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At any location near the Earths surface, the magnetic field may be expressed as the vector sum of the contributions from three main sources: the main field generated in the Earths core, the crustal field from local rocks and a rapidly varying external field from currents flowing in the upper atmosphere and magnetosphere, which also induces currents in the sea and the ground.
The field generated in the Earths core accounts for most of the field observed at the Earths surface, and its strength and direction vary slowly with time. The strength varies from about 22000 nanoTeslas (nT) in South America to 67000 nT near Antarctica. It is generated by a convective dynamo operating in the Earth's fluid outer core, which surrounds the solid inner core. The convection is driven by both thermal and compositional buoyancy sources at the inner core boundary. These are produced as the Earth slowly cools and iron in the iron-rich fluid alloy solidifies onto the inner core giving off latent heat and the light constituent of the alloy. The buoyancy forces cause fluid to rise and the Coriolis force, due to the Earth's rotation, causes the fluid flows to be helical. It is thought that this fluid motion twists and shears magnetic field, generating new magnetic field to replace that which diffuses away. The field observed at the Earths surface approximates that of a dipole, currently tilted at about 10° to the axis of rotation of the Earth. However there are appreciable spatial departures from this simple model and they are best characterized at the Earths surface by a spherical harmonic series.
In contrast, the strength and direction of the crustal field may be regarded as essentially constant, only varying over geological timescales. Its strength is generally less than 200 nT but there are a few locations where much larger, highly localized, crustal fields exist. Aeromagnetic and marine magnetic surveys help map the geology as different rock types and formations have different magnetic signatures.
The strength of the external field variations depends mainly on latitude and at high latitudes during magnetic storms this may be more than 1000 nT on timescales of seconds to hours. The direction of the field may vary by a few degrees during such events.
Magnetic storms are caused by the interaction of the solar wind with the Earths magnetic field. The solar wind is a stream of charged particles continuously emitted by the Sun and its pressure on the Earth's magnetic field creates a bounded comet-shaped region surrounding the Earth called the magnetosphere. When there is a disturbance in the Earth-directed solar wind, often caused by activity associated with sunspots such as coronal mass ejections and coronal holes, the current systems inside the magnetosphere are enhanced and cause magnetic disturbances and storms. The transfer of energy from the solar wind to the magnetosphere through reconnection processes is greater when the magnetic field embedded in the solar wind is directed southward. High latitude current systems are enhanced as charged particles of solar origin are accelerated down the magnetic field lines. These energetic charged particles collide with atoms and molecules in the upper atmosphere, resulting in often spectacular light displays at high latitudes, the aurora.
Solar activity and the associated geomagnetic activity can cause considerable problems for certain kinds of technology, in particular satellites and Earth-based conductors such as power grids and pipelines. Space weather can affect satellites and satellite communications in a variety of ways, for example through radiation effects on digital chips, changes in atmospheric drag and ionospheric scintillation of signals. On the ground the rapid geomagnetic variations during magnetic storms can induce currents in power transmission grids and other ground-based conductors. They can also cause difficulties for specialized navigation such as directional drilling using geomagnetic field referencing.
The external field is also influenced by the direction of the Sun and this results in smaller and regular diurnal and seasonal variations. These variations are caused mainly by electrical currents in the upper atmosphere, peaking at altitudes around 110 km above the Earth's surface. The upper atmosphere is ionized by the Sun's ultraviolet and X-radiation to create the ionosphere, and the free ions and electrons are moved by winds and tides arising from the heating effects of the Sun and the gravitational pull of the Sun and the Moon. This creates the required conditions for a dynamo to operate, i.e. motion of a conductor in a magnetic field. Both the irregular and regular variations in the external field are affected by the approximately 11 year solar activity cycle.
In practice it is difficult to separate out these three main sources (core, crust and external) from observations of the geomagnetic field vector because of overlaps in the spatial and temporal frequency domains. However, if it is assumed that the region where observations are made is source-free, the magnetic field B is then the negative gradient of a scalar potential V which satisfies Laplaces equation . The scalar potential is the sum of the potentials from internal sources, Vi, and external sources, Ve. A solution to Laplace's equation for Vi is
where are radius, colatitude and longitude of the point of interest, a is the Earths reference radius, are the Gauss spherical harmonic coefficients of order m and degree n at time t, ni max is maximum degree of the spherical harmonic expansion for the internal potential Vi, and are the Schmidt semi-normalized Legendre polynomials of θ. B is described by the orthogonal components X (northerly intensity), Y (easterly intensity), and Z (vertical intensity, positive downwards), total intensity F, horizontal intensity H, inclination (or dip) I (the angle between the horizontal plane and the field vector, measured positive downwards), and declination (or magnetic variation) D (the horizontal angle between true north and the field vector, measured positive eastwards). The orthogonal components can be computed from the potential using the equations:
and D, I, H and F can be computed from the orthogonal components using the equations:
The Gauss coefficients constitute a spherical harmonic model of the Earths magnetic field and one such model is the World Magnetic Model. This model can be used to calculate current values of the magnetic field at any location and to produce global charts. Shown in Figures 1 and 2 are the charts of declination at 2012.5 and its annual rate of change. Magnetic field calculators and full sets of charts can be accessed at www.geomag.bgs.ac.uk.
Spherical harmonic models for the last 100 years or so are indicating that there is an overall weakening of the Earths magnetic field and that it is becoming less dipolar. This may have consequences for the trajectories of energetic charged particles that enter the Earths magnetosphere. One manifestation of this is the deepening, and westwards movement, of the South Atlantic Anomaly, a region where the Earths magnetic field is weaker than elsewhere (see Figure 3). Energetic charged particles are able to penetrate closer to the Earth and cause a radiation hazard for satellites passing through this region.
The input data for producing these global spherical harmonic models are observations collected around the world at observatories (of which there are currently about 160), networks of repeat stations and latterly, measurements from satellites. The distribution of observatories is largely determined by the location of habitable land and by the availability of local expertise, funds, and energy supply, and as result, it is uneven and a little sparse in some regions. Some observatories have had to move because of encroaching urbanization. Ground-based magnetic field observations are submitted to one of several World Data Centres.
Observations of declination in the UK have been made for over 400 years (Figure 4). Declination is the angle required to correct a magnetic compass bearing to a true bearing and in 1824 this was about 24° (blue/left-hand axis). Nowadays this angle is much smaller and is due to change sense in the UK for the first time since the 17th century. Since the 1860s when continuous observations at Greenwich became more reliable, several extremes in the rate of change of declination (pink/right-hand axis) have occurred, most prominently at around 1925, 1969 and 1978. These extremes are seen in other observatories around the world and are called geomagnetic jerks. Understanding their origin is important, not only because they result from interesting dynamical processes in the core and may help determine the conductivity of the mantle, but also for improving time-dependent models of the geomagnetic field and for the strictly practical purpose of forecasting its future behaviour for use in navigation with a magnetic compass.
International scientific campaigns such as the first International Polar Year in 1882/3, the second International Polar Year in 1932/3 and the International Geophysical Year in 1957/8 encouraged the opening of many observatories around the world. Geomagnetism is a cross-disciplinary science, and as a result, observatories are run by a wide variety of institutes whose interests range from geology, mapping, geophysics (including seismology and earthquake prediction), meteorology to solar-terrestrial physics and astronomy. Most observatories now run three sets of equipment: triaxial fluxgate systems making automatic non-absolute vector measurements, proton precession magnetometers making automatic absolute scalar measurements and fluxgate theodolites requiring manual operation to make absolute vector observations.
From the late 1950s to the 1970s a series of Russian and American satellites made magnetic field observations but it was not till 1979 that the first satellite made precise, oriented observations of the field. Magsat, an American mission, collected vector data for 7 months at altitudes up to 550 km. It was another 20 years till the next vector satellite surveys. The Danish-led mission Ørsted was launched in 1999 into a higher orbit than Magsat and returned vector data for over 5 years and scalar data for over 12 years. The German-led mission CHAMP was launched in 2000 into a lower orbit than Magsat and returned both vector and scalar data till 2010. Triaxial fluxgate and absolute total intensity magnetometers are placed on a boom to keep them remote from the magnetic effects of the main body of the satellite and accurate sensor orientation is achieved by star cameras. These satellites provide excellent global coverage of homogeneous data and it is expected that these surveys will be augmented with other satellite datasets such as those from the European satellite constellation, Swarm, due to be launched in 2012. With these magnetic survey satellites we are now able to map the Earths magnetic field to higher accuracy than ever before and to better understand its various sources
Campbell, W. H., 1997. Introduction to Geomagnetic Fields. Cambridge University Press.
Hulot, G., Balogh, A., Christensen, U. R., Constable, C., Mandea, M. and Olsen, N. (Eds), 2010.. Terrestrial Magnetism. Space Science Reviews, . Cambridge University Press.Volume 155, 1-4, Springer.
Jacobs, J. A., 1987. Geomagnetism Volumes 1, 2 and 3. Academic Press. [Volume 1: history of geomagnetism, instrumentation, overviews of main and crustal fields. Volume 2: origins of the Earth's magnetic field and that of the moon and other planets. Volume 3: rock magnetism, palaeomagnetism and the ancient magnetic field behaviour, conductivity structure of the Earth, indices of geomagnetic activity, magnetic field characteristics during solar quiet conditions.]
Jacobs, J. A., 1991. Geomagnetism Volume 4. Academic Press. [This volume covers the solar-terrestrial environment including the solar wind, the Earth's magnetosphere, magnetopause, magnetotail, ionosphere, pulsations, plasma waves, magnetospheric storms and sub-storms, auroras.]
Merrill, R. T., M. W. McElhinny and P. L. McFadden, 1996. The Magnetic Field of the Earth. Academic Press.
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