Gravitation

In physics, gravitation or gravity is the tendency of objects with mass to accelerate toward each other, or, in other words, two masses attract each other. Gravitation is one of the four fundamental interactions in nature, the other three being the electromagnetic force, the weak nuclear force, and the strong nuclear force. Gravitation is the weakest of these interactions, but acts over great distances and is always attractive. In classical mechanics, gravitation is given by Newton's gravitational force, which is an inverse-square law. In general relativity, gravitation arises out of spacetime being curved by the presence of mass, and is not a force. In quantum gravity theories, either the graviton is the postulated carrier of the gravitational force, or time-space itself is envisioned as discrete in nature, or both.

Classically, the gravitational attraction of the earth endows objects with weight and causes them to fall to the ground when dropped. Moreover, gravitation is the reason for the very existence of the earth, the sun, and other celestial bodies; without it matter would not have coalesced into these bodies and life as we know it would not exist. Gravitation is also responsible for keeping the earth and the other planets in their orbits around the sun, the moon in its orbit around the earth, for the formation of tides, and for various other natural phenomena that we observe.

History of gravitational theory

Since the time of the Greek philosopher Aristotle in the 4th century BC, there have been many attempts to understand and explain gravity. Aristotle believed that there was no effect without a cause, and therefore no motion without a force. He hypothesized that everything tried to move towards their proper place in the crystalline spheres of the heavens, and that physical bodies fell toward the center of the Earth in proportion to their weight. Another example of an attempted explanation is that of the Indian astronomer Brahmagupta who, in 628 AD, wrote that "bodies fall towards the earth as it is in the nature of the earth to attract bodies, just as it is in the nature of water to flow".

In 1687, the English physicist and mathematician Sir Isaac Newton published the famous Principia, which hypothesizes the inverse-square 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 them answer pretty nearly." Most modern non-relativistic gravitational calculations are based on Newton's work.

Newton's law of universal gravitation

In 1687 Newton published his work on the universal law of gravity in his book Philosophiae Naturalis Principia Mathematica ( Latin:Mathematical Principles of Natural Philosophy). Newton’s law of gravitation states that: every particle in the universe attracts every other particle with a force that is directly proportional to the product of their masses and inversely proportional to the square of the distance between them. If the particles have masses m₁ and m₂ and are separated by a distance r (from their centers of gravity), the magnitude of this gravitational force is:

$F=G{\frac {m_{1}m_{2}}{r^{2}}}$

where:

F is the magnitude of the gravitational force between the two point masses

G is the gravitational constant

m₁ is the mass of the first point mass

m₂ is the mass of the second point mass

r is the distance between the two point masses

To see the change in gravity on earth based on the altitude (r in the above equation) based on real examples, you can use the eXtreme High Altitude Calculator

Gravitational potential

The above equation leads to the equation for the work done in moving a mass from infinity to a distance R, which is obtained by integrating the force of gravity:

$U_{g}(R)=\int _{\infty }^{R}{Gm_{1}m_{2} \over r^{2}}dr=-{Gm_{1}m_{2} \over R}$

and this is known as the gravitational potential energy, which has its zero point at infinity.

Using the Earth as an example, the work done in moving a mass from the Earth's surface to a distance h above the surface is given by:

$W(h)=\int _{r_{e}}^{r_{e}+h}{Gmm_{e} \over r^{2}}dr=-{\frac {Gmm_{e}}{r_{e}+h}}+{Gmm_{e} \over r_{e}}=-{\frac {Gmm_{e}}{r_{e}}}{\frac {h}{r_{e}+h}}=gmh{\frac {r_{e}}{r_{e}+h}},$

where G is the universal gravitational constant, m is the object's mass, r_e is the Earth's radius, and m_e is the Earth's mass. Further

$g\equiv {\frac {Gm_{e}}{r_{e}^{2}}},$

is the gravitational acceleration, g = 9.81 m/s² on earth. Taking unit mass m = 1 in the last equation, we obtain the classical gravitational field U(h) of the Earth, with the zero of potential for h = 0 (at the surface of the earth). Note that for small heights h = x the gravitational potential field is linear in the height,

$U(x)=gx\quad {\hbox{for}}\quad x\ll r_{e}.$

General relativity

Newton's conception and quantification of gravitation held until the beginning of the 20th century, when the German-born physicist Albert Einstein proposed the general theory of relativity. In this theory Einstein proposed that inertial motion occurs when objects are in free-fall instead of when they are at rest with respect to a massive object such as the Earth (as is the case in classical mechanics). The problem is that in flat spacetimes such as those of classical mechanics and special relativity, there is no way that inertial observers can accelerate with respect to each other, as free-falling bodies can do as they each are accelerated towards the center of a massive object.

To deal with this difficulty, Einstein proposed that spacetime is curved by the presence of matter, and that free-falling objects are following the geodesics of the spacetime. More specifically, Einstein discovered the field equations of general relativity, which relate the presence of matter and the curvature of spacetime. The Einstein field equations are a set of 10 simultaneous, non-linear, differential equations whose solutions give the components of the metric tensor of spacetime. This metric tensor allows to calculate not only angles and distances between space-time intervals (segments) measured with the coordinates against which the spacetime manifold is being mapped but also the affine-connection from which the curvature is obtained, thereby describing the spacetime's geometrical structure. Notable solutions of the Einstein field equations include:

• The 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.
• The Reissner-Nordström 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 solution for rotating massive objects. This solution also produces black holes with multiple event horizons.
• The cosmological Robertson-Walker solution, which predicts the expansion of the universe.

General relativity has enjoyed much success because of how its predictions have been regularly confirmed. For example:

• General relativity accounts for the anomalous precession of the planet Mercury.
• 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 Eddington in 1919, 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 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 the Robertson-Walker metric) was confirmed by Edwin Hubble in 1929.

Specifics

Earth's gravity

Every planetary body, including the Earth, is surrounded by its own gravitational field, which exerts an attractive force on any object that comes under its influence. This field is proportional to the body's mass and varies inversely with the square of distance from the body. 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 9.81 m/s² or 32.2 ft/s². This means that, ignoring air resistance, an object falling freely near the earth's surface increases in speed by 9.81 m/s (around 22 mph) for each second of its descent. Thus, an object starting from rest will attain a speed of 9.81 m/s after one second, 19.62 m/s after two seconds, and so on. 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. However, because the mass of the earth is huge, the acceleration produced on the earth by this same force is negligible.

Equations for a falling body

Under normal earth-bound conditions, when objects move owing to a constant gravitational force a set of kinematical and dynamical equations describe the resultant trajectories. For example, Newton’s law of gravitation simplifies to F = mg, where m is the mass of the body. This assumption is reasonable for objects falling to earth over the relatively short vertical distances of our everyday experience, but is very much untrue over larger distances, such as spacecraft trajectories, because the acceleration far from the surface of the Earth will not in general be g. A further example is the expression that we use for the calculation of potential energy of a body = mgh. This expression can be used only over small distances from the earth. Similarly the expression for the maximum height reached by a vertically projected body,"h = u^2/2g " 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.

Gravity and 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 and even the theory of dark matter. Although we haven't traveled to all the planets nor to the sun, we know their mass. The mass is 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.

Applications

A vast number of mechanical contrivances depend in some way on gravity for their operation. For example, a height difference can provide a useful pressure differential in a liquid, as in the case of an intravenous drip or a water tower. The gravitational potential energy of water can be used to generate hydroelectricity as well as to haul a tramcar up an incline, using a system of water tanks and pulleys; the Lynton and Lynmouth Cliff Railway [1] in Devon, England employs just such a system. Also, a weight hanging from a cable over a pulley provides a constant tension in the cable, including the part on the other side of the pulley to the weight.

Examples are numerous: For example molten lead, when poured into the top of a shot tower, will coalesce into a rain of spherical lead shot, first separating into droplets, forming molten spheres, and finally freezing solid, undergoing many of the same effects as meteoritic tektites, which will cool into spherical, or near-spherical shapes in free-fall. Also, a fractionation tower can be used to manufacture some materials by separating out the material components based on their specific gravity. Weight-driven clocks are powered by gravitational potential energy, and pendulum clocks depend on gravity to regulate time. Artificial satellites are an application of gravitation which was mathematically described in Newton's Principia.

Gravity is used in geophysical exploration to investigate density contrasts in the subsurface of the Earth. Sensitive gravimeters use a complicated spring and mass system (in most cases) to measure the strength of the "downward" component of the gravitational force at a point. Measuring many stations over an area reveals anomalies measured in mGal or microGal (1 gal is 1 cm/s^2. Average gravitational acceleration is about 981 gal, or 981,000 mGal.). After corrections for the obliqueness of the Earth, elevation, terrain, instrument drift, etc., these anomalies reveal areas of higher or lower density in the crust. This method is used extensively in mineral and petroleum exploration, as well as time-lapse groundwater modeling. The newest instruments are sensitive enough to read the gravitational pull of the operator standing over them.

Alternative theories

Historical alternative theories

• Aristotelian theory of gravity
• Le Sage's theory of gravitation (1784) also called LeSage gravity, proposed by Georges-Louis Le Sage, based on a fluid-based 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 theories

• Brans-Dicke 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 bi-metric 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 new and highly controversial Process Physics theory attempts to address gravity
• The self-creation cosmology theory of gravity (1982) by G.A. Barber in which the Brans-Dicke theory is modified to allow mass creation.
• Nonsymmetric gravitational theory (NGT) (1994) by John Moffat
• The satirical theory of Intelligent falling (2002, in its first incarnation as "Intelligent grappling")
• Tensor-vector-scalar gravity (TeVeS) (2004), a relativistic modification of MOND by Jacob Bekenstein

electrogavitics, magnetogravitics, gravity wave harmonics: electrogravitics: (eg. see books published by integrity research institute [2]) basic principle: electrons push, protons pull - using this principle, Nikola Tesla predicted gravitational repulsion in the 1880s, experimented with it in the 1890s, & designed the cigar shaped aircraft in the early 20th century. The Biefeld-Brown effect (1923) demonstrates this & Thomas Townsend Brown later designed asymetric capacitors suchas the disc shaped aircraft with a negatively electrical charged (repulsion) plate on the bottom & the positively charged (attraction) plate on top. gravity wave harmonics (eg. see book: How to Build a Flying Saucer and Other Proposals in Speculative Engineering, T.B. Pawlicki): gravity is a wave like any other - all the planets rest at harmonic intervals in a standing wave from the source of the wave, the sun.

See also

• Artificial gravity
• Escape velocity
• General relativity
• Gravitational radiation (gravitational waves)
• Gravitational binding energy
• Gravity Research Foundation
• Gravity and the divergence theorem
• Kepler's third law of planetary motion
• Newton's laws of motion
• n-body problem
• The Pioneer spacecraft anomaly
• Scalar Gravity
• Speed of gravity
• Standard gravitational parameter
• Weight
• Weightlessness

Notes

• 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 0-520-08816-6 ISBN 0-520-08817-4
• 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.)

References

1. Halliday, David; Robert Resnick; Kenneth S. Krane (2001). Physics v. 1. New York: John Wiley & Sons. ISBN 0-471-32057-9. 
2. Serway, Raymond A.; Jewett, John W. (2004). Physics for Scientists and Engineers, 6th ed.. Brooks/Cole. ISBN 0-534-40842-7. 
3. Tipler, Paul (2004). Physics for Scientists and Engineers: Mechanics, Oscillations and Waves, Thermodynamics, 5th ed.. W. H. Freeman. ISBN 0-7167-0809-4. 
4. Jefimenko, Oleg D., "Causality, electromagnetic induction, and gravitation : a different approach to the theory of electromagnetic and gravitational fields". Star City [West Virginia] : Electret Scientific Co., c1992. ISBN 0-917406-09-5
5. Heaviside, Oliver, "A gravitational and electromagnetic analogy". The Electrician, 1893.

External links

• Gravity Probe B Experiment The Official Einstein website from Stanford University
• Center for Gravity, Electrical, and Magnetic Studies