Geophysical Remote Sensing - Lecture Material - Completely Remote Sensing tutorial, GPS, and GIS -
Geophysical Remote Sensing

NOTE: Many of the ideas and examples presented on this and the following two pages require some background knowledge of the basics of Geology. If desired at this time, you can review a subsection in Section 2 that covers Fundamentals of Geology.

We begin this survey of Geophysical Remote Sensing with the first American triumph in space: the launch and operation of Explorer 1, on January 31, 1958, four months after the Soviet Union launched Sputnik I (see the Overview). The history-making launch of Explorer 1 riding on a Redstone-Jupiter C rocket is shown here:

The launch of Explorer 1 (small long object at very top) aboard a Redstone-Jupiter C rocket.

A good summary of this and several of the other early U.S. launches is found at this Explorer site.

Instead of the more conventional-looking satellites (most with thrusters to adjust their orbits) that we shall depict throughout this Tutorial, Explorer 1 itself was a small rocket with its own engine. It was thus actually the fourth stage of the rocket assembly. Here is a picture (against a black background to simulate the darkness of space) of Explorer 1:

The fourth stage of the first rocket to send an American payload - Explorer 1 - into Earth orbit.

This 4th stage was 2.03 m (6.67 ft) long and 15 cm (6 inches) wide. Its bottom contained fuel for getting the entire assembly into orbit. The payload - scientific instruments including a cosmic ray detector, micrometeorite package, and several temperature sensors - was mounted in the cross-lattice frame. The top was protected by a nose cone shroud. Once in orbit, this assembly rotated rapidly. Explorer 1 functioned successfully for 3 months until its batteries gave out.

Explorer 1 made a major discovery about the interaction between the Earth's geomagnetic field and incoming charged particles from the Sun and extra-solar space. A team headed by Dr. James Van Allen put together an instrument package centered on a Geiger counter suited to measuring variations in particle radiation. As it orbited, Explorer 1 repeatedly passed through a region in which the amount of radiation increased significantly. When Pioneer 3 was placed in a highly elliptical orbit in December 1958, it was determined that there were actually two peaks in counts as shown in this plot.

Plot of particle counts determined by the Pioneer 3 spacecraft.

These zones of increased intensity proved to be due to trapped particles held in the Earth's magnetic field. They were concentrated in two torus or doughnut-shaped zones that were named the Inner and Outer Van Allen Belts. This illustration is a two-dimensional cutaway sketch of streamlines representing solar wind particles as they passed through Earth's magnetic field.

The Van Allen Belts, in a 2-dimensional display.

The Inner V.A. Belt reaches its maximum intensity at 5000 km (3000 miles) but extends inward to about 1000 km (600 miles) The Outer Belt starts at 1500 km (9300 miles) and peaks at 22000 km (15500 miles). That belt is dominated by trapped electrons from the solar wind; the Inner Belt is marked by protons brought in mainly as cosmic rays. Two important conclusions from the discovery of the Van Allen Belts: 1) they have for eons provided protection to terrestrial surface dwellers from these potentially devastating particle bombardments - a fact critical to the successful development of life on Earth; and 2) both spacecraft and humans would need to be shielded effectively when passing through the Belts (as would astronauts journeying beyond Earth for extended periods).

In recent years, some spectacular images of the particle-trapping fields around the entire Earth have been taken by sensors on satellites placed in highly elliptical orbits or at Lagrangian points (where Earth-Sun gravitational forces balance out) or enroute to the Sun or other distant bodies. In the top image, the Earth's radiation field in the excited atmosphere is seen in the Extreme Ultraviolet (EUV) part of the spectrum by the IMAGE (Imager for Magnetopause to Aurora Global Exploration) satellite; the shape of this field is determined largely by the Earth's magnetic field (note the trailing pattern, related to the geomagnetic tail [see below]). The arc-shaped inner belt is now called the plasmasphere. The distribution of the trapped solar particles in this image is strongly controlled by the Earth's magnetosphere (see below).

IMAGE EUV image of the Earth's environs, as partly controlled by its magnetic field.

The Van Allen Belts become much weaker above 75°N and 75°S. This allows more particles to reach the the upper atmosphere and collide with oxygen, nitrogen and argon atoms in the air to generate ions that in their excited states give off constantly moving, colorful, wavy displays known as the Aurora Borealis in the northern hemisphere and the Aurora Australis in the southern hemisphere. This geophysical phenomenon occurs mainly at the higher latitudes but sometimes extends below 40°; it is seen most frequently around 70° latitudes. The image below shows the aurora as photographed on the ground in Colorado.

The Northern Lights, seen from the ground; the green color associates with excited oxygen, the red with nitrogen.

A similar scene appears below, along with a panel of images showing the influence of modes of excitation:

Ground view of the northern lights.
Modes of excitation affecting the colors of the Aurora Borealis.

Here is a view of the Aurora Borealis as taken by astronauts on the Space Shuttle.

Photograph of the Aurora Borealis display as seen from the Space Shuttle (Mission STS-47).

The auroras can occur simultaneously in both the northern and southern hemispheres, as depicted in this image from IMAGE at a distance of 7.2 earth radii.

The high latitude auroras seen from space, showing their true scale sizes relative to Earth.

A superb aurora occurred over North America on November 7 and 8, 2004. Here is a ground scene of that event and a view from space in which the military DMSP satellite captured this aurora as a white band across the northern U.S.-southern Canada.

Ground view of Aurora Borealis on November 7, 2004
Defense Mapping Satellite Program image of the above aurora on November 8, 2004.

The High Energy Neutral Atom instrument on IMAGE sends back images of auroras like this one, from which intensity variations can be extracted:

HENA image of the Earth's environs.
Colorized intensity variations in neutral atom excitation, as measured by IMAGE's HENA instrument.

An example of symbiosis in remote sensing is this: A satellite named SOHO whose job is to monitor solar activity reported intense solar storms in mid-July. This was predicted to produce a spectacular Aurora Borealis flare-up visible as far south as the northern U.S. Unfavorable viewing conditions caused rather subdued displays. But, a NASA satellite called Polar (launched in 1996) designed to monitor just such phenomena produced this view in the visible from space:

The Aurora Borealis activated by a solar storm; this visible image was made on July 15, 2000 by the Polar satellite; note the arctic islands and landmasses, with Greenland being the largest.

Other excitations produce displays seen in the Ultraviolet. Here is an IMAGE EUV view of excited helium extending well out beyond the Earth's atmosphere:

Helium plasma excitation beyond the bulk of Earth's atmosphere.

Many satellites have been placed in space by various nations to get global scale data on the Earth's magnetosphere and its ionosphere (a globe-circling band located largely between 80-400 km [50-250 miles] above the surface, containing electrons stripped by gamma rays from nitrogen and oxygen). Here is a plot of the global distribution of the ionosphere, measured by the Jason-1 satellite (pages 8-7 and 14-12) whose prime mission is to measure Sea Surface Heights.

Variations in the ionosphere (maximum in the Tropics) as measured by Jason-1.

To better understand both the solar influence on that part of the (thin) atmosphere and the possible feedback influence of Man, more integrated data on the Mesosphere and lower Thermosphere/Ionosphere, between 40 and 110 miles (60-180 km), has been sought through the launch on December 7, 2003 of the TIMED (Thermosphere-Ionosphere-Mesosphere-Energetics-Dynamics) satellite. TIMED carries four sensors designed to measure different properties in this zone. This diagram shows its general role and objectives as it orbits at 338 miles (624 km) above Earth. Data have not yet been released for inspection by the public.

Schematic showing the TIMED operations.

Other satellites have made countless measurements and observations of the inner atmosphere (about 97% by mass of its gases [about 78% N2, 21% O2, 0.93% A(rgon), 0.35% CO2]). The atmosphere tends to be homogeneous (mixed uniformly) within the bottom (near surface) 30 km (18 miles). The upper thin atmosphere extends out to about 120 km (75 miles). At greater distances outward the gases separate into shells (the heterosphere) with the innermost being molecular nitrogen, then atomic oxygen, then atomic helium, and a thick (from 3500-10000 km [2200-6000 miles]) outermost layer of atomic hydrogen. (See Section 14 for a fuller treatment of meteorological remote sensing of the lower atmosphere.)

Much was learned about the Earth's natural environment above its surface - both in regards to the nature and distribution of particles and fields and to the various atmospheric zones - in the first decade of the space program. Of special note is the OGO (Orbiting Geophysical Observatory) series, of which 6 were launched in the 1960s. Three of these have nearly polar orbits and are referred to as POGOs.

Satellites have been the main tool for measuring the terrestrial geopotential fields at global scales. This includes such physical properties as regional magnetic and gravity variations or anomalies originating within the solid Earth but expressed at the surface. In particular, such properties are more difficult to measure under the oceans but data derived from satellites provide the means to determine the distribution of magnetic and gravity differences over large tracts of marine seafloor. The magnetic field varies over time but the gravity field is almost completely time invariant.

The Earth's dipolar geomagnetic field (first examined scientifically by W. Gilbert in 1600) results from slow motions in its fluid Outer Core (the Inner Core is very hot, under extreme pressure, but solid). The movement is powered by the Earth's rotation and by thermal gradients. Detached electrons from the Iron-Nickel core material produce electric currents that through the dynamo effect generate the magnetic field (which can be depicted by lines of force) that presently emanates from the Earth's South to its North magnetic poles. (This phenomenon of magnetic field generation was discovered by H.C. Oersted in 1819 quite serendipitously during a demonstration of electric currents to his students; the needle of a compass lying nearby moved when the current flowed, from which he deduced this cause-effect relation.)

The geomagnetic field (derivative from the lines of force data) is composed of three parts: 1) the Main Field, caused by the internal processes in the core, which accounts for more than 95% of the total field strength; 2) the External Field, resulting from processes in the ionosphere leading to a superimposed field; and 3) the Anomalous Induced Field, caused by induced (secondary) magnetism generated in iron minerals (such as magnetite and hematite) found mainly in the crust. Including in the induced field are those substances that have an inherited remanent (permanently induced) magnetism; these give rise to local variations called anomalies that tell geophysicists and prospectors about localized to regional concentrations of certain rock types and possible commercial minerals. The geomagnetic field strength is commonly plotted in intensity units. The basic unit is the oersted (1 dyne per unit pole), which is numerically equivalent to the gauss, the preferred term when magnetic induction is measured. A derivative unit is the γ, which is 10-5 gauss. In the SI units system, intensity is measured in Teslas (defined in units of Newtons/Ampere-meter) or more commonly nanoTeslas (nT; 10-9 Teslas); an nT is the equivalent of the γ in strength.

Although more complicated in its details, the Earth's geomagnetic field can be likened to that associated with a simple, straight bar magnet, as pictured thusly:

Sketch showing part of the Earth's dipolar magnetic field as depicted by the lines of magnetic force.

This pattern of symmetrical lines of force (the magnetic flux) is idealized to describe the concept. Actually, the main geomagnetic field is much distorted by interaction with the solar wind (a plasma of mostly charged particles spewed out from the Sun and driven outward at high speeds) which exerts a "pressure" on the field compressing it on the side facing the Sun and drawing it out in a streamlined elongation away from the Sun. In two dimensions, the modified field appears like this, as determined from satellite measurements:

The distorted magnetosphere surrounding Earth.

The region around Earth in which the terrestrial magnetic field is enclosed by the solar wind is termed the geomagnetic cavity. The outer cavity is bound by the magnetopause. Where the solar wind encounters the magnetosphere on the Sun-facing side, a magnetohydrodynamic bow shock wave is produced as much of the solar wind is deflected around the magnetopause. On that side, the region between the bow shock front and the magnetopause is called the magnetosheath. Behind the Earth, on its nightside, the magnetic lines of force are stretched out into the magnetic tail which extends for well over 150,000 km (about 100,000 miles).

Note that the magnetic pole and the Earth's rotational pole are currently about 11° apart. Both poles wander (precess) so that this angle changes with time. The angle between true North and magnetic north, or between the geographic and magnetic meridians, is called the magnetic declination. The angle between the path of a magnetic line of force at some latitude and the horizontal (Earth's flat surface) is the magnetic inclination (it can be determined locally with a magnetic dip needle [held vertically]). The angle is zero at the magnetic equator (field line parallel to the surface, 90° at the poles, and at intermediate angles between these two reference positions. Both declination and inclination shift globally or in a region over time; long-period variations in direction and intensity are called secular changes. This effect is shown here for nearly four centuries of ground-based data from Great Britain:

Shifts in magnetic declination and inclination measured since 1500 AD in Great Britain.

Variations in magnetic inclination, declination, total intensity, and horizontal and vertical intensity vectors can be determined from ground and space measurements. Over the years, these have become part of the geomagnetic community's data base called the International Geomagnetic Reference Field (IGRF), now updated every four years. Here is a global plot of the general geospatial distribution of magnetic inclination values for 1995.

Worldwide variations in magnetic inclination for the year 1995.

The total magnetic field as determined by satellite measurements can be shown in this global diagram, with the solid black lines representing intensity values and the dashed lines denoting typical annual variations, both plotted in units of nanoTeslas (nT).

Plot of generalized global distribution of the Earth's magnetic field and its annual variations.

The geomagnetic measurements have confirmed and refined our knowledge of the magnitudes and distribution of global intensities. These range from about 25000 nT at the equator to 65000 nT at the poles (or from 0.25 to 0.65 gauss). This next illustration is a general depiction of this variation (low values in blue; high in red):

Global geomagnetic intensity variations.

The secular variation in intensity can be as much as 150 nT per year. Here is a global map of cumulate changes during the years 1925-27 as determined from many ground stations:

Secular variations in the total intensity of the geomagnetic field integrated through the years 1925-1927.

Geomagnetic measurements were among the first geophysical data acquired by early American satellites such as several Explorers, Pioneer I and V, IMP-I, and the OGO series and by such Russian satellites as the first two in the Lunik series that also went to the Moon. A major advance in surveying geomagnetic anomalies was made by Magsat, launched in 1979. Although data collection was short-lived owing to the limited duration of the mission which ended in June 1980, the spacecraft operated long enough to provide an invaluable set of measurements still being examined 20 years later. Here, for example, is a 1995-produced map of variations in intensity over most of Australia.

Map of geomagnetic intensity variations over Australia, using Magsat data.

When produced as color-coded maps, Magsat-determined intensity variations are impressive in their detail. This map was made to cover the North polar region:

Magsat intensity anomalies in the polar region of Earth's northern hemisphere.

Major anomalies worldwide were identified by Magsat. This next map shows significant anomalies (in nT, ranging from -12 in blue to +12 in pink) plotted on a topographic/bathymetric base as a gray background with some first order surface features superimposed. One of particular interest is the Central African Anomaly (blue area low just above the red area high in the middle of Africa).

Magnetic anomalies (in nT) of large sizes on a world map; produced by Purucker.

Since the Magsat benchmark mission, other satellites have, or will be, orbited to monitor and improve the geomagnetic properties measured conveniently from space. These include POGS (Polar Orbiting Geomagnetic Survey) in 1990, Oersted (a Danish mission; 1999), Champ (German; 2000), and SAC-C (Argentina; 2000). Champ, as an example, makes both magnetic and gravity (acceleration) measurements:

Magnetic and gravity measurements made by the polar-orbiting CHAMP satellite.

We would be remiss if the essential results of years of paleomagnetic studies were not included here. While satellite data support this work, they are not the prime means by which knowledge of the history of changes in the Earth's magnetic field is obtained. This has been done mainly through ground sampling of rocks collected on the continents or from the oceans' floor. This approach is not remote sensing in strictu senso but it does lead to reconstruction of magnetic field geometry at global scales that assumed different orientations in the past. And, it provides an "excuse" to introduce into this Tutorial a review of the now fully accepted paradigm called Plate Tectonics which dominates models of the Earth's geologic history and modes of operation. That will serve as background for remote sensing topics covered in several Sections dealing largely with geologic applications. (Plate Tectonics is also considered in the 'Geology Tutorial' on page 2-1a that should be looked at now if you are unfamiliar with the concept.)

The basis underlying paleomagnetism is the discovery that the magnetic field shifts its polarity with a rather irregular periodicity over tens to hundreds of thousands of years. Thus today's North geomagnetic pole (in which the magnetic lines of force enter Earth from space) has been a South pole (from which the lines emerge) many times in the past. This switching back and forth of the N and S magnetic poles relative to Earth's North rotational pole is termed magnetic reversal. When the two North's coincide, the present-day polarity is arbitrarily said to be normal; when the South magnetic pole is located near the North rotational pole, polarity is reverse. It is possible to determine polarity at a given time in the past (as determined by radiometric dating) by measuring the polarity of a rock sample containing ferromagnetic mineral(s). Magnetite, Fe3O4, is most frequently used. Magnetite is one of the first accessory minerals to crystallize in a basaltic magma/lava. As the magma temperature drops through 580° C, magnetite passes through the Curie point, at which it takes on its magnetic orientation, becoming like a dipolar "needle". During continued cooling, magnetite grains will orient their N-S polar axis, much like a compass, such that the north pole of a crystal will align with the lines of force and will point to where the geomagnetic North pole was at the time when the crystal was "frozen" in place as the magma solidified. The process by which this occurs is called thermoremanent magnetism.

The application is this: Continental basalts (and sometimes sedimentary rocks) containing magnetite are sampled at the place being studied, usually by coring, with the core's spatial position established by fixing its three-dimensional orientation. The (radiometrically dated) sample is then examined in the laboratory for its "fossilized" magnetic orientation (referenced to its internal field position). This determines the alignment (direction and inclination) of the permanent magnetic field imposed on the magnetite before rock consolidation at the time well into the past when the lava was extruded or sediment deposited. After the sample is placed in context with its 3-D orientation, this paleomagnetic field geometry will point to some position on the Earth (relative to today's geography) that represented an apparent location of the poles at the time of the rock's age. Furthermore, the polarity (normal or reversed) could also be determined. The same technique, and resulting information, has been applied to oriented basaltic rocks beneath ocean floor sediments that were retrieved by submarine core drilling. Two major discoveries, vital to developing the concepts of plate tectonics and continental drift, gradually emerged through the 1960s to the present.

The first is sea floor spreading. Through deeper parts of the several ocean basins, volcanic upwelling has built long, relatively narrow rises or ridges which today are sites of active marine volcanism. Lavas emerging today take on the normal polarity that has persisted over the last 700,000 years. When recovered as cores, the solid basalts have magnetic orientations consistent with modern pole locations. But, as sampling moves away laterally from the ridges, the basalts become progressively older. When their polarities are determined, a pattern of alternating polarities (normal-reverse-normal-reverse-normal.....) emerges. Actually, this pattern was initially determined by geomagnetic surveys using magnetometers towed behind ships. Even more remarkably, the pattern on one side of the ridge is matched by a pattern on the opposite side. This diagram should help to visualize the observation (black is normal polarity; white is reverse):

Cross-section through the Mid-Atlantic Ridge, showing patterns of changing magnetic polarities; adapted from Vine and Matthews.

The figure shows normal-reverse patterns for the last 9 million years (horizontal top scale). The current and the three most recent preceding magnetic epochs are named. Average rates of plate movement are shown by arrows. The N-R patterns are repeated in samples from all the oceans, so that the polarity shifts are clearly global in effect. These distinctive patterns form the basis of a geomagnetic age dating method that has been proven to work well. There is enough variation and uniqueness in the patterns (each, a "fingerprint" showing some distinctive repeated normal-reverse sequence) to allow suites of rocks formed over a span of several million years or so to be singled out and separated and then mapped according to the age of each. This magnetochronology has been carried back into the Cretaceous Period some 100+ million years ago.

Enough radiometric ages collected at many locations within the sea floors of the different named oceans have been determined to allow maps of relative age based on the polarity change sequence to be produced for the entire globe. Here is one in which the youngest ages are in red and oldest in blue (thus the blue regions were formed first and have been driven away from the ridges towards plate boundaries). It follows from the defining age determinations that the seafloor is everywhere relatively young inasmuch as older basaltic units at sea floors of pre-Cretaceous age have been completely or largely destroyed by subduction (see below):

As the ages of basalt lavas were determined, and it became evident that the extruded lavas became progressively older moving towards continental land masses on either side of the ridge, a mechanism to explain these patterns was proposed independently by H. Hess of Princeton University and R. Dietz of NOAA (who was actually first, but whose seminal paper was held up by incredulous reviewers; personal comm.). Sea floor spreading postulates that lavas from the oceanic crust or mantle rise to the surface at the ridge, pour out, and push laterally against two lithospheric plates (oceanic crust plus the top of the Upper Mantle) on either side. This acts more or less continuously for long times. The plates slide along the asthenosphere (region of the Upper Mantle hot enough for the rocks to act as though viscous (i.e., "taffy" soft material), moving in a motion likened to a conveyor belt until they encounter a boundary with another plate. (There are 7 major plates and a larger number of smaller plates; see page I-1c of this Introduction or the top of page 17-3 for a global map of these plates). Several different responses are possible at these boundaries, as shown in this next diagram which summarizes much of the main idea behind plate tectonics.

Schematic diagram summarizing the (generally accepted) theory of plate tectonics
From Tarbuck and Lutgens, The Earth, 3rd Ed., 1990, Merrill Publ.

A Mid-Ocean ridge appears at the left divergent boundary, from which lithospheric plates move in opposite directions. The ridge is cut by a number of transform faults which break the plate into segments. A series of slight rises are evident. Each may be associated with a set of magnetic reversals. At the far left is one type of convergent boundary - where two oceanic plates approach each other. One plate is driven downward (subduction) beneath the other into the mantle, gradually melting as it gets deeper. Some of the molten rock reaches the surface to form a chain of volcanic islands (and sediment) called an Island Arc (Indonesia is an example). The right moving plate moves against a convergent boundary located at/near the edge of an embedded continental assemblage of rocks on its own plate. Above its subduction zone, melted rock and tectonic upwelling and compression produce folded sedimentary rocks and volcanic and plutonic (magmas that intrude rocks above but don't reach the surface) rocks to form one or more mountain chains (the Coast Ranges and Sierra Nevada/Cascades along the western part of the U.S. are an example). In this idealized diagram, the continent-bearing plate is shown as splitting along a rift zone formed along another type of divergent boundary. The plate to its right is moving against another plate that has a second continent in its crustal portion; again mountains are developed by folding, faulting, and intrusion (the Himalayas against the Indian subcontinent are an example).

One might wonder about the mass balance associated with the plate movements. As a plate is heated up during subduction, it (at least partially) melts. Some of that now fluidized material is moved laterally back towards one or more spreading ridges. Thus, a closed cycle of moving rock and magma results. The process at a ridge is aided by 1-2 sets of circulating convection currents in the Mantle which provide the energy to power the cycle. Possibly some convection occurs above the crust-mantle boundary (the so-called Moho, abbreviated from its discover's difficultly pronounced name, the Yugoslavian seismologist A. Mohorovicik [Mo-ho-ro-vitch-ick]) and may couple with the drag applied by the upper convective movements that affect a lithospheric plate from below.

Now to the second discovery: Polar Wandering. When oriented rock samples of a given age are analyzed to determine where their magnetic components are pointing to the location of the magnetic pole on the Earth's sphere at the time of their formation, rocks of different ages are found to have polar field entry locations N Poles) in notably different parts of the present-day world (its geography today is the reference state). One might surmise from the geographic spread that results that the magnetic poles have wandered over much of the globe relative to its rotational poles. This next figure shows plots of magnetic pole positions on a modern geographic grid (latitude-longitude) for the northern hemisphere, with the age of the rocks involved shown by letters (denoting geologic time from oldest to youngest: Ca = Cambrian; S = Silurian; D = Devonian; C = Carboniferous; P = Permian; T = Triassic; J = Jurassic; K = Cretaceous; E = Eocene). For a table showing the geologic time scale, with assigned ages, click here).

Polar wandering plots for north pole data obtained on two continents from the beginning of the Paleozoic to the Present.
From H. Levin, The Earth Through Time, 4th Ed., Saunders

At first glance, this map seems to display a puzzling anomaly: how can now far apart continents record two sets of pole locations when at present we know that only one pole point is the norm. The poles seemingly occupied different positions from the Paleozoic onward until the Present (and still other positions in the Precambrian). One might surmise that the poles were indeed in different locations on the Earth's surface at various times in the past, but that would be hard to explain since the magnetic poles apparently have always been close to the rotational poles owing to the mechanism of magnetic field generation that assumes the electrical currents in the Outer Core move generally subparallel to the Equator. Thus, it's odd indeed to have two sets of pole patterns in North America and Europe, moving approximately along similar paths, but separated (offset) from each other.

The answer to this duality conundrum is tied to the concept of continental drift . At various times in the past, the continents did not have their present shapes (their "true" edges are just beyond their sealevel outlines) or relative positions. In fact, today's continental crustal masses have been once joined into two supercontinents (derived from the Late Paleozoic megacontinent Pangaea, which has since split into Gondwana and Laurasia, each of which then divided further into the present-day continents). As a supercontinent comes apart, its new pieces move across the globe embedded in wandering crustal plates. Pangaea itself resulted from collisions of plates bearing earlier continental masses which were welded together, only to then resplit later; evidence suggests there were similar large supercontinents of different shapes/sizes and locations during Early Paleozoic and Precambrian times.

If the North American and Euro-Asian continents were relocated on the terrestrial globe back to their Early Paleozoic positions, the two curves in the above figure will almost superimpose. This is strong proof of the drift hypothesis. Thus, since these continents were then conjoined, their pole locations were the same but have now moved apart because their continents have separated, so that in today's geography the wandering paths seem to be recording two different pole location histories. Their intermediate pole positions help to locate their different relative locations at each indicated time.

As a transition to a topic - gravity - covered in the next page, we show now a summary of recently orbited and planned magnetic and gravity measuring satellites for the first decade of the 21st Century:

Satellites expected to be operating in the first 10 years of the 21st Century to gather magnetic and gravity data for the whole Earth and for large regions.

Information on CHAMP and COSMIC, now both in orbit, is available by clicking on these links to the Internet.