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[1] [2] [3] This is a general physical law derived from empirical observations by what Isaac Newton called inductive reasoning. [4] It is a part of classical mechanics and was formulated in Newton's work Philosophiæ Naturalis Principia Mathematica ("the Principia"), first published on 5 July 1687.
Newton's laws are often stated in terms of point or particle masses, that is, bodies whose volume is negligible. This is a reasonable approximation for real bodies when the motion of internal parts can be neglected, and when the separation between bodies is much larger than the size of each.
In the spherical-coordinates example above, there are no cross-terms; the only nonzero metric tensor components are g rr = 1, g θθ = r 2 and g φφ = r 2 sin 2 θ. In his special theory of relativity , Albert Einstein showed that the distance ds between two spatial points is not constant, but depends on the motion of the observer.
[2] [3] The Principia is considered one of the most important works in the history of science. [4] The French mathematical physicist Alexis Clairaut assessed it in 1747: "The famous book of Mathematical Principles of Natural Philosophy marked the epoch of a great revolution in physics. The method followed by its illustrious author Sir Newton ...
Sir Isaac Newton (/ ˈ nj uː t ən /; 4 January [O.S. 25 December] 1643 – 31 March [O.S. 20 March] 1727) [a] was an English polymath active as a mathematician, physicist, astronomer, alchemist, theologian, and author. [5] Newton was a key figure in the Scientific Revolution and the Enlightenment that followed. [6]
Traditionally the Newton–Euler equations is the grouping together of Euler's two laws of motion for a rigid body into a single equation with 6 components, using column vectors and matrices. These laws relate the motion of the center of gravity of a rigid body with the sum of forces and torques (or synonymously moments ) acting on the rigid body.
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Corollary 2 shows that, putting this in another way, the centripetal force is proportional to (1/P 2) * R where P is the orbital period. Corollary 3 shows that if P 2 is proportional to R, then the centripetal force would be independent of R. Corollary 4 shows that if P 2 is proportional to R 2, then the centripetal force would be proportional ...