Earth ... our home planet

Introduction to Earth

The Earth is the third planet from the Sun, and our home. Of all the planets in the Solar System, Earth is the ONLY one that harbors life, the ONLY one that holds water in three states of gas, liquid, and solid simultaneously, and the ONLY one in the so-called "habitable zone." We know more about the Earth than any other planet because we live here and have spent so many millennia studying is geology, zoology, botany, meteorology, and hydrology. So often we take this planet of our for granted. You go outside and see an endless horizon, huge forests and oceans, and seemingly limitless stores of energy reserves. Two significant events have forever altered mankind's view of this planet: Rachel Carson's book, "Silent Spring," which tells of the food chain accumulation of the insect spray DDT such that birds no longer were on this planet. Second was the photograph from the Apollo 8 mission which showed the Earth hanging over the Moon's horizon. Earth seemed so small and fragile against the vastness of space. Clearly, stewardship of this planet is a must for its inhabitants if we wish to leave a livable world to our children. With this concept of stewardship of Earth's limited resources in mind, we move into a study of this planet and the processes that shape our world.

Planetary data

Mass (kg), and mass relative to Earth

59.74x1023 kg = 1.0000 earths

Equatorial diameter (km)

12,756

Mean density (gm/cm3)

5.52

Acceleration of gravity (m/s2)

9.798

Velocity of escape (km/s)

11.2

Period of rotation

23.9345 hours

Period of revolution

365.25 days

Aphelion (AU)

1.0167

Aphelion (km)

152,100,000

Perihelion (AU)

.9833

Perihelion (km)

147,100,000

Mean orbital distance from the sun (AU)

1.0000

Mean orbital distance from the sun (km)

149,600,000

Orbital velocity (km/s)

29.79

Eccentricity

.0167

Oblateness

0.0034

Inclination to the ecliptic

0.000 degrees

Inclination of the equator to the orbit

23.44 degrees

Number of natural satellites

1

Names of natural satellites

Moon

More Information on the Planet Earth from the Nine Planets Website

Much of the information below is direct from the Nine Planets Website. Some material has been altered by me for this course, while other items and comments are directly copied. I hope to maintain a continuous update of this material to keep up with the findings from space satellites and telescopes.

Earth is the third planet from the Sun and the fifth largest:

orbit: 149,600,000 km (1.00 AU) from Sun
diameter: 12,756.3 km
mass: 5.972x1024 kg
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):

Name of Layer

Location Relative to Surface

Crust

0-40 km

Upper Mantle

40-400 km

Transition Region

400-650

Lower Mantle

650-2700 km

"D" :Layer

2700-2890 km

Outer Core

2890-5150 km

Inner Core

5150-6378 km

earth crust


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:

Earth Region

Mass (1024kg)

Atmosphere

0.0000051

Oceans

0.0014

Crust

0.026

Mantle

4.043

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:

Element

% Composition

Iron

34.6

Oxygen

29.5

Silicon

15.2

Magnesium

12.7

Nickel

2.4

Sulfur

1.9

Titanium

0.05


The Earth is the most dense 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 (right).


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 itself 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% 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.

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; see this diagram.)

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 - The Moon


Earth has only one natural satellite, the Moon. But thousands of small artificial satellites have also been placed in orbit around the Earth.
Asteroid 3753 (1986 TO) has a complicated orbital relationship with the Earth; it's not really a moon, but instead the term "companion" is used when describing it relative to our planet. It is somewhat similar to the situation with Saturn's moons Janus and Epimetheus for example.
Lilith, a hypothesized moon that is invisible to earth-bound people what thought to exist but has been proven to be absent. However, its story is interesting.

Some Quick Moon Facts

Distance from Earth

384,000 km

Radius

1738 km

Mass

7.35x1022 kg

Sidereal Period of Orbit

27.9 days

Synodic Period of Orbit

29.5 days

Below is a short list of links to information about the Earth::

Earth from NASA , Earth from Nine Planets, Earth from LANL, Earth from JPL, USGS

Geology

This page only serves to give you planetary data, which you will need for comparative purposes and the quiz later. You can now either return to Earth Introduction, the Syllabus, the Home Page, or better yet ... move forward to the Earth Structure lesson.


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