Earth's gravity, denoted by g, refers to the gravitational attraction that the Earth exerts on objects on or near its surface. Its strength is usually quoted in terms of the acceleration it gives to falling bodies (acceleration due to gravity), which in SI units is measured in m/s² (metres per second per second, equivalently written as m·s−2 or N/kg). It has an approximate value of 9.8 m/s², which means that, ignoring air resistance, the speed of an object falling freely near the Earth's surface increases by about 9.8 metres per second every second.
The precise strength of the Earth's gravity varies depending on location. The nominal "average" value at the Earth's surface, known as is, by definition, 9.80665 m/s² (32.1740 ft/s²). This quantity is denoted variously as gn, ge (though this sometimes means the normal equatorial value on Earth, 9.78033 m/s²), g0, gee, or simply g (which is also used for the variable local value). The symbol g should not be confused with G, the gravitational constant, or g, the abbreviation for gram (which is not italicized).
Apparent gravity is weaker at lower latitudes (nearer the equator), for two reasons. The first is that the surface of the Earth is not an inertial frame of reference: a centripetal force is required to keep objects on the surface moving in a circular path around the Earth's axis as the Earth rotates. In providing this centripetal force, some of the gravitational force on an object is "used up" leaving less to contribute to the object's weight. The apparent force due to rotation is called the centrifugal force; on the surface of the Earth, it depends on an object's mass and its latitude (it's zero at the poles and largest at the equator) so it is customarily combined with the Newtonian gravity. Thus, the local gravity, g, is not purely the result of gravitational force, but is actually effective gravity, a combination of true gravity and centrifugal force. It is effective gravity that you measure when you step on a scale or hang a plumb bob. This effect on its own would result in a range of values of g from 9.789 m·s−2 at the equator to 9.832 m·s−2 at the poles.
The second reason is that the Earth's equatorial bulge (itself also caused by centrifugal force) causes objects at the equator to be farther from the planet's centre than objects at the poles. Because the force due to gravitational attraction between two bodies (the Earth and the object being weighed) varies inversely with the square of the distance between them, objects at the equator experience a weaker gravitational pull than objects at the poles.
In combination, the equatorial bulge and the effects of centrifugal force mean that sea-level gravitational acceleration increases from about 9.780 m·s-2 at the equator to about 9.832 m·s-2 at the poles, so an object will weigh about 0.5% more at the poles than at the equator.
The same two factors influence the direction of the effective gravity. Anywhere on Earth away from the equator or poles, effective gravity points not exactly toward the center of the Earth, but rather perpendicular to the surface of the geoid, which, due to the flattened shape of the Earth, is somewhat toward the opposite pole. About half of the deflection is due to centrifugal force, and half because the extra mass around the equator causes a change in the direction of the true gravitational force relative to what it would be on a spherical Earth.
Gravity decreases with altitude, since greater altitude means greater distance from the Earth's centre. All other things being equal, an increase in altitude from sea level to the top of Mount Everest (8,850 metres) causes a weight decrease of about 0.28%. (An additional factor affecting apparent weight is the decrease in air density at altitude, which lessens an object's buoyancy.) It is a common misconception that astronauts in orbit are weightless because they have flown high enough to "escape" the Earth's gravity. In fact, at an altitude of 400 kilometres (250 miles), equivalent to a typical orbit of the Space Shuttle, gravity is still nearly 90% as strong as at the Earth's surface, and weightlessness actually occurs because orbiting objects are in free-fall.
If the Earth were of perfectly uniform composition, during a descent to the centre of the Earth, gravity would decrease linearly with distance, reaching zero at the centre. In reality, the gravitational field peaks within the Earth at the core-mantle boundary where it has a value of 10.7 m/s², because of the marked increase in density at that boundary.
Local variations in topography (such as the presence of mountains) and geology (such as the density of rocks in the vicinity) cause fluctuations in the Earth's gravitational field, known as gravitational anomalies. Some of these anomalies can be very extensive, resulting in bulges in sea level, and throwing pendulum clocks out of synchronisation.
The study of these anomalies forms the basis of gravitational geophysics. The fluctuations are measured with highly sensitive gravimeters, the effect of topography and other known factors is subtracted, and from the resulting data conclusions are drawn. Such techniques are now used by prospectors to find oil and mineral deposits. Denser rocks (often containing mineral ores) cause higher than normal local gravitational fields on the Earth's surface. Less dense sedimentary rocks cause the opposite. Paris, France has been shown by this method to almost certainly be sitting on a huge, untouchable oilfield .
In air, objects experience a supporting buoyancy force which reduces the apparent strength of gravity (as measured by an object's weight). The magnitude of the effect depends on air density (and hence air pressure); see Apparent weight for details.
The gravitational effects of the Moon and the Sun (also the cause of the tides) have a very small effect on the apparent strength of Earth's gravity, depending on their relative positions; typical variations are 2 µm/s² (0.2 mGal) over the course of a day.
|Amsterdam||9.813 m/s²||Istanbul||9.808 m/s²||Paris||9.809 m/s²|
|Athens||9.807 m/s²||Havana||9.788 m/s²||Rio de Janeiro||9.788 m/s²|
|Auckland, NZ||9.799 m/s²||Helsinki||9.819 m/s²||Rome||9.803 m/s²|
|Bangkok||9.783 m/s²||Kuwait||9.793 m/s²||San Francisco||9.800 m/s²|
|Brussels||9.811 m/s²||Lisbon||9.801 m/s²||Singapore||9.781 m/s²|
|Buenos Aires||9.797 m/s²||London||9.812 m/s²||Stockholm||9.818 m/s²|
|Calcutta||9.788 m/s²||Los Angeles||9.796 m/s²||Sydney||9.797 m/s²|
|Cape Town||9.796 m/s²||Madrid||9.800 m/s²||Taipei||9.790 m/s²|
|Chicago||9.803 m/s²||Manila||9.784 m/s²||Tokyo||9.798 m/s²|
|Copenhagen||9.815 m/s²||Mexico City||9.779 m/s²||Vancouver, BC||9.809 m/s²|
|Nicosia||9.797 m/s²||New York||9.802 m/s²||Washington, DC||9.801 m/s²|
|Jakarta||9.781 m/s²||Oslo||9.819 m/s²||Wellington, NZ||9.803 m/s²|
|Frankfurt||9.810 m/s²||Ottawa||9.806 m/s²||Zurich||9.807 m/s²|
If the terrain is at sea level, we can estimate g:
This is the International Gravity Formula 1967, the 1967 Geodetic Reference System Formula, Helmert's equation or Clairault's formula.
The first correction to this formula is the free air correction (FAC), which accounts for heights above sea level. Gravity decreases with height, at a rate which near the surface of the Earth is such that linear extrapolation would give zero gravity at a height of one half the radius of the Earth, i.e. the rate is 9.8 m·s−2 per 3 200 km. Thus:
For flat terrain above sea level a second term is added, for the gravity due to the extra mass; for this purpose the extra mass can be approximated by an infinite horizontal slab, and we get 2πG times the mass per unit area, i.e. 4.2 m3·s−2·kg−1 (0.042 μGal·kg−1·m²)) (the Bouguer correction). For a mean rock density of 2.67 g·cm−3 this gives 1.1 s−2 (0.11 mGal·m−1). Combined with the free-air correction this means a reduction of gravity at the surface of ca. 2 µm·s−2 (0.20 mGal) for every meter of elevation of the terrain. (The two effects would cancel at a surface rock density of 4/3 times the average density of the whole Earth.)
For the gravity below the surface we have to apply the free-air correction as well as a double Bouguer correction. With the infinite slab model this is because moving the point of observation below the slab changes the gravity due to it to its opposite. Alternatively, we can consider a spherically symmetrical Earth and subtract from the mass of the Earth that of the shell outside the point of observation, because that does not cause gravity inside. This gives the same result.
Helmert's equation may be written equivalently to the version above as either:
An alternate formula for g as a function of latitude is the WGS (World Geodetic System) 84 Ellipsoidal Gravity Formula:
A spot check comparing results from the WGS-84 formula with those from Helmert's equation (using increments 10 degrees of latitude starting with zero) indicated that they produce values which differ by less than 10-6 m·s-2.
Additionally, Newton's second law, F = ma, where m is mass and a is acceleration, here tells us that
Comparing the two formulas it is seen that:
Note that this formula only works because of the pleasant (but non-obvious) mathematical fact that the gravity of a uniform spherical body, as measured on or above its surface, is the same as if all its mass were concentrated at a point at its centre. This is what allows us to use the Earth's radius for r.
The value obtained agrees approximately with the measured value of g. The difference may be attributed to several factors, mentioned above under "Variations":
There are significant uncertainties in the values of r and m1 as used in this calculation, and the value of G is also rather difficult to measure precisely.
If G, g and r are known then a reverse calculation will give an estimate of the mass of the Earth. This method was used by Henry Cavendish.
|Body|| Multiple of|
|Earth||1 (by definition)||9.8226|
For spherical bodies, surface gravity (cloud-top gravity for the gas giants) is calculated as follows: g = (m·G)/rm2 When a planet’s mean radius is unavailable, it can be calculated from planetary volume as follows: rm = (v·k)(1/3)
When a planet’s mean radius is unavailable, it can be calculated from planetary volume as follows: rm = (v·k)(1/3)