For other uses, see Gravity (disambiguation).
"Gravitation" and "Law of Gravity" redirect here. For other uses, see Gravitation (disambiguation) and Law of Gravity (disambiguation).
Hammer and feather drop: Apollo 15 astronaut David Scott on the Moon enacting the legend of Galileo's gravity experiment. (1.38 MB, ogg/Theora format).
Gravity or gravitation is a natural phenomenon by which all things attract one another including stars, planets, galaxies and even light and subatomic particles. Gravity is responsible for the formation of the universe (e.g. creating spheres of hydrogen, igniting them under pressure to form stars and grouping them in to galaxies). Gravity is a cause of time dilation (time lapses more slowly in strong gravitation). Without gravity, the universe would be without thermal energy and composed only of equally spaced particles. On Earth, gravity gives weight to physical objects and causes the tides. Gravity has an infinite range, and it cannot be absorbed, transformed, or shielded against.
Gravity is most accurately described by the general theory of relativity (proposed by Albert Einstein in 1915) which describes gravity, not as a force, but as a consequence of the curvature of spacetime caused by the uneven distribution of mass/energy. For most applications, gravity is well approximated by Newton's law of universal gravitation, which postulates that the gravitational force of two bodies of mass is directly proportional to the product of their masses and inversely proportional to the square of the distance between them.
Gravity is the weakest of the four fundamental interactions of nature. The gravitational attraction is approximately 10^{−38} times the strength of the strong force (i.e. gravity is 38 orders of magnitude weaker), 10^{−36} times the strength of the electromagnetic force, and 10^{−29} times the strength of the weak force. As a consequence, gravity has a negligible influence on the behavior of subatomic particles, and plays no role in determining the internal properties of everyday matter (but see quantum gravity). On the other hand, gravity is the dominant force at the macroscopic scale, that is the cause of the formation, shape, and trajectory (orbit) of astronomical bodies, including those of asteroids, comets, planets, stars, and galaxies. It is responsible for causing the Earth and the other planets to orbit the Sun; for causing the Moon to orbit the Earth; for the formation of tides; for natural convection, by which fluid flow occurs under the influence of a density gradient and gravity; for heating the interiors of forming stars and planets to very high temperatures; for solar system, galaxy, stellar formation and evolution; and for various other phenomena observed on Earth and throughout the universe.
In pursuit of a theory of everything, the merging of general relativity and quantum mechanics (or quantum field theory) into a more general theory of quantum gravity has become an area of research.
Contents
 1 History of gravitational theory
 1.1 Scientific revolution
 1.2 Newton's theory of gravitation
 1.3 Equivalence principle
 1.4 General relativity
 1.5 Gravity and quantum mechanics
 2 Specifics
 2.1 Earth's gravity
 2.2 Equations for a falling body near the surface of the Earth
 2.3 Gravity and astronomy
 2.4 Gravitational radiation
 2.5 Speed of gravity
 3 Anomalies and discrepancies
 4 Alternative theories
 4.1 Historical alternative theories
 4.2 Recent alternative theories
 5 See also
 6 Footnotes
 7 References
 8 Further reading
 9 External links
History of gravitational theory
Main article: History of gravitational theory
Classical mechanics 
Second law of motion


Branches
 Applied
 Celestial
 Continuum
 Dynamics
 Kinematics
 Kinetics
 Statics
 Statistical

Fundamentals
 Acceleration
 Angular momentum
 Couple
 D'Alembert's principle
 Energy
 Force
 Frame of reference
 Impulse
 Inertia / Moment of inertia
 Mass
Mechanical power
 Mechanical work
Moment
 Momentum
 Space
 Speed
 Time
 Torque
 Velocity
 Virtual work

Formulations

Newton's laws of motion

Analytical mechanics
Lagrangian mechanics
Hamiltonian mechanics
Routhian mechanics
Hamilton–Jacobi equation
Appell's equation of motion
Udwadia–Kalaba equation

Core topics
 Damping (ratio)
 Displacement
 Equations of motion
 Euler's laws of motion
 Fictitious force
 Friction
 Harmonic oscillator
 Inertial / Noninertial reference frame
 Mechanics of planar particle motion
 Motion (linear)
 Newton's law of universal gravitation
 Newton's laws of motion
 Relative velocity
 Rigid body
 dynamics
 Euler's equations
 Simple harmonic motion
 Vibration

Rotation
 Circular motion
 Rotating reference frame
 Centripetal force
 Centrifugal force
 reactive
 rotating reference frame
 Coriolis force
 Pendulum
 Tangential speed
 Rotational speed
 Angular acceleration / displacement / frequency / velocity

Scientists
 Galileo
 Newton
 Kepler
 Horrocks
 Halley
 Euler
 d'Alembert
 Clairaut
 Lagrange
 Laplace
 Hamilton
 Poisson
 Daniel Bernoulli
 Johann Bernoulli
 Cauchy


Scientific revolution
Modern work on gravitational theory began with the work of Galileo Galilei in the late 16th and early 17th centuries. In his famous (though possibly apocryphal^{[1]}) experiment dropping balls from the Tower of Pisa, and later with careful measurements of balls rolling down inclines, Galileo showed that gravity accelerates all objects at the same rate. This was a major departure from Aristotle's belief that heavier objects accelerate faster.^{[2]} Galileo 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
Main article: Newton's law of universal gravitation
Sir Isaac Newton, an English physicist who lived from 1642 to 1727
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."^{[3]} The equation is the following:
Where F is the force, m_{1} and m_{2} are the masses of the objects interacting, r is the distance between the centers of the masses and G is the gravitational constant.
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 for by the actions of the other planets. Calculations by both John Couch Adams and Urbain Le Verrier predicted the general position of the planet, and Le Verrier's calculations are what led Johann Gottfried Galle to the discovery of Neptune.
A discrepancy in Mercury's orbit pointed out flaws in Newton's theory. By the end of the 19th century, it was known that its orbit 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 theory of general relativity, which accounted for the small discrepancy in Mercury's orbit.
Although Newton's theory has been superseded by the Einstein's general relativity, most modern nonrelativistic gravitational calculations are still made using the Newton's theory because it is simpler to work with and it gives sufficiently accurate results for most applications involving sufficiently small masses, speeds and energies.
Equivalence principle
The equivalence principle, explored by a succession of researchers including Galileo, Loránd Eötvös, and Einstein, expresses the idea that all objects fall in the same way. The simplest way to test the weak equivalence principle is to drop two objects of different masses or compositions in a vacuum and see whether they hit the ground at the same time. Such experiments demonstrate that all objects fall at the same rate when other forces (such as air resistance and electromagnetic effects) are negligible. More sophisticated tests use a torsion balance of a type invented by Eötvös. Satellite experiments, for example STEP, are planned for more accurate experiments in space.^{[4]}
Formulations of the equivalence principle include:
 The weak equivalence principle: The trajectory of a point mass in a gravitational field depends only on its initial position and velocity, and is independent of its composition.^{[5]}
 The Einsteinian equivalence principle: The outcome of any local nongravitational experiment in a freely falling laboratory is independent of the velocity of the laboratory and its location in spacetime.^{[6]}
 The strong equivalence principle requiring both of the above.
General relativity
See also: Introduction to general relativity
Twodimensional analogy of spacetime distortion generated by the mass of an object. Matter changes the geometry of spacetime, this (curved) geometry being interpreted as gravity. White lines do not represent the curvature of space but instead represent the coordinate system imposed on the curved spacetime, which would be rectilinear in a flat spacetime.
General relativity 


Fundamental concepts
 Equivalence principle
 Special relativity
 World line
 Riemannian geometry

Phenomena
 Kepler problem
 Gravitational lensing
 Gravitational waves
 Framedragging
 Geodetic effect
 Event horizon
 Singularity
 Black hole

Spacetime 
 Spacetime diagrams
 Minkowski spacetime
 Wormhole


Equations 
 Linearized gravity
 Einstein field equations
 Friedmann
 Geodesics
 Mathisson–Papapetrou–Dixon
 Hamilton–Jacobi–Einstein

Formalisms 

Advanced theory 
 Kaluza–Klein theory
 Quantum gravity


Solutions
 Schwarzschild
 Reissner–Nordström
 Gödel
 Kerr
 Kerr–Newman
 Kasner
 Lemaître–Tolman
 TaubNUT
 Milne
 Robertson–Walker
 ppwave
 van Stockum dust

Scientists
 Einstein
 Lorentz
 Hilbert
 Poincaré
 Schwarzschild
 de Sitter
 Reissner
 Nordström
 Weyl
 Eddington
 Friedman
 Milne
 Zwicky
 Lemaître
 Gödel
 Wheeler
 Robertson
 Bardeen
 Walker
 Kerr
 Chandrasekhar
 Ehlers
 Penrose
 Hawking
 Raychaudhuri
 Taylor
 Hulse
 van Stockum
 Taub
 Newman
 Yau
 Thorne
 others


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.^{[7]}^{[8]} 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 paths are called geodesics. Like Newton's first law of motion, Einstein's theory states that if a force is applied on an object, it would deviate from a geodesic. For instance, we are no longer following geodesics while standing because the mechanical resistance of the Earth exerts an upward force on us, and we are noninertial on the ground as a result. 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 FriedmannLemaîtreRobertsonWalker solution, which predicts the expansion of the universe.
The tests of general relativity included the following:^{[9]}
 General relativity accounts for the anomalous perihelion precession of Mercury.^{[10]}
 The prediction that time runs slower at lower potentials has been confirmed by the Pound–Rebka experiment, the Hafele–Keating experiment, and the GPS.
 The prediction of the deflection of light was first confirmed by Arthur Stanley Eddington from his observations during the Solar eclipse of May 29, 1919.^{[11]}^{[12]} Eddington measured starlight deflections twice those predicted by Newtonian corpuscular theory, in accordance with the predictions of general relativity. However, his interpretation of the results was later disputed.^{[13]} More recent tests using radio interferometric measurements of quasars passing behind the Sun have more accurately and consistently confirmed the deflection of light to the degree predicted by general relativity.^{[14]} See also gravitational lens.
 The time delay of light passing close to a massive object was first identified by Irwin I. Shapiro in 1964 in interplanetary spacecraft signals.
 Gravitational radiation has been indirectly confirmed through studies of binary pulsars.
 Alexander Friedmann in 1922 found that Einstein equations have nonstationary solutions (even in the presence of the cosmological constant). In 1927 Georges Lemaître showed that static solutions of the Einstein equations, which are possible in the presence of the cosmological constant, are unstable, and therefore the static universe envisioned by Einstein could not exist. Later, in 1931, Einstein himself agreed with the results of Friedmann and Lemaître. Thus general relativity predicted that the Universe had to be nonstatic—it had to either expand or contract. The expansion of the universe discovered by Edwin Hubble in 1929 confirmed this prediction.^{[15]}
 The theory's prediction of frame dragging was consistent with the recent Gravity Probe B results.^{[16]}
 General relativity predicts that light should lose its energy when travelling away from the massive bodies. The group of Radek Wojtak of the Niels Bohr Institute at the University of Copenhagen collected data from 8000 galaxy clusters and found that the light coming from the cluster centers tended to be redshifted compared to the cluster edges, confirming the energy loss due to gravity.^{[17]}
Gravity and quantum mechanics
Main articles: Graviton and Quantum gravity
In the decades after the discovery of general relativity, it was realized that general relativity is incompatible with quantum mechanics.^{[18]} 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.^{[19]}^{[20]} This reproduces general relativity in the classical limit. However, this approach fails at short distances of the order of the Planck length,^{[18]} where a more complete theory of quantum gravity (or a new approach to quantum mechanics) is required.
Specifics
Earth's gravity
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, the strength of this field at any given point above the surface 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.^{[citation needed]} The rate of acceleration of falling objects near the Earth's surface varies very slightly depending on elevation, latitude, and other factors. For purposes of weights and measures, a standard gravity value is defined by the International Bureau of Weights and Measures, under the International System of Units (SI).
That value, denoted g, is g = 9.80665 m/s^{2} (32.1740 ft/s^{2}).^{[21]}^{[22]}
The standard value of 9.80665 m/s^{2} is the one originally adopted by the International Committee on Weights and Measures in 1901 for 45° latitude, even though it has been shown to be too high by about five parts in ten thousand.^{[23]} This value has persisted in meteorology and in some standard atmospheres as the value for 45° latitude even though it applies more precisely to latitude of 45°32'33".^{[24]}
Assuming the standardized value for g and ignoring air resistance, this means that an object falling freely near the Earth's surface increases its velocity by 9.80665 m/s (32.1740 ft/s or 22 mph) for each second of its descent. Thus, an object starting from rest will attain a velocity of 9.80665 m/s (32.1740 ft/s) after one second, approximately 19.62 m/s (64.4 ft/s) after two seconds, and so on, adding 9.80665 m/s (32.1740 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. It is relevant to note that Earth's gravity doesn't have exactly the same value in all regions. There are slight variations in different parts of the globe due to latitude, surface features such as mountains and ridges, and perhaps unusually high or low subsurface densities.^{[25]}
If an object with comparable mass to that of the Earth were to fall towards it, then the corresponding acceleration of the Earth would be observable.
According to Newton's 3rd Law, the Earth itself experiences a force equal in magnitude and opposite in direction to that which it exerts on a falling object. This means that the Earth also accelerates towards the object until they collide. Because the mass of the Earth is huge, however, the acceleration imparted to the Earth by this opposite force is negligible in comparison to the object's. If the object doesn't bounce after it has collided with the Earth, each of them then exerts a repulsive contact force on the other which effectively balances the attractive force of gravity and prevents further acceleration.
The force of gravity on Earth is the resultant (vector sum) of two forces:^{[dubious – discuss]}^{[citation needed]} (a) The gravitational attraction in accordance with Newton's universal law of gravitation, and (b) the centrifugal force^{[dubious – discuss]}^{[citation needed]}, which results from the choice of an earthbound, rotating frame of reference. At the equator, the force of gravity is the weakest due to the centrifugal force caused by the Earth's rotation. The force of gravity varies with latitude and increases from about 9.780 m/s^{2} at the Equator to about 9.832 m/s^{2} at the poles.
Equations for a falling body near the surface of the Earth
Ball falling freely under gravity. See text for description.
Main article: Equations for a falling body
Under an assumption of constant gravitational attraction, Newton's law of universal 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/s^{2} on Earth. This resulting force is the object's weight. The acceleration due to gravity is equal to this g. An initially stationary 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}⁄_{20} of a second the ball drops one unit of distance (here, a unit is about 12 mm); by ^{2}⁄_{20} it has dropped at total of 4 units; by ^{3}⁄_{20}, 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 initial velocity v is useful for small heights and small initial velocities only.
Gravity and astronomy
Gravity acts on stars that conform our Milky Way.
^{[26]}
The application of Newton's law of gravity has enabled the acquisition of much of the detailed information we have about the planets in our solar system, the mass of the Sun, and details of quasars; even the existence of dark matter is inferred using Newton's law of gravity. 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 exerted on one object by another is directly proportional to the product of those objects' masses and inversely proportional to the square of the distance between them.
Gravitational radiation
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 B1913+16. It is believed that neutron star mergers and black hole formation may create detectable amounts of gravitational radiation. Gravitational radiation observatories such as the Laser Interferometer Gravitational Wave Observatory (LIGO) have been created to study the problem. No confirmed detections have been made of this hypothetical radiation.
Speed of gravity
Main article: Speed of gravity
In December 2012, a research team in China announced that it had produced measurements of the phase lag of Earth tides during full and new moons which seem to prove that the speed of gravity is equal to the speed of light.^{[27]} This means that if the Sun suddenly disappeared, the Earth would keep orbiting it normally for 8 minutes, which is the time light takes to travel that distance. The team's findings were released in the Chinese Science Bulletin in February 2013.^{[28]}
Anomalies and discrepancies
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.
Rotation curve of a typical spiral galaxy: predicted (A) and observed (B). The discrepancy between the curves is attributed to dark matter.
 Extrafast stars: 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.
 Flyby anomaly: Various spacecraft have experienced greater acceleration than expected during gravity assist maneuvers.
 Accelerating expansion: The metric expansion of space 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 are reinterpreted to take this into account, the expansion is not speeding up after all,^{[29]} however this conclusion is disputed.^{[30]}
 Anomalous increase of the astronomical unit: Recent measurements indicate that planetary orbits are widening faster than if this were solely through the sun losing mass by radiating energy.
 Extra energetic photons: Photons travelling through galaxy clusters should gain energy and then lose it again on the way out. The accelerating expansion of the universe should stop the photons returning all the energy, but even taking this into account photons from the cosmic microwave background radiation gain twice as much energy as expected. This may indicate that gravity falls off faster than inversesquared at certain distance scales.^{[31]}
 Extra massive hydrogen clouds: The spectral lines of the Lymanalpha forest suggest that hydrogen clouds are more clumped together at certain scales than expected and, like dark flow, may indicate that gravity falls off slower than inversesquared at certain distance scales.^{[31]}
 Power: Proposed extra dimensions could explain why the gravity force is so weak.^{[32]}
Alternative theories
Main article: Alternatives to general relativity
Historical alternative theories
 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.
 Ritz's theory of gravitation, Ann. Chem. Phys. 13, 145, (1908) pp. 267–271, WeberGauss electrodynamics applied to gravitation. Classical advancement of perihelia.
 Nordström's theory of gravitation (1912, 1913), an early competitor of general relativity.
 Kaluza Klein theory (1921)
 Whitehead's theory of gravitation (1922), another early competitor of general relativity.
Recent alternative theories
 Brans–Dicke theory of gravity (1961) ^{[33]}
 Induced gravity (1967), a proposal by Andrei Sakharov according to which general relativity might arise from quantum field theories of matter
 ƒ(R) gravity (1970)
 Horndeski theory (1974) ^{[34]}
 Supergravity (1976)
 String theory
 In the modified Newtonian dynamics (MOND) (1981), Mordehai Milgrom proposes a modification of Newton's Second Law of motion for small accelerations ^{[35]}
 The selfcreation cosmology theory of gravity (1982) by G.A. Barber in which the BransDicke theory is modified to allow mass creation
 Loop quantum gravity (1988) by Carlo Rovelli, Lee Smolin, and Abhay Ashtekar
 Nonsymmetric gravitational theory (NGT) (1994) by John Moffat
 Tensor–vector–scalar gravity (TeVeS) (2004), a relativistic modification of MOND by Jacob Bekenstein
 Gravity as an entropic force, gravity arising as an emergent phenomenon from the thermodynamic concept of entropy.
 In the superfluid vacuum theory the gravity and curved spacetime arise as a collective excitation mode of nonrelativistic background superfluid.
 Chameleon theory (2004) by Justin Khoury and Amanda Weltman.
 Pressuron theory (2013) by Olivier Minazzoli and Aurélien Hees.
See also

Gravitation portal 

Physics portal 
 Angular momentum
 Antigravity, the idea of neutralizing or repelling gravity
 Artificial gravity
 Birkeland current
 Gravitational wave
 Gravitational wave background
 Cosmic gravitational wave background
 Einstein–Infeld–Hoffmann equations
 Escape velocity, the minimum velocity needed to escape from a gravity well
 gforce, a measure of acceleration
 Gauge gravitation theory
 Gauss's law for gravity
 Gravitational binding energy
 Gravity assist
 Gravity gradiometry
 Gravity Recovery and Climate Experiment
 Gravity Research Foundation
 Jovian–Plutonian gravitational effect
 Kepler's third law of planetary motion
 Lagrangian point
 Microg environment, also called microgravity
 Mixmaster dynamics
 nbody problem
 Newton's laws of motion
 Pioneer anomaly
 Scalar theories of gravitation
 Speed of gravity
 Standard gravitational parameter
 Standard gravity
 Weightlessness
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 ^ 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."
 ^ *Chandrasekhar, Subrahmanyan (2003). Newton's Principia for the common reader. Oxford: Oxford University Press. (pp.1–2). The quotation comes from a memorandum thought to have been written about 1714. As early as 1645 Ismaël Bullialdus had argued that any force exerted by the Sun on distant objects would have to follow an inversesquare law. However, he also dismissed the idea that any such force did exist. See, for example, Linton, Christopher M. (2004). From Eudoxus to Einstein—A History of Mathematical Astronomy. Cambridge: Cambridge University Press. p. 225. ISBN 9780521827508.
 ^ M.C.W.Sandford (2008). "STEP: Satellite Test of the Equivalence Principle". Rutherford Appleton Laboratory. Retrieved 20111014.
 ^ Paul S Wesson (2006). Fivedimensional Physics. World Scientific. p. 82. ISBN 9812566619.
 ^ Haugen, Mark P.; C. Lämmerzahl (2001). Principles of Equivalence: Their Role in Gravitation Physics and Experiments that Test Them. Springer. arXiv:grqc/0103067. ISBN 9783540412366.
 ^ "Gravity and Warped Spacetime". blackholes.org. Retrieved 20101016.
 ^ Dmitri Pogosyan. "Lecture 20: Black Holes—The Einstein Equivalence Principle". University of Alberta. Retrieved 20111014.
 ^ Pauli, Wolfgang Ernst (1958). "Part IV. General Theory of Relativity". Theory of Relativity. Courier Dover Publications. ISBN 9780486641522.
 ^ 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.)
 ^ Dyson, F.W.; 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 (571–581): 291–333. Bibcode:1920RSPTA.220..291D. doi:10.1098/rsta.1920.0009. . Quote, p. 332: "Thus the results of the expeditions to Sobral and Principe can leave little doubt that a deflection of light takes place in the neighbourhood of the sun and that it is of the amount demanded by Einstein's generalised theory of relativity, as attributable to the sun's gravitational field."
 ^ Weinberg, Steven (1972). Gravitation and cosmology. John Wiley & Sons. . Quote, p. 192: "About a dozen stars in all were studied, and yielded values 1.98 ± 0.11" and 1.61 ± 0.31", in substantial agreement with Einstein's prediction θ_{☉} = 1.75"."
 ^ Earman, John; Glymour, Clark (1980). "Relativity and Eclipses: The British eclipse expeditions of 1919 and their predecessors". Historical Studies in the Physical Sciences 11: 49–85. doi:10.2307/27757471.
 ^ Weinberg, Steven (1972). Gravitation and cosmology. John Wiley & Sons. p. 194.
 ^ See W.Pauli, 1958, pp.219–220
 ^ "NASA's Gravity Probe B Confirms Two Einstein SpaceTime Theories". Nasa.gov. Retrieved 20130723.
 ^ Bhattacharjee, Yudhijit. "Galaxy Clusters Validate Einstein's Theory". News.sciencemag.org. Retrieved 20130723.
 ^ ^{a} ^{b} 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.
 ^ Bureau International des Poids et Mesures (2006). "The International System of Units (SI)" (PDF) (8th ed.). p. 131. Retrieved 20091125.
Unit names are normally printed in Roman (upright) type ... Symbols for quantities are generally single letters set in an italic font, although they may be qualified by further information in subscripts or superscripts or in brackets.
 ^ "SI Unit rules and style conventions". National Institute For Standards and Technology (USA). September 2004. Retrieved 20091125.
Variables and quantity symbols are in italic type. Unit symbols are in Roman type.
 ^ List, R. J. editor, 1968, Acceleration of Gravity, Smithsonian Meteorological Tables, Sixth Ed. Smithsonian Institution, Washington, D.C., p. 68.
 ^ U.S. Standard Atmosphere, 1976, U.S. Government Printing Office, Washington, D.C., 1976. (Linked file is very large.)
 ^ "Astronomy Picture of the Day".
 ^ "Milky Way Emerges as Sun Sets over Paranal". www.eso.org. European Southern Obseevatory. Retrieved 29 April 2015.
 ^ Chinese scientists find evidence for speed of gravity, astrowatch.com, 12/28/12.
 ^ TANG, Ke Yun; HUA ChangCai; WEN Wu; CHI ShunLiang; YOU QingYu; YU Dan (February 2013). "Observational evidences for the speed of the gravity based on the Earth tide" (PDF). Chinese Science Bulletin 58 (45): 474–477. doi:10.1007/s1143401256033. Retrieved 12 June 2013.
 ^ Dark energy may just be a cosmic illusion, New Scientist, issue 2646, 7 March 2008.
 ^ Swisscheese model of the cosmos is full of holes, New Scientist, issue 2678, 18 October 2008.
 ^ ^{a} ^{b} Chown, Marcus (16 March 2009). "Gravity may venture where matter fears to tread". New Scientist (2699). Retrieved 4 August 2013.
 ^ CERN (20 January 2012). "Extra dimensions, gravitons, and tiny black holes".
 ^ Brans, C.H. (Mar 2014). "JordanBransDicke Theory". Scholarpedia 9: 31358. Bibcode:2014Schpj...931358B. doi:10.4249/scholarpedia.31358.
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 ^ Milgrom, M. (Jun 2014). "The MOND paradigm of modified dynamics". Scholarpedia 9: 31410. Bibcode:2014SchpJ...931410M. doi:10.4249/scholarpedia.31410.
References
 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.). Brooks/Cole. ISBN 0534408427.
 Tipler, Paul (2004). Physics for Scientists and Engineers: Mechanics, Oscillations and Waves, Thermodynamics (5th ed.). W. H. Freeman. ISBN 0716708094.
Further reading
 Thorne, Kip S.; Misner, Charles W.; Wheeler, John Archibald (1973). Gravitation. W.H. Freeman. ISBN 0716703440.
External links

Look up gravity in Wiktionary, the free dictionary. 

Wikimedia Commons has media related to Gravitation. 
 Hazewinkel, Michiel, ed. (2001), "Gravitation", Encyclopedia of Mathematics, Springer, ISBN 9781556080104
 Hazewinkel, Michiel, ed. (2001), "Gravitation, theory of", Encyclopedia of Mathematics, Springer, ISBN 9781556080104
The fundamental interactions of physics


Physical forces
 Strong interaction
 Weak interaction
 Electromagnetism
 Gravitation




Theories of gravitation


Standard 
Newtonian gravity (NG) 
 Newton's law of universal gravitation
 History of gravitational theory


General relativity (GR) 
 Introduction
 History
 Mathematics
 Resources
 Tests
 PostNewtonian formalism
 Linearized gravity
 ADM formalism



Alternatives to
general relativity 
Paradigms 
 Classical theories of gravitation
 Quantum gravity
 Theory of everything


Classical 
 Einstein–Cartan
 Bimetric theories
 Gauge theory gravity
 Teleparallelism
 Composite gravity
 f(R) gravity
 Massive gravity
 Modified Newtonian dynamics (MOND)
 Nonsymmetric gravitation
 Scalar–tensor theories
 Scalar–tensor–vector
 Conformal gravity
 Scalar theories
 Whitehead
 Geometrodynamics
 Induced gravity
 Tensor–vector–scalar
 Chameleon
 Pressuron


Quantisation 
 Euclidean quantum gravity
 Canonical quantum gravity
 Wheeler–DeWitt equation
 Loop quantum gravity
 Spin foam
 Causal dynamical triangulation
 Causal sets
 DGP model


Unification 
 Kaluza–Klein theory
 Supergravity


Unification and
quantisation 
 Noncommutative geometry
 Semiclassical gravity
 Superfluid vacuum theory
 String theory
 Mtheory
 Ftheory
 Heterotic string theory
 Type I string theory
 Type 0 string theory
 Bosonic string theory
 Type II string theory
 Little string theory
 Twistor theory


Generalisations /
Extensions of GR 
 Scale relativity
 Liouville gravity
 Lovelock theory
 (2+1)dimensional topological gravity
 Gauss–Bonnet gravity
 Jackiw–Teitelboim gravity



PreNewtonian theories
and Toy models 
 Aristotelian physics
 CGHS model
 RST model
 Mechanical explanations
 Fatio–Le Sage
 Entropic gravity
 Gravitational interaction of antimatter


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