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Chapter 2 Newtonian Mechanics I
Chapter 2 Newtonian Mechanics I

Model Four
Model Four

Parallel Axis Theorem, Torque
Parallel Axis Theorem, Torque

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Lecture2_FreeFall

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Gravity and Inertia (Rec. 1.23.14) (* file)

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... that I = ICM + 4ML2/9. Figure P10.28b shows the same object in a different orientation. Demonstrate that the moment of inertia of the triangular plate, about the y axis is Ih = ICM + ML2/9. Demonstrate that the sum of the moments of inertia of the triangles shown in parts (a) and (b) of the figure m ...
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... • If there is no change in object’s energy, then no work is done on the object. • Applies to potential energy: For a barbell held stationary, no further work is done  no further change in energy. • Applies to decreasing energy: The more kinetic energy something has  the more work is required to sl ...
Hewitt/Lyons/Suchocki/Yeh, Conceptual Integrated Science
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611: Electromagnetic Theory II

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Laws Of Motion - Physics With Pradeep

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Department of Natural Sciences

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Calculus-Based Physics I

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2012-JJC-PH-H2-P2-Prelim

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Chapter 5 - Stress in Fluids
Chapter 5 - Stress in Fluids

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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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