The gravitational attraction between the original gaseous matter in the
universe allowed it to
form stars which eventually condensed into galaxies, so gravity is responsible for many of the large-scale structures in the universe. Gravity has an infinite range, although its effects become weaker as objects get farther away.
The nature and mechanism of gravity was explored by a wide range of ancient scholars. In
Aristotle believed that objects fell towards the Earth because the Earth was the center of the Universe and attracted all of the mass in the Universe towards it. He also thought that the speed of a falling object should increase with its weight, a conclusion which was later shown to be false. While Aristotle's view was widely accepted throughout Ancient Greece, there were other thinkers such as
Plutarch who correctly predicted that the attraction of gravity was not unique to the Earth.
Although he didn't understand gravity as a force, the ancient Greek philosopher
Archimedes discovered the
center of gravity of a triangle. He also postulated that if two equal weights did not have the same center of gravity, the center of gravity of the two weights together would be in the middle of the line that joins their centers of gravity.Two centuries later, the Roman engineer and architect Vitruvius contended in his De architectura that gravity is not dependent on a substance's weight but rather on its "nature".
In the 6th century CE, the Byzantine Alexandrian scholar John Philoponus proposed the theory of impetus, which modifies Aristotle's theory that "continuation of motion depends on continued action of a force" by incorporating a causative force which diminishes over time.
In the ancient
Middle East, gravity was a topic of fierce debate. The
Al-Biruni believed that the force of gravity was not unique to the Earth, and he correctly assumed that other
heavenly bodies should exert a gravitational attraction as well. In contrast,
Al-Khazini held the same position as Aristotle that all matter in the Universe is attracted to the center of the Earth.
Leaning Tower of Pisa, where according to legend Galileo performed an experiment about the speed of falling objects
In the mid-16th century, various European scientists experimentally disproved the
Aristotelian notion that heavier objects
fall at a faster rate. In particular, the
Domingo de Soto wrote in 1551 that bodies in
free fall uniformly accelerate. De Soto may have been influenced by earlier experiments conducted by other Dominican priests in Italy, including those by
Benedetto Varchi, Francesco Beato,
Luca Ghini, and
Giovan Bellaso which contradicted Aristotle's teachings on the fall of bodies. The mid-16th century Italian physicist
Giambattista Benedetti published papers claiming that, due to
specific gravity, objects made of the same material but with different masses would fall at the same speed. With the 1586
Delft tower experiment, the
Simon Stevin observed that two cannonballs of differing sizes and weights fell at the same rate when dropped from a tower. Finally, in the late 16th century,
Galileo Galilei's careful measurements of balls rolling down
inclines allowed him to firmly establish that gravitational acceleration is the same for all objects. Galileo postulated that
air resistance is the reason that objects with a low density and high
surface area fall more slowly in an atmosphere.
In 1604, Galileo correctly hypothesized that the distance of a falling object is proportional to the
square of the time elapsed. This was later confirmed by Italian scientists
Riccioli between 1640 and 1650. They also calculated the magnitude of
the Earth's gravity by measuring the oscillations of a pendulum.
English physicist and mathematician, Sir
Isaac Newton (1642–1727)
In 1684, Newton sent a manuscript to
Edmond Halley titled De motu corporum in gyrum ('On the motion of bodies in an orbit'), which provided a physical justification for
Kepler's laws of planetary motion. Halley was impressed by the manuscript and urged Newton to expand on it, and a few years later Newton published a groundbreaking book called Philosophiæ Naturalis Principia Mathematica (Mathematical Principles of Natural Philosophy). In this book, Newton described gravitation as a universal force, and claimed 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." This statement was later condensed into the following inverse-square law:
where F is the force, m1 and m2 are the masses of the objects interacting, r is the distance between the centers of the masses and G is the
gravitational constant6.674×10−11 m3⋅kg−1⋅s−2..
Newton's Principia was well-received by the scientific community, and his law of gravitation quickly spread across the European world. More than a century later, in 1821, his theory of gravitation rose to even greater prominence when it was used to predict the existence of
Neptune. In that year, the French astronomer
Alexis Bouvard used this theory to create a table modeling the orbit of
Uranus, which was shown to differ significantly from the planet's actual trajectory. In order to explain this discrepancy, many astronomers speculated that there might be a large object beyond the orbit of Uranus which was disrupting its orbit. In 1846, the astronomers
John Couch Adams and
Urbain Le Verrier independently used Newton's law to predict Neptune's location in the night sky, and the planet was discovered there within a day.
Eventually, astronomers noticed an eccentricity in the orbit of the planet
Mercury which could not be explained by Newton's theory: the
perihelion of the orbit was increasing by about 42.98
arcseconds per century. The most obvious explanation for this discrepancy was an as-yet-undiscovered celestial body (such as a planet orbiting the Sun even closer than Mercury), but all efforts to find such a body turned out to be fruitless. Finally, in 1915,
Albert Einstein developed a theory of
general relativity which was able to accurately model Mercury's orbit.
In general relativity, the effects of gravitation are ascribed to
spacetimecurvature instead of a force. Einstein began to toy with this idea in the form of the
equivalence principle, a discovery which he later described as "the happiest thought of my life." In this theory, free fall is considered to be equivalent to inertial motion, meaning that free-falling inertial objects are accelerated relative to non-inertial observers on the ground. In contrast to
Newtonian physics, Einstein believed that it was possible for this acceleration to occur without any force being applied to the object.
Einstein proposed that spacetime is curved by matter, and that free-falling objects are moving along locally straight paths in curved spacetime. These straight paths are called
geodesics. As in Newton's first law of motion, Einstein believed that a force applied to an object would cause it to deviate from a geodesic. For instance, people standing on the surface of the Earth are prevented from following a geodesic path because the mechanical resistance of the Earth exerts an upward force on them. This explains why moving along the geodesics in spacetime is considered inertial.
Einstein's description of gravity was quickly accepted by the majority of physicists, as it was able to explain a wide variety of previously baffling experimental results. In the coming years, a wide range of experiments provided additional support for the idea of general relativity. Today, Einstein's theory of relativity is used for all gravitational calculations where absolute precision is desired, although Newton's inverse-square law continues to be a useful and fairly accurate approximation.
modern physics, general relativity remains the framework for the understanding of gravity. Physicists continue to work to find
solutions to the
Einstein field equations that form the basis of general relativity, while some scientists have speculated that general relativity may not be applicable at all in certain scenarios.
Einstein field equations
The Einstein field equations are a
system of 10
partial differential equations which describe how matter affects the curvature of spacetime. The system is often expressed in the form
An illustration of the Schwarzschild metric, which describes spacetime around a spherical, uncharged, and nonrotating object with mass
A major area of research is the discovery of
exact solutions to the Einstein field equations. Solving these equations amounts to calculating a precise value for the metric tensor (which defines the curvature and geometry of spacetime) under certain physical conditions. There is no formal definition for what constitutes such solutions, but most scientists agree that they should be expressable using
elementary functions or
linear differential equations. Some of the most notable solutions of the equations include:
Schwarzschild solution, which describes spacetime surrounding a
spherically symmetric non-
rotating uncharged massive object. For compact enough objects, this solution generated a
black hole with a central
singularity. At points far away from the central mass, the accelerations predicted by the Schwarzschild solution are practically identical to those predicted by Newton's theory of gravity.
Reissner–Nordström solution, which analyzes a non-rotating spherically symmetric object with charge and was independently discovered by several different researchers between 1916 and 1921. In some cases, this solution can predict the existence of black holes with double
Kerr solution, which generalizes the Schwarzchild solution to rotating massive objects. Because of the difficulty of factoring in the effects of rotation into the Einstein field equations, this solution was not discovered until 1963.
Kerr–Newman solution for charged, rotating massive objects. This solution was derived in 1964, using the same technique of complex coordinate transformation that was used for the Kerr solution.
Today, there remain many important situations in which the Einstein field equations have not been solved. Chief among these is the
two-body problem, which concerns the geometry of spacetime around two mutually interacting massive objects (such as the Sun and the Earth, or the two stars in a
binary star system). The situation gets even more complicated when considering the interactions of three or more massive bodies (the "n-body problem"), and some scientists suspect that the Einstein field equations will never be solved in this context. However, it is still possible to construct an approximate solution to the field equations in the n-body problem by using the technique of
post-Newtonian expansion. In general, the extreme nonlinearity of the Einstein field equations makes it difficult to solve them in all but the most specific cases.
Despite its success in predicting the effects of gravity at large scales, general relativity is ultimately incompatible with
quantum mechanics. This is because general relativity describes gravity as a smooth, continuous distortion of spacetime, while quantum mechanics holds that all forces arise from the exchange of discrete particles known as
quanta. This contradiction is especially vexing to physicists because the other three fundamental forces (strong force, weak force and electromagnetism) were reconciled with a quantum framework decades ago. As a result, modern researchers have begun to search for a theory that could unite both gravity and quantum mechanics under a more general framework.
Testing the predictions of general relativity has historically been difficult, because they are almost identical to the predictions of Newtonian gravity for small energies and masses. Still, since its development, an ongoing series of experimental results have provided support for the theory:
total solar eclipse provided one of the first opportunities to test the predictions of general relativity.
In 1919, the British astrophysicist
Arthur Eddington was able to confirm the predicted
gravitational lensing of light during
that year's solar eclipse. Eddington measured starlight deflections twice those predicted by Newtonian corpuscular theory, in accordance with the predictions of general relativity. Although Eddington's analysis was later disputed, this experiment made Einstein famous almost overnight and caused general relativity to become widely accepted in the scientific community.
In 1959, American physicists
Robert Pound and
Glen Rebka performed
an experiment in which they used
gamma rays to confirm the prediction of
gravitational time dilation. By sending the rays down a 74-foot tower and measuring their frequency at the bottom, the scientists confirmed that light is
redshifted as it moves towards a source of gravity. The observed redshift also supported the idea that time runs more slowly in the presence of a gravitational field.
In 1971, scientists discovered the first-ever black hole in the galaxy
Cygnus. The black hole was detected because it was emitting bursts of
x-rays as it consumed a smaller star, and it came to be known as
Cygnus X-1. This discovery confirmed yet another prediction of general relativity, because Einstein's equations implied that light could not escape from a sufficiently large and compact object.
General relativity states that gravity acts on light and matter equally, meaning that a sufficiently massive object could warp light around it and create a
gravitational lens. This phenomenon was first confirmed by observation in 1979 using the 2.1 meter telescope at
Kitt Peak National Observatory in Arizona, which saw two mirror images of the same quasar whose light had been bent around the galaxy
An initially-stationary object that is allowed to fall freely under gravity drops a distance that is proportional to the square of the elapsed time. This image spans half a second and was captured at 20 flashes per second.
Every planetary body (including the Earth) is surrounded by its own gravitational field, which can be conceptualized with Newtonian physics as exerting 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.
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.
The strength of the gravitational field is numerically equal to the acceleration of objects under its influence. The rate of acceleration of falling objects near the Earth's surface varies very slightly depending on latitude, surface features such as mountains and ridges, and perhaps unusually high or low sub-surface densities. 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).
The force of gravity on Earth is the resultant (vector sum) of two forces: (a) The gravitational attraction in accordance with Newton's universal law of gravitation, and (b) the centrifugal force, which results from the choice of an earthbound, rotating frame of reference. The force of gravity is weakest at the equator because of the
centrifugal force caused by the Earth's rotation and because points on the equator are furthest from the center of the Earth. The force of gravity varies with latitude and increases from about 9.780 m/s2 at the Equator to about 9.832 m/s2 at the poles. Canada's
Hudson Bay has less gravity than any place on Earth.
General relativity predicts that energy can be transported out of a system through gravitational radiation. The first indirect evidence for gravitational radiation was through measurements of the
Hulse–Taylor binary in 1973. This system consists of a pulsar and neutron star in orbit around one another. Its orbital period has decreased since its initial discovery due to a loss of energy, which is consistent for the amount of energy loss due to gravitational radiation. This research was awarded the Nobel Prize in Physics in 1993.
The first direct evidence for gravitational radiation was measured on 14 September 2015 by the
LIGO detectors. The gravitational waves emitted during the collision of two black holes 1.3 billion light years from Earth were measured. This observation confirms the theoretical predictions of Einstein and others that such waves exist. It also opens the way for practical observation and understanding of the nature of gravity and events in the Universe including the Big Bang.Neutron star and
black hole formation also create detectable amounts of gravitational radiation. This research was awarded the Nobel Prize in physics in 2017.
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. This means that if the Sun suddenly disappeared, the Earth would keep orbiting the vacant point normally for 8 minutes, which is the time light takes to travel that distance. The team's findings were released in Science Bulletin in February 2013.
In October 2017, the
LIGO and Virgo detectors received gravitational wave signals within 2 seconds of gamma ray satellites and optical telescopes seeing signals from the same direction. This confirmed that the speed of gravitational waves was the same as the speed of light.
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
Extra-fast 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 through gravitation but not electromagnetically, would account for the discrepancy. Various
modifications to Newtonian dynamics have also been proposed.
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, however this conclusion is disputed.
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 inverse-squared at certain distance scales.
Extra massive hydrogen clouds: The spectral lines of the
Lyman-alpha 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 inverse-squared at certain distance scales.
^Vitruvius, Marcus Pollio (1914).
"7". In Alfred A. Howard (ed.). De Architectura libri decem [Ten Books on Architecture]. VII. Herbert Langford Warren, Nelson Robinson (illus), Morris Hicky Morgan. Harvard University, Cambridge: Harvard University Press. p. 215.
^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."
^Hofmann-Wellenhof, B.; Moritz, H. (2006). Physical Geodesy (2nd ed.). Springer.
ISBN978-3-211-33544-4. § 2.1: "The total force acting on a body at rest on the earth's surface is the resultant of gravitational force and the centrifugal force of the earth's rotation and is called gravity.