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Relativistic Gravity and the Origin of Inertia and Inertial Mass arXiv
Relativistic Gravity and the Origin of Inertia and Inertial Mass arXiv

... Alfred Einstein was inspired by Mach’s principle. The General Theory of Relativity attempted to interpret inertia, considering that it is the gravitational effect of the whole Universe, but as pointed out by Einstein, it failed to do so [1]. Einstein showed that the field equation of General Relati ...
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... that the upper and lower boundaries are flat plates, and the upper one moves with a constant velocity in the x-direction, it is not unreasonable to guess that there is no dependence on, or motion in, the z-direction. In other words v = (u, v, 0), where u, v, and p are independent of z. In this case, ...
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... When body projected with initial velocity u by making angle  with the horizontal. Then after time t, (at point P) it’s direction is perpendicular to u . Magnitude of velocity at point P is given by v  u cot  . (from sample problem no. 9) For vertical motion : Initial velocity (at point O)  u sin ...
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... The car travels at a constant speed from the bottom A of the dip to the top B of the hump. If the radius of curvature of the road at A is ρA = 120 m and the car acceleration at A is 0.4g, determine the car speed v. If the acceleration at B must be limited to 0.25g, determine the minimum radius of cu ...
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N-body problem

In physics, the n-body problem is the problem of predicting the individual motions of a group of celestial objects interacting with each other gravitationally. Solving this problem has been motivated by the desire to understand the motions of the Sun, Moon, planets and the visible stars. In the 20th century, understanding the dynamics of globular cluster star systems became an important n-body problem. The n-body problem in general relativity is considerably more difficult to solve.The classical physical problem can be informally stated as: given the quasi-steady orbital properties (instantaneous position, velocity and time) of a group of celestial bodies, predict their interactive forces; and consequently, predict their true orbital motions for all future times.To this purpose the two-body problem has been completely solved and is discussed below; as is the famous restricted 3-Body Problem.
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