Gravitation is a natural phenomenon by which objects with mass attract one another.^{[1]} In everyday life, gravitation is most commonly thought of as the agency which lends weight to objects with mass. Gravitation compels dispersed matter to coalesce, thus it accounts for the very existence of the Earth, the Sun, and most of the macroscopic objects in the universe. It is responsible for keeping the Earth and the other planets in their orbits around the Sun; for keeping the Moon in its orbit around the Earth, for the formation of tides; for convection (by which hot fluids rise); for heating the interiors of forming stars and planets to very high temperatures; and for various other phenomena that we observe. Modern physics describes gravitation using the general theory of relativity, in which gravitation is a consequence of the curvature of spacetime which governs the motion of inertial objects. The simpler Newton's law of universal gravitation provides an excellent approximation for most calculations.
The terms gravitation and gravity are mostly interchangeable in everyday use, but a distinction may be made in scientific usage. "Gravitation" is a general term describing the phenomenon by which bodies with mass are attracted to one another, while "gravity" refers specifically to the gravitational force exerted by the Earth on objects in its vicinity.^{[2]}^{[3]}
History of gravitational theory Edit
 Main article: History of gravitational theory
Scientific revolution Edit
Modern work on gravitational theory began with the work of Galileo Galilei in the late 16th century and early 17th century. In his famous (though probably apocryphal)^{[4]} experiment dropping balls from the Tower of Pisa, and later with careful measurements of balls rolling down inclines, Galileo showed that gravitation accelerates all objects at the same rate. This was a major departure from Aristotle's belief that heavier objects are accelerated faster.^{[5]} (Galileo correctly postulated air resistance as the reason that lighter objects may fall more slowly in an atmosphere.) Galileo's work set the stage for the formulation of Newton's theory of gravity.
Newton's theory of gravitation Edit
 Main article: Newton's law of universal gravitation
In 1687, English mathematician Sir Isaac Newton published Principia, which hypothesizes the inversesquare law of universal gravitation. In his own words, “I deduced that the forces which keep the planets in their orbs must be reciprocally as the squares of their distances from the centers about which they revolve; and thereby compared the force requisite to keep the Moon in her orb with the force of gravity at the surface of the Earth; and found them answer pretty nearly.” Fortytwo years earlier Ismaël Bullialdus had proposed much the same theory.
Newton's theory enjoyed its greatest success when it was used to predict the existence of Neptune based on motions of Uranus that could not be accounted by the actions of the other planets. Calculations by John Couch Adams and Urbain Le Verrier both predicted the general position of the planet, and Le Verrier's calculations are what led Johann Gottfried Galle to the discovery of Neptune.
Ironically, it was another discrepancy in a planet's orbit that helped to point out flaws in Newton's theory. By the end of the 19th century, it was known that the orbit of Mercury showed slight perturbations that could not be accounted for entirely under Newton's theory, but all searches for another perturbing body (such as a planet orbiting the Sun even closer than Mercury) had been fruitless. The issue was resolved in 1915 by Albert Einstein's new General Theory of Relativity, which accounted for the small discrepancy in Mercury's orbit.
Although Newton's theory has been superseded, most modern nonrelativistic gravitational calculations are still made using Newton's theory because it is a much simpler theory to work with than General Relativity, and gives sufficiently accurate results for most applications.
General relativity Edit
 Main article: Introduction to general relativity
In general relativity, the effects of gravitation are ascribed to spacetime curvature instead of a force. The starting point for general relativity is the equivalence principle, which equates free fall with inertial motion and describes freefalling inertial objects as being accelerated relative to noninertial observers on the ground.^{[6]}^{[7]} In Newtonian physics, however, no such acceleration can occur unless at least one of the objects is being operated on by a force.
Einstein proposed that spacetime is curved by matter, and that freefalling objects are moving along locally straight paths in curved spacetime. These straight lines are called geodesics. Like Newton's First Law, Einstein's theory stated that if there is a force applied to an object, it would deviate from the geodesics in spacetime.^{[8]} For example, we are no longer following the geodesics while standing because the mechanical resistance of the Earth exerts an upward force on us. Thus, we are noninertial on the ground. This explains why moving along the geodesics in spacetime is considered inertial.
Einstein discovered the field equations of general relativity, which relate the presence of matter and the curvature of spacetime and are named after him. The Einstein field equations are a set of 10 simultaneous, nonlinear, differential equations. The solutions of the field equations are the components of the metric tensor of spacetime. A metric tensor describes a geometry of spacetime. The geodesic paths for a spacetime are calculated from the metric tensor.
Notable solutions of the Einstein field equations include:
 The Schwarzschild solution, which describes spacetime surrounding a spherically symmetric nonrotating uncharged massive object. For compact enough objects, this solution generated a black hole with a central singularity. For radial distances from the center which are much greater than the Schwarzschild radius, the accelerations predicted by the Schwarzschild solution are practically identical to those predicted by Newton's theory of gravity.
 The ReissnerNordström solution, in which the central object has an electrical charge. For charges with a geometrized length which are less than the geometrized length of the mass of the object, this solution produces black holes with two event horizons.
 The Kerr solution for rotating massive objects. This solution also produces black holes with multiple event horizons.
 The KerrNewman solution for charged, rotating massive objects. This solution also produces black holes with multiple event horizons.
 The cosmological RobertsonWalker solution, which predicts the expansion of the universe.
General relativity has enjoyed much success because of how its predictions of phenomena which are not called for by the theory of gravity have been regularly confirmed. For example:
 General relativity accounts for the anomalous perihelion precession of Mercury.Template:Fn
 The prediction that time runs slower at lower potentials has been confirmed by the PoundRebka experiment, the HafeleKeating experiment, and the GPS.
 The prediction of the deflection of light was first confirmed by Arthur Eddington in 1919,^{[9]} and has more recently been strongly confirmed through the use of a quasar which passes behind the Sun as seen from the Earth. See also gravitational lensing.
 The time delay of light passing close to a massive object was first identified by Irwin Shapiro in 1964 in interplanetary spacecraft signals.
 Gravitational radiation has been indirectly confirmed through studies of binary pulsars.
 The expansion of the universe (predicted by Alexander Friedmann) was confirmed by Edwin Hubble in 1929.
Gravity and quantum mechanicsEdit
 Main article: Graviton
Several decades after the discovery of general relativity it was realized that general relativity is incompatible with quantum mechanics.^{[10]} It is possible to describe gravity in the framework of quantum field theory like the other fundamental forces, such that the attractive force of gravity arises due to exchange of virtual gravitons, in the same way as the electromagnetic force arises from exchange of virtual photons.^{[11]}^{[12]} This reproduces general relativity in the classical limit. However, this approach fails at short distances of the order of the Planck length,^{[13]} where a more complete theory of quantum gravity (or a new approach to quantum mechanics) is required. Many believe the complete theory to be string theory,^{[14]} or more currently M Theory.
Specifics Edit
Earth's gravityEdit
 Main article: Earth's gravity
Every planetary body (including the Earth) is surrounded by its own gravitational field, which exerts an attractive force on all objects. Assuming a spherically symmetrical planet (a reasonable approximation), the strength of this field at any given point is proportional to the planetary body's mass and inversely proportional to the square of the distance from the center of the body.
The strength of the gravitational field is numerically equal to the acceleration of objects under its influence, and its value at the Earth's surface, denoted g, is approximately expressed below as the standard average.
g = 9.8 m/s^{2} = 32.2 ft/s^{2}
This means that, ignoring air resistance, an object falling freely near the earth's surface increases its velocity with 9.8 m/s (32.2 ft/s or 22 mph) for each second of its descent. Thus, an object starting from rest will attain a velocity of 9.8 m/s (32.2 ft/s) after one second, 19.6 m/s (64.4 ft/s) after two seconds, and so on, adding 9.8 m/s (32.2 ft/s) to each resulting velocity. Also, again ignoring air resistance, any and all objects, when dropped from the same height, will hit the ground at the same time.
According to Newton's 3rd Law, the Earth itself experiences an equal and opposite force to that acting on the falling object, meaning that the Earth also accelerates towards the object (until the object hits the earth, then the Law of Conservation of Energy states that it will move back with the same acceleration with which it initially moved forward, canceling out the two forces of gravity.). However, because the mass of the Earth is huge, the acceleration of the Earth by this same force is negligible, when measured relative to the system's center of mass.
Equations for a falling body near the surface of the Earth Edit
 Main article: Equations for a falling body
Under an assumption of constant gravity, Newton’s law of gravitation simplifies to F = mg, where m is the mass of the body and g is a constant vector with an average magnitude of 9.81 m/s². The acceleration due to gravity is equal to this g. An initiallystationary object which is allowed to fall freely under gravity drops a distance which is proportional to the square of the elapsed time. The image on the right, spanning half a second, was captured with a stroboscopic flash at 20 flashes per second. During the first 1/20th of a second the ball drops one unit of distance (here, a unit is about 12 mm); by 2/20ths it has dropped at total of 4 units; by 3/20ths, 9 units and so on.
Under the same constant gravity assumptions, the potential energy, E_{p}, of a body at height h is given by E_{p} = mgh (or E_{p} = Wh, with W meaning weight). This expression is valid only over small distances h from the surface of the Earth. Similarly, the expression for the maximum height reached by a vertically projected body with velocity v is useful for small heights and small initial velocities only. In case of large initial velocities we have to use the principle of conservation of energy to find the maximum height reached. This same expression can be solved for v to determine the velocity of an object dropped from a height h immediately before hitting the ground, , assuming negligible air resistance.
Gravity and astronomyEdit
 Main article: Gravitation (astronomy)
The discovery and application of Newton's law of gravity accounts for the detailed information we have about the planets in our solar system, the mass of the Sun, the distance to stars, quasars and even the theory of dark matter. Although we have not traveled to all the planets nor to the Sun, we know their masses. These masses are obtained by applying the laws of gravity to the measured characteristics of the orbit. In space an object maintains its orbit because of the force of gravity acting upon it. Planets orbit stars, stars orbit galactic centers, galaxies orbit a center of mass in clusters, and clusters orbit in superclusters. The force of gravity is proportional to the mass of an object and inversely proportional to the square of the distance between the objects.
Gravitational radiationEdit
 Main article: Gravitational wave
In general relativity, gravitational radiation is generated in situations where the curvature of spacetime is oscillating, such as is the case with coorbiting objects. The gravitational radiation emitted by the solar system is far too small to measure. However, gravitational radiation has been indirectly observed as an energy loss over time in binary pulsar systems such as PSR 1913+16. It is believed that neutron star mergers and black hole formation may create detectable amounts of gravitational radiation. Gravitational radiation observatories such as LIGO have been created to study the problem. No confirmed detections have been made of this hypothetical radiation, but as the science behind LIGO is refined and as the instruments themselves are endowed with greater sensitivity over the next decade, this may change.
Anomalies and discrepanciesEdit
There are some observations that are not adequately accounted for, which may point to the need for better theories of gravity or perhaps be explained in other ways.
 Stars in galaxies follow a distribution of velocities where stars on the outskirts are moving faster than they should according to the observed distributions of normal matter. Galaxies within galaxy clusters show a similar pattern. Dark matter, which would interact gravitationally but not electromagnetically, would account for the discrepancy. Various modifications to Newtonian dynamics have also been proposed.
 The two Pioneer spacecraft seem to be slowing down in a way which has yet to be explained.^{[15]}
 Various spacecraft have experienced greater accelerations during slingshot maneuvers than expected.
 The expansion of the universe seems to be speeding up. Dark energy has been proposed to explain this. A recent alternative explanation is that the geometry of space is not homogeneous (due to clusters of galaxies) and that when the data is reinterpreted to take this into account, the expansion is not speeding up after all^{[16]}, however this conclusion is disputed^{[17]}.
Alternative theoriesEdit
 Main article: Alternatives to general relativity
Historical alternative theoriesEdit
 Aristotelian theory of gravity
 Le Sage's theory of gravitation (1784) also called LeSage gravity, proposed by GeorgesLouis Le Sage, based on a fluidbased explanation where a light gas fills the entire universe.
 Nordström's theory of gravitation (1912, 1913), an early competitor of general relativity.
 Whitehead's theory of gravitation (1922), another early competitor of general relativity.
Recent alternative theoriesEdit
 BransDicke theory of gravity (1961)
 Induced gravity (1967), a proposal by Andrei Sakharov according to which general relativity might arise from quantum field theories of matter
 Rosen bimetric theory of gravity
 In the modified Newtonian dynamics (MOND) (1981), Mordehai Milgrom proposes a modification of Newton's Second Law of motion for small accelerations
 The selfcreation cosmology theory of gravity (1982) by G.A. Barber in which the BransDicke theory is modified to allow mass creation
 Nonsymmetric gravitational theory (NGT) (1994) by John Moffat
 Tensorvectorscalar gravity (TeVeS) (2004), a relativistic modification of MOND by Jacob Bekenstein
See alsoEdit
 Antigravity, the idea of neutralizing or repelling gravity
 Artificial gravity
 Escape velocity, the minimum velocity needed to fly away from a massive space object
 General relativity
 gforce, a measure of acceleration
 Gravitational field
 Gravitational waves
 Gravitational binding energy
 Gravity Research Foundation
 Gauss's law for gravity
 JovianPlutonian gravitational effect
 Kepler's third law of planetary motion
 Newton's laws of motion
 nbody problem
 The Pioneer spacecraft anomaly
 Scalar Gravity
 Speed of gravity
 Standard gravitational parameter
 Standard gravity
 Weight
 Weightlessness
 Lagrange Points
 Gravity assist
NotesEdit
 Template:Fnb Proposition 75, Theorem 35: p.956  I.Bernard Cohen and Anne Whitman, translators: Isaac Newton, The Principia: Mathematical Principles of Natural Philosophy. Preceded by A Guide to Newton's Principia, by I. Bernard Cohen. University of California Press 1999 ISBN 0520088166 ISBN 0520088174
 Template:Fnb Max Born (1924), Einstein's Theory of Relativity (The 1962 Dover edition, page 348 lists a table documenting the observed and calculated values for the precession of the perihelion of Mercury, Venus, and Earth.)
FootnotesEdit
 ↑ Does Gravity Travel at the Speed of Light?, UCR Mathematics. 1998. Retrieved 3 July 2008
 ↑ http://ocw.mit.edu/NR/rdonlyres/EarthAtmosphericandPlanetarySciences/12090Spring2007/LectureNotes/earthsurface_10.pdf
 ↑ http://alex.edfac.usyd.edu.au/Methods/Science/studentwork/MassoftheEarth/gravitationandgravity.htm
 ↑ Ball, Phil (06 2005). "Tall Tales". Nature News. doi: . ISSN 00280836.
 ↑ Galileo (1638), Two New Sciences, First Day Salviati speaks: "If this were what Aristotle meant you would burden him with another error which would amount to a falsehood; because, since there is no such sheer height available on earth, it is clear that Aristotle could not have made the experiment; yet he wishes to give us the impression of his having performed it when he speaks of such an effect as one which we see."
 ↑ http://www.blackholes.org/relativity6.html
 ↑ http://laser.phys.ualberta.ca/~egerton/genrel.htm
 ↑ Law of Geodesic Motion http://blog.sauliaus.info/temp/gravity.pdf
 ↑ Dyson; Eddington, A.S., & Davidson, C.R. (1920). "A Determination of the Deflection of Light by the Sun's Gravitational Field, from Observations Made at the Total Eclipse of May 29, 1919". Phil. Trans. Roy. Soc. A 220: 291–333, http://adsabs.harvard.edu/abs/1920RSPTA.220..291D.
 ↑ Randall, Lisa (2005). Warped Passages: Unraveling the Universe's Hidden Dimensions, Ecco. ISBN 0060531088.
 ↑ Feynman, R. P.; Morinigo, F. B., Wagner, W. G., & Hatfield, B. (1995). Feynman lectures on gravitation, AddisonWesley. ISBN 0201627345.
 ↑ Zee, A. (2003). Quantum Field Theory in a Nutshell, Princeton University Press. ISBN 0691010196.
 ↑ Randall, Lisa (2005). Warped Passages: Unraveling the Universe's Hidden Dimensions, Ecco. ISBN 0060531088.
 ↑ Greene, Brian (2000). The elegant universe: superstrings, hidden dimensions, and the quest for the ultimate theory. New York: Vintage Books. ISBN 0375708111.
 ↑ Wanted: Einstein Jr, The Economist, 6th March 2008.
 ↑ Dark energy may just be a cosmic illusion, New Scientist, issue 2646, 7th March 2008.
 ↑ Swisscheese model of the cosmos is full of holes, New Scientist, issue 2678, 18th October 2008.
ReferencesEdit
 Halliday, David; Robert Resnick; Kenneth S. Krane (2001). Physics v. 1. New York: John Wiley & Sons. ISBN 0471320579.
 Serway, Raymond A.; Jewett, John W. (2004). Physics for Scientists and Engineers (6th ed. ed.), Brooks/Cole. ISBN 0534408427.
 Tipler, Paul (2004). Physics for Scientists and Engineers: Mechanics, Oscillations and Waves, Thermodynamics (5th ed. ed.), W. H. Freeman. ISBN 0716708094.
External links Edit
Look up Gravitation in Wiktionary, the free dictionary. 
 Chapter 10. Gravity, from Light and Matter: educational materials for physics and astronomy
 Gravity Probe B Experiment The Official Einstein website from Stanford University
 Center for Gravity, Electrical, and Magnetic Studies
 Gravity for kids (flash)
 Ask a scientist, Physics Archive
 How stuff works:
 Alternative theory of gravity explains large structure formation  without dark matter PhysOrg.com
 Do it yourself, gravitation experiment
 How to calculate the size of the gravitation
 Gravity simulator  watch gravity in action
