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Chapter5
Chapter5

... 1. Make a rough sketch of the problem, if there is not already one supplied as part of the problem, and identify the object(s) whose motion is to be studied, if that is not clear. 2. Identify all the forces acting on the object (and only on that object) by constructing a carefully labeled external f ...
NEWTON`S FIRST LAW
NEWTON`S FIRST LAW

... walking, or a car smashing into a wall (think about what happens to the car!). IV. Finally draw an object in motion and indicate its momentum. Write the formula for momentum above the drawing. Momentum = kg x m/s. Label your object’s mass and its velocity, and give it direction. For example you coul ...
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Chapter 13 - Gravitation

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Chapter 6 The Gravitational Force and the Gravitational Field

... Observations Regarding Universal Gravitation 1. The force acts over all space. Every object in the universe feels gravity from every other object in the universe. 2. Force is proportional to mass. 3. The force that one object feels from another is equal and opposite to the force the other object fe ...
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... Gravitation • Gravitational force is… – directly proportional to the product of the masses of the two bodies – inversely proportional to the square of the distance between the centers of the two masses – If the objects are large (e.g. planets, moons) then the radii would be included in r ...
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Forces - Solon City Schools

PhyzSpringboard: Newton`s Second Law Felix
PhyzSpringboard: Newton`s Second Law Felix

... 2. a.The following is a statement of Newton’s second law of motion (although it’s not the one he stated in the Principia). ...
Study Guide For Final File
Study Guide For Final File

... 2. Define macroscopic as it relates to systems studied in Physics. (p.6) 3. A variable is a factor that affects the behavior of the system. Please define and give an example of the following: a) independent variable and b) dependent variable. (p.8) 4. Please describe how matter and mass are not the ...
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Mongar Higher Secondary School

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TAKS Obj 5

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Physics 132, Midterm Exam #1, April 27, 2010 Page Score _______

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Physics CPA Midterm Review Guide Midterm Topics (percentages

... b) What is the orbital velocity and orbital period of a satellite that orbits at a distance 3x earth radius from the earth’s surface? v = 3850 m/s, T = 2.89 hours ...
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Chap. 12 P.P - Moline High School

... Both are independent of each other. a. horizontal motion -force stays constant b. vertical motion -pulling it down at a rate of 9.8 m/s2 ...
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PHYS 1443 – Section 501 Lecture #1

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Chapter 12: Gravitation

... Earlier in the course, we talked about the fact that the net gravitational force on an object is called the weight of the object, and we wrote this as Fgrav = w = mg , in which g = 9.81 m/s 2 near the surface of the Earth. Also, we discussed gravitational potential energy, U grav ≡ mgy , near the su ...
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Newton`s Second Law.

... vector. Apart from examples and applications, which we will get to shorlty, there is a lot going on “under the hood” in Newton’s second law which we need to discuss. First of all, let us deal with a common mental mistake made by beginners. It is perhaps tempting to read Newton’s second law as a lite ...
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Work, Power, and Energy

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Gravitational Fields (AIS) - Atlanta International School Moodle

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Dynamics of the Elastic Pendulum

... • Thanks to our mentor Joseph Gibney for getting us started on the MATLAB program and the derivations of equations of motion. • Special thanks to Dr. Peter Lynch of the University College Dublin, Director of the UCD Meteorology & Climate Centre, for emailing his M-file and allowing us to include vid ...
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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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