Earth - Educational facts and history of the planet Earth.
Earth
Earth is the third planet from the Sun and the fifth largest:
Planet Profile
mass : 5.972e24 kg
History of Earth
Earth is the only planet whose English name does not derive        from Greek/Roman mythology.        The name derives from Old English and Germanic.  There are, of course, hundreds        of other names for the planet in other languages .   In Roman Mythology, the goddess of the Earth was Tellus - the fertile soil (Greek: Gaia , terra mater - Mother Earth).
It was not until the time of Copernicus (the        sixteenth century) that it        was understood that the Earth is just another planet.
Earth, of course, can be studied without the aid of spacecraft.  Nevertheless        it was not        until the twentieth century that we had maps  of the entire planet.        Pictures of the planet taken from space are of considerable importance; for        example, they        are an enormous help in weather prediction and especially in tracking and        predicting hurricanes.         And they are extraordinarily beautiful.
The Earth is divided into several layers which have distinct chemical        and seismic properties (depths in km):
0-  40  Crust
2890-5150  Outer core
5150-6378  Inner core
The crust varies considerably in thickness, it is thinner under the oceans, thicker under the continents. The inner        core and crust are solid; the outer core and mantle layers are plastic or semi-fluid. The various layers are separated by discontinuities which are evident in seismic data; the best known of these is the Mohorovicic discontinuity between the crust and upper mantle.
Most of the mass of the Earth is in the mantle, most of the rest in the core; the part we inhabit is a tiny fraction of the whole (values below x10^24 kilograms):
atmosphere     = 0.0000051
outer core     = 1.835
inner core     = 0.09675
The core is probably composed mostly of iron (or nickel/iron) though       it is possible that some lighter elements may be present, too.        Temperatures at the center of the        core may be as high as 7500 K, hotter than the surface of the Sun . The lower mantle is probably mostly silicon, magnesium and oxygen with some        iron, calcium and aluminum.        The upper mantle is mostly olivene and pyroxene        (iron/magnesium silicates ),        calcium and aluminum.        We know most of this only from seismic techniques; samples from the upper mantle        arrive at the surface as lava from volcanoes but the majority of the Earth is        inaccessible.        The crust is primarily quartz (silicon dioxide) and other        silicates like feldspar. Taken as a whole, the Earth's chemical composition        (by mass) is:
34.6%  Iron
0.05% Titanium
The Earth is the densest major body in the        solar system.
The other terrestrial planets probably have similar structures and compositions with some differences: the Moon has at most a small core; Mercury has an extra large core        (relative to its diameter); the mantles of Mars and the Moon are much thicker;        the Moon and Mercury may not have chemically        distinct crusts; Earth may be the only one with distinct inner and outer cores.        Note, however, that our knowledge of planetary interiors is mostly theoretical        even for the Earth.
Unlike the other terrestrial planets,        Earth's crust is divided into several separate solid        plates which float around independently on top of the hot mantle below.        The theory that describes this is known as plate tectonics .        It is characterized by two major processes: spreading and subduction.  Spreading        occurs when two plates move away from each other and new crust is created by        upwelling magma from below. Subduction occurs when        two plates collide and the edge of one  dives        beneath the other and ends up being destroyed in the mantle.        There is also transverse motion at some plate boundaries (i.e. the San Andreas        Fault in California) and collisions between continental plates        (i.e. India/Eurasia).        There are (at present)  eight major plates:
North American Plate - North America, western North Atlantic and Greenland
South American Plate - South America and western South Atlantic
Antarctic Plate - Antarctica and the "Southern Ocean"
Eurasian Plate - eastern North Atlantic, Europe and Asia except for India
African Plate - Africa, eastern South Atlantic and western Indian Ocean
Indian-Australian Plate - India, Australia, New Zealand and        most of Indian Ocean
Nazca Plate - eastern Pacific Ocean adjacent to South America
Pacific Plate - most of the Pacific Ocean (and the southern coast of        California!)
There are also twenty or more small plates such as the Arabian, Cocos, and         Philippine Plates.  Earthquakes are much more common at the plate boundaries.        Plotting their locations makes it easy to see the plate boundaries.
The Earth's surface is very young .        In the relatively        short (by astronomical standards) period of 500,000,000 years or so        erosion and tectonic processes        destroy and recreate most of the Earth's        surface and thereby eliminate almost all traces of earlier        geologic surface history (such as impact craters).        Thus the very early history of the Earth has mostly been erased.        The Earth is 4.5 to 4.6 billion years old,        but the oldest known rocks are about        4 billion years old and rocks older than 3 billion years are rare.        The oldest fossils of living organisms are less than 3.9 billion years old.        There is no record of the critical period when life was first getting started.
71 Percent of the Earth's surface is covered with water.        Earth is the only planet on which water can exist in liquid form on the surface        (though there may be liquid ethane or methane on Titan's surface and liquid water beneath the surface        of Europa ).        Liquid water is, of course, essential for life as we know it.        The heat capacity of the oceans is also very important in keeping the Earth's        temperature relatively stable.  Liquid water is also responsible for most of the        erosion and weathering of the Earth's continents, a process unique in the solar        system today (though it may have occurred on Mars in the past).
The Earth's atmosphere is 77% nitrogen,        21% oxygen, with traces of        argon, carbon dioxide and water.        There was probably a very much larger amount of carbon dioxide in the        Earth's atmosphere when the Earth was first formed, but it has since been        almost all incorporated into carbonate rocks and to a lesser extent dissolved        into the oceans and consumed by living plants. Plate tectonics and biological        processes now        maintain a continual flow of carbon dioxide from the atmosphere to these        various "sinks" and back again. The tiny amount of carbon        dioxide resident in the atmosphere at any time is extremely        important to the maintenance of the Earth's surface temperature via the greenhouse effect .        The greenhouse effect raises the average surface temperature        about 35 degrees C above what it would otherwise be        (from a frigid -21 C to a comfortable +14 C); without it the oceans        would freeze and life as we know it would be impossible. (Water vapor is also an important greenhouse gas.)
The presence of free oxygen is quite remarkable from a chemical point of view.        Oxygen is a very reactive gas and under "normal" circumstances would quickly        combine with other elements.        The oxygen in Earth's atmosphere is produced and maintained by        biological processes.  Without life there would be no free oxygen.
The interaction of the Earth and the Moon slows the Earth's rotation by about 2 milliseconds per century. Current research indicates that about 900 million years ago there were 481 18-hour days in a year.
Earth has a modest magnetic field produced by electric currents in the outer core.       The interaction of the solar wind ,       the Earth's magnetic field        and the Earth's upper atmosphere causes the auroras (see the Interplanetary Medium ). Irregularities in these factors cause the magnetic poles to move and even reverse relative to the surface; the geomagnetic north  pole is currently located in northern Canada. (The "geomagnetic north pole" is the position on the Earth's surface directly above the south pole of the Earth's field.)
The Earth's magnetic field and its interaction with the solar wind also produce the Van Allen radiation belts, a pair of doughnut shaped rings of ionized gas (or plasma) trapped in orbit around the Earth. The outer belt stretches from 19,000 km in altitude to 41,000 km; the inner belt lies between 13,000 km and 7,600 km in altitude.
Earth's Satellite
Encyclopedia of the Atmospheric Environment
Open Issues
Our knowledge of the interior of the Earth is derived almost entirely from        highly indirect evidence.  How can we get more information?
How fast is Earth's core growing?
Despite substantial increases in the solar "constant" the average temperature        on the surface of the Earth has remained very stable for several billion years.        The best theory is that this has been accomplished by varying the amount of        carbon dioxide in the atmosphere to regulate the greenhouse effect .        But just how is this done?          The Gaia Hypothesis asserts that the        biosphere actively regulates it. More detailed information about Venus and Mars        may provide clues.
How much more carbon dioxide can we dump        into the Earth's atmosphere before it ends up like Venus?