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$\bullet$ Consult Appendix E. Calculate the radial acceleration (in $\mathrm{m} / \mathrm{s}^{2}$ and $g^{\prime} \mathrm{s}$ ) of an object (a) on the ground at the earth'sequator and (b) at the equator of Jupiter (which takes 0.41 day to spin once), turning with the planet.

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a) 0.0337 $\mathrm{m} / \mathrm{s}^{2}$$3.44 \times 10^{-3} g$b) 2.3 $\mathrm{m} / \mathrm{s}^{2}$0.23$g$

Physics 101 Mechanics

Chapter 3

Motion in a Plane

Physics Basics

Motion Along a Straight Line

Motion in 2d or 3d

Newton's Laws of Motion

University of Michigan - Ann Arbor

Simon Fraser University

University of Winnipeg

Lectures

03:28

Newton's Laws of Motion are three physical laws that, laid the foundation for classical mechanics. They describe the relationship between a body and the forces acting upon it, and its motion in response to those forces. These three laws have been expressed in several ways, over nearly three centuries, and can be summarised as follows: In his 1687 "Philosophiæ Naturalis Principia Mathematica" ("Mathematical Principles of Natural Philosophy"), Isaac Newton set out three laws of motion. The first law defines the force F, the second law defines the mass m, and the third law defines the acceleration a. The first law states that if the net force acting upon a body is zero, its velocity will not change; the second law states that the acceleration of a body is proportional to the net force acting upon it, and the third law states that for every action there is an equal and opposite reaction.

04:16

In mathematics, a proof is a sequence of statements given to explain how a conclusion is derived from premises known or assumed to be true. The proof attempts to demonstrate that the conclusion is a logical consequence of the premises, and is one of the most important goals of mathematics.

01:53

Consult Appendix E. Calcul…

03:13

$\bullet$ Consult Appendix…

02:07

Compute the centripetal ac…

02:51

Using Appendix F, along wi…

02:34

Using astronomical data fr…

02:23

The planet Jupiter rotates…

03:36

00:39

02:48

Find the angular velocity,…

02:45

(a) Compute the radial acc…

04:27

Calculate the following:

03:12

Using astronomical data in…

01:31

Consider points on the Ear…

04:33

The earth rotates once per…

So for party, we know that T equals 24 hours, which simply equals 86,400 seconds on. We know that the radius of the earth is going to be equal to 6.38 times 10 to the sixth meters. For part B. We know that ah t equals point for one of a day. So this will simply be ableto 35,424 seconds. And the radius here is equaling 7.18 times 10 to the seventh meters. Now, in order to find us a formula for the trust centripetal acceleration or the radio acceleration, we know that a SSA Brett is going to equal v squared the linear velocity divided by the radius. We know that the linear velocity is equal to the angular velocity Omega times, the radius. And we know that omega the angular velocity is equal to two pi divided by t the period. So if we were to substitute omega into the formula for a philosophy and then substitute that into the formula for the centripetal acceleration, we find that the radio looks in for the central blow till aeration is equal in for pi squared bar over t T Square brother. So at this point, we can say that for a party, the radio acceleration is going to be equal to four. Pi squared 6.38 times 10 to the sixth, divided by 86,400 squared No and this is giving us 0.337 meters per second squared. If we divide this by 9.8, we're getting 3.44 times 10 to the negative third G and for part B, we do the exact same calculation for pi squared times new radius of 7.18 times 10 to the seventh and then again divided by 35,424. And this is equaling 2.26 meters per second squared where we can say 0.230 g. So these will be your final answers. These are the explorations and meters per second. That is the end of the solution. Thank you for watching

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