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Momentum
Momentum

... In this chapter we begin our study of more realistic systems in which the objects are no longer point particles but have extension in space. Up until now we’ve generally limited ourselves to the dynamics of point masses, first in one dimension and then generalized to two and three dimensions. Indeed ...
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... In both cases your momentum will decrease to zero in the collision. Given that the time Dt of the collision is the same, then the force exerted on YOU will be the same!! If a truck is approaching at 30 mph, then you’d be better off hitting the wall in that case. On the other hand, if it’s only a mos ...
Chap.4 Conceptual Modules Fishbane
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... In both cases your momentum will decrease to zero in the collision. Given that the time Dt of the collision is the same, then the force exerted on YOU will be the same!! If a truck is approaching at 30 mph, then you’d be better off hitting the wall in that case. On the other hand, if it’s only a mos ...
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... If there are no dissipative forces like friction, the total energy is constant (the law of energy conservation). Since E is a constant we can relate the change in kinetic and potential energy as: ∆KE = −∆P E Work is a measure of energy transfer. In the absence of friction, when positive work is done ...
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Classical central-force problem



In classical mechanics, the central-force problem is to determine the motion of a particle under the influence of a single central force. A central force is a force that points from the particle directly towards (or directly away from) a fixed point in space, the center, and whose magnitude only depends on the distance of the object to the center. In many important cases, the problem can be solved analytically, i.e., in terms of well-studied functions such as trigonometric functions.The solution of this problem is important to classical physics, since many naturally occurring forces are central. Examples include gravity and electromagnetism as described by Newton's law of universal gravitation and Coulomb's law, respectively. The problem is also important because some more complicated problems in classical physics (such as the two-body problem with forces along the line connecting the two bodies) can be reduced to a central-force problem. Finally, the solution to the central-force problem often makes a good initial approximation of the true motion, as in calculating the motion of the planets in the Solar System.
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