| Home. | Universe Galaxies And Stars Archives. | | |
| Universe | Big Bang | Galaxies | Stars | Solar System | Planets | Hubble Telescope | NASA | Search Engine | | |
Newton's developed three main laws to explain his theories. |
Isaac Newton's theory of universal gravitation (part of classical mechanics) states the following: Every single point mass attracts every other point mass by a force pointing along the line combining the two. The force is proportional to the product of the two masses and inversely proportional to the square of the distance between the point masses:
Assuming SI units, F is measured in newtons (N), m_{1} and m_{2} in kilograms (kg), r in metres (m), and the constant G is approximately equal to 6.67 × 10^{-11} N m^{2} kg^{-2}. G was first accurately measured in the Cavendish experiment by the British scientist Henry Cavendish in 1798, it was also the first test of Newton's theory of gravitation between masses in the laboratory. This was 111 years after the publication of "Philosophiae Naturalis Principia Mathematica" and 71 years after Newton's death, so all of Newton's calculations could not use the value of G; instead he could only calculate a force relative to another force. Newton's law of gravitation resembles Coulomb's law of electrical forces. Newton's law is used to calculate the Gravitational force between two masses; similarly Coulomb's Law is used to calculate the magnitude of electrical force between two charged bodies. Coulomb's Law's equation has the product of two charges in place of the product of the masses which is in Newton's Law of Gravitation. Hence, according to Coulomb's Law, the electrical force is proportional to the product of the charged bodies divided by the distance between them. Acceleration due to gravity Let a_{1} be the acceleration due to gravity experienced by the first point mass. Newton's second law states that F = m_{1} a_{1}, meaning that a_{1} = F / m_{1}. Substituting F from the earlier equation gives: and similarly for a_{2}. Assuming SI units, gravitational acceleration (as acceleration in general) is measured in metres per second squared (m/s^{2} or m s^{-2}). Non-SI units include galileos, gees (see later), and feet per second squared. The force attracting a mass to the earth also attracts the earth to the mass, so that their acceleration to each other is given by: If m_{1} is negligible compared to m_{2}, small masses would have approximately the same acceleration. However, for appreciably large m_{1}, the combined acceleration, should be considered. If r changes proportionally very little during an object's travel - such as an object falling near the surface of the earth - then the acceleration due to gravity appears very nearly constant (see also Earth's gravity). Across a large body, variations in r, and the consequent variation in gravitational strength, can create a significant tidal force. For example, the near and far side of the earth are around 6,350 km different distance from the Moon; although a small difference compared to the 385,000 km average separation, this is enough to cause a slightly different gravitational force by the moon on the earth's oceans on each side compared to that exercised on the earth itself, and hence give rise to the tides. Bodies with spatial extent If the bodies in question have spatial extent (rather than being theoretical point masses), then the gravitational force between them is calculated by summing the contributions of the notional point masses which constitute the bodies. In the limit, as the component point masses become "infinitely small", this entails integrating the force (in vector form, see below) over the extents of the two bodies. In this way it can be shown that an object with a spherically-symmetric distribution of mass exerts the same gravitational attraction on external bodies as if all the object's mass were concentrated at a point at its centre. (This is not generally true for non-spherically-symmetrical bodies.) For points inside a spherically-symmetric distribution of matter, Newton's Shell theorem can be used to find the gravitational force. The theorem tells us how different parts of the mass distribution affect the gravitational force measured at a point located a distance r_{0} from the center of the mass distribution:
As a consequence, for example, within a shell of uniform thickness and density there is no net gravitational acceleration. Newton's laws of universal gravitation: Vector form. Newton's law of universal gravitation can be written as a vector equation to account for the direction of the gravitational force as well as its magnitude. In this formula, quantities in bold represent vectors. where
It can be seen that the vector form of the equation is the same as the scalar form given earlier, except that F is now a vector quantity, and the right hand side is multiplied by the appropriate unit vector. Also, it can be seen that F_{12} = - F_{21}. Gravitational field. The gravitational field is a vector field that describes the gravitational force which would be applied on an object in any given point in space, per unit mass. It is actually equal to the gravitational acceleration at that point. It is a generalization of the vector form, which becomes particularly useful if more than 2 objects are involved (such as a rocket between the Earth and the Moon). For 2 objects (e.g. object 2 is a rocket, object 1 the Earth), we simply write instead of and m instead ofm_{2} and define the gravitational field as: so that we can write: This formulation is dependent on the objects causing the field. The field has units of acceleration; in SI, this is m/s^{2}. Gravitational fields are also conservative; that is, the work done by gravity from one position to another is path-independent. This has the consequence that there exists a gravitational potential field V(r) such that
If m_{1} is a point mass or the mass of a sphere with homogeneous mass distribution, the force field g(r) outside the sphere is isotropic, i.e., depends only on the distance r from the center of the sphere. In that case Problems with Newton's theory. Newton's description of gravity is sufficiently accurate for many practical purposes and is therefore widely used. Deviations from it are small when the dimensionless quantities f/c^{2} and (v/c)^{2} are both much less than one, where f is the gravitational potential, v is the velocity of the objects being studied, and c is the speed of light. For example, Newtonian gravity provides an accurate description of the Earth/Sun system, since where r_{orbit} is the radius of the Earth's orbit around the Sun. In situations where either dimensionless parameter is large, then General relativity must be used to describe the system. General relativity reduces to Newtonian gravity in the limit of small potential and low velocities, so Newton's law of gravitation is often said to be the low-gravity limit of general relativity. Newton's laws of universal gravitation: Theoretical concerns.
Newton's laws of universal gravitation: Disagreement with observation.
The observed fact that gravitational and inertial masses are the same for all bodies is unexplained within Newton's system. General relativity takes this as a postulate. See equivalence principle. Newton's laws of universal gravitation: Newton's reservations. While Newton was able to formulate his law of gravity in his monumental work, he was deeply uncomfortable with the notion of "action at a distance" which his equations implied. He never, in his words, "assigned the cause of this power". In all other cases, he used the phenomenon of motion to explain the origin of various forces acting on bodies, but in the case of gravity, he was unable to experimentally identify the motion that produces the force of gravity. Moreover, he refused to even offer a hypothesis as to the cause of this force on grounds that to do so was contrary to sound science. He lamented that "philosophers have hitherto attempted the search of nature in vain" for the source of the gravitational force, as he was convinced "by many reasons" that there were "causes hitherto unknown" that were fundamental to all the "phenomena of nature". These fundamental phenomena are still under investigation and, though hypotheses abound, the definitive answer is yet to be found. In Newton's 1713 General Scholium in the second edition of Principia:
Newton's laws of universal gravitation: Einstein's solution. These objections were mooted by Einstein's theory of General relativity, in which gravitation is an attribute of curved spacetime instead of being due to a force propagated between bodies. In Einstein's theory, masses distort spacetime in their vicinity, and other particles move in trajectories determined by the geometry of spacetime. This allowed a description of the motions of light and mass that was consistent with all available observations. Newton's theory continues to be used as an excellent approximation of the effects of gravity. Relativity is only required when there is a need for extreme accuracy, or when dealing with gravitation for very massive objects. Go To Print Article |
Universe - Galaxies and Stars: Links and Contacts |
| GNU License | Contact | Copyright | WebMaster | Terms | Disclaimer | Top Of Page. | |