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by: Mrs. Clemens Smitham

Astronomy SCI 1901A

Mrs. Clemens Smitham
Clayton State
GPA 3.79

Harold Banke

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Harold Banke
Class Notes
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This 3 page Class Notes was uploaded by Mrs. Clemens Smitham on Monday October 5, 2015. The Class Notes belongs to SCI 1901A at Clayton State University taught by Harold Banke in Fall. Since its upload, it has received 36 views. For similar materials see /class/219551/sci-1901a-clayton-state-university in Science at Clayton State University.

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Date Created: 10/05/15
Kepler s Laws of Planetary Motion 1 The orbit of each planet is an ellipse with the Sun at one focus 2 An imaginary line from the Sun to a planet sweeps out equal areas in equal times 3 The squares of the planets time periods are directly proportional to the cubes of their semimajor axes If 2f T22 D23 Newton s Laws of Motion 1 An object at rest or in uniform motion in a straight line will remain that way forever unless acted upon by a net external force Uniform means not speeding up or slowing down Net means the final total of several things together 2 The acceleration of an object is directly proportional to the net external force applied to it and inversely proportional to the object s mass 3 For every force there is an equal but opposite force Momentum Momentum is a measure of the inertia of a moving body Linear momentum is calculated as the product of a body s mass and its velocity momentum p m V Newton s lSt law of motion may be restated as In the absence of external net force a body s momentum remains constant Newton s 2nd law defines force in terms of the rate of change of momentum The faster a body s momentum changes the larger must be the force acting on it Newton s 3rd law tells us that in a set of colliding objects the collisions generate equal but opposite forces which change each object s momentum in opposite ways so that all changes in momentum cancel out and the set has the same final M momentum as its original total momentum Momentum is said to be conserved momentum is neither created nor destroyed and the total momentum in the Universe today is the same as it was a million years ago and the same as it will be a million years in the future This Law of Conservation of Momentum is one of the most basic laws of the Universe This law allowed Newton to picture the Universe as a giant mechanical clockwork In addition to linear momentum a second type of momentum is called angular momentum This represents the inertia of rotating and revolving objects angular momentum L m v r Examples Spinning top Skater Planet Solar nebula


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