit of Saturn on the nightside.[15] Jupiter's magnetosphere is stronger than the Earth's by an order of magnitude, and its magnetic moment is approximately 18,000 times larger.[16]

See also

References

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