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Earth
Chandler Wobble

polar motion, a periodic rotation of the Earth’s spin axis about a mean axis, somewhat like the wobble of a spinning top. Slight variations in latitude and longitude result from this wobble because the poles are displaced from their mean positions. The north pole of rotation rotates counterclockwise around its mean position.

Polar motion is primarily made up of two discrete periodic oscillations: one, called the Chandler Wobble, has about a 14-month period, and the other has a 12-month period. The combination of these two wobbles causes the poles to trace spiral paths out of, around, and eventually back into their mean positions over a period of about 6.5 years. The separation between the actual and mean poles was exceptionally large in about 1952, when they were separated by 12 m (37 feet), or 0.37 arc second (0.37″). Their maximum separation during the 6.5-year period averages about 0.25″.

Polar motion was first predicted by the Swiss physicist Leonhard Euler in 1765 using dynamical theory and a rigid model of the Earth; he predicted a 10-month oscillation period for the phenomenon. Observational proof for the postulated latitude variations was obtained in the mid-1880s, and about that time the American astronomer S.C. Chandler analyzed these data and obtained both the 14-month and the 12-month periods. The four-month difference between Euler’s predicted period and the actual duration of the Chandler Wobble is due to the elasticity of the Earth’s mantle and the mobility of the oceans, which together subtly affect the Earth’s response to rotation and for which Euler had not provided in his calculations.

1 July 2002: The Solar and Heliospheric Observatory (SOHO) satellite reveals a massive solar eruption more than 30 times the Earth's diameter. The eruption formed when a loop of a magnetic field over the surface of the Sun trapped hot gas.
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Brightest Star in the Solar System

Astronomical observations of the Earth’s rotational position in space, which are used in determining Universal Time, must be corrected for slight variations in longitude caused by polar motion.

geomagnetic field

geophysics
Also known as: Earth’s magnetic field, geomagnetism, terrestrial magnetism

geomagnetic field, magnetic field associated with Earth. It is primarily dipolar (i.e., it has two poles, the geomagnetic North and South poles) on Earth’s surface. Away from the surface the dipole becomes distorted.

In the 1830s the German mathematician and astronomer Carl Friedrich Gauss studied Earth’s magnetic field and concluded that the principal dipolar component had its origin inside Earth instead of outside. He demonstrated that the dipolar component was a decreasing function inversely proportional to the square of Earth’s radius, a conclusion that led scientists to speculate on the origin of Earth’s magnetic field in terms of ferromagnetism (as in a gigantic bar magnet), various rotation theories, and various dynamo theories. Ferromagnetism and rotation theories generally are discredited—ferromagnetism because the Curie point (the temperature at which ferromagnetism is destroyed) is reached only 20 or so kilometres (about 12 miles) beneath the surface, and rotation theories because apparently no fundamental relation exists between mass in motion and an associated magnetic field. Most geomagneticians concern themselves with various dynamo theories, whereby a source of energy in the core of Earth causes a self-sustaining magnetic field.

Earth’s steady magnetic field is produced by many sources, both above and below the planet’s surface. From the core outward, these include the geomagnetic dynamo, crustal magnetization, the ionospheric dynamo, the ring current, the magnetopause current, the tail current, field-aligned currents, and auroral, or convective, electrojets. The geomagnetic dynamo is the most important source because, without the field it creates, the other sources would not exist. Not far above Earth’s surface the effect of other sources becomes as strong as or stronger than that of the geomagnetic dynamo. In the discussion that follows, each of these sources is considered and the respective causes explained.

Earth’s magnetic field is subject to variation on all timescales. Each of the major sources of the so-called steady field undergoes changes that produce transient variations, or disturbances. The main field has two major disturbances: quasiperiodic reversals and secular variation. The ionospheric dynamo is perturbed by seasonal and solar cycle changes as well as by solar and lunar tidal effects. The ring current responds to the solar wind (the ionized atmosphere of the Sun that expands outward into space and carries with it the solar magnetic field), growing in strength when appropriate solar wind conditions exist. Associated with the growth of the ring current is a second phenomenon, the magnetospheric substorm, which is most clearly seen in the aurora borealis. An entirely different type of magnetic variation is caused by magnetohydrodynamic (MHD) waves. These waves are sinusoidal variations in the electric and magnetic fields that are coupled to changes in particle density. They are the means by which information about changes in electric currents is transmitted, both within Earth’s core and in its surrounding environment of charged particles. Each of these sources of variation is also discussed separately below.

Observations of Earth’s magnetic field

Representation of the field

Electric and magnetic fields are produced by a fundamental property of matter, electric charge. Electric fields are created by charges at rest relative to an observer, whereas magnetic fields are produced by moving charges. The two fields are different aspects of the electromagnetic field, which is the force that causes electric charges to interact. The electric field, E, at any point around a distribution of charge is defined as the force per unit charge when a positive test charge is placed at that point. For point charges the electric field points radially away from a positive charge and toward a negative charge.

A magnetic field is generated by moving charges—i.e., an electric current. The magnetic induction, B, can be defined in a manner similar to E as proportional to the force per unit pole strength when a test magnetic pole is brought close to a source of magnetization. It is more common, however, to define it by the Lorentz-force equation. This equation states that the force felt by a charge q, moving with velocity v, is given by F = q(vxB).

In this equation bold characters indicate vectors (quantities that have both magnitude and direction) and nonbold characters denote scalar quantities such as B, the length of the vector B. The x indicates a cross product (i.e., a vector at right angles to both v and B, with length vB sin θ). Theta is the angle between the vectors v and B. (B is usually called the magnetic field in spite of the fact that this name is reserved for the quantity H, which is also used in studies of magnetic fields.) For a simple line current the field is cylindrical around the current. The sense of the field depends on the direction of the current, which is defined as the direction of motion of positive charges. The right-hand rule defines the direction of B by stating that it points in the direction of the fingers of the right hand when the thumb points in the direction of the current.

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In the International System of Units (SI) the electric field is measured in terms of the rate of change of potential, volts per metre (V/m). Magnetic fields are measured in units of tesla (T). The tesla is a large unit for geophysical observations, and a smaller unit, the nanotesla (nT; one nanotesla equals 10−9 tesla), is normally used. A nanotesla is equivalent to one gamma, a unit originally defined as 10−5 gauss, which is the unit of magnetic field in the centimetre-gram-second system. Both the gauss and the gamma are still frequently used in the literature on geomagnetism even though they are no longer standard units.

Both electric and magnetic fields are described by vectors, which can be represented in different coordinate systems, such as Cartesian, polar, and spherical. In a Cartesian system the vector is decomposed into three components corresponding to the projections of the vector on three mutually orthogonal axes that are usually labeled x, y, z. In polar coordinates the vector is typically described by the length of the vector in the x-y plane, its azimuth angle in this plane relative to the x axis, and a third Cartesian z component. In spherical coordinates the field is described by the length of the total field vector, the polar angle of this vector from the z axis, and the azimuth angle of the projection of the vector in the x-y plane. In studies of Earth’s magnetic field all three systems are used extensively.

The nomenclature employed in the study of geomagnetism for the various components of the vector field is summarized in the figure. B is the vector magnetic field, and F is the magnitude or length of B. X, Y, and Z are the three Cartesian components of the field, usually measured with respect to a geographic coordinate system. X is northward, Y is eastward, and, completing a right-handed system, Z is vertically down toward the centre of Earth. The magnitude of the field projected in the horizontal plane is called H. This projection makes an angle D (for declination) measured positive from the north to the east. The dip angle, I (for inclination), is the angle that the total field vector makes with respect to the horizontal plane and is positive for vectors below the plane. It is the complement of the usual polar angle of spherical coordinates. (Geographic and magnetic north coincide along the “agonic line.”)