Centripetal Force r mv F 2 Suggested activity Carry out activities to

Centripetal force r mv f 2 suggested activity carry

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Centripetal Force, r mv F 2 Suggested activity: Carry out activities to understand centripetal force using a Centripetal Force Kit. Note: Objects that orbit the Earth will experience free fall toward the centre of the Earth. Satellite and planetary motion systems are circular motions which are constantly experiencing a centripetal acceleration, a where:
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KSSM PHYSICS FORM 4 65 CONTENT STANDARD LEARNING STANDARD NOTES v = linear velocity r = radius of orbit 3.1.6 Determine the mass of the Earth and the Sun using Newton ’s universal law of gravitation and centripetal force. Suggested activity: To determine the mass of the Earth and the Sun using: Newton s universal law of gravitation centripetal force: r mv F 2 speed of the Earth orbiting the Sun: where, r = average radius of orbit T = period of the Earth orbiting the Sun 2 E r mM G F T r 2 v π r v a 2
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KSSM PHYSICS FORM 4 66 CONTENT STANDARD LEARNING STANDARD NOTES 3.2 Kepler’s L aws Pupils are able to: 3.2.1 Explain Kepler’s Laws. Suggested activity: Sketch an elliptical shape based on the elliptical dual- focus concept using thread and pencil. Discuss that the elliptical orbits of the planets in the solar system are almost circular. Note: Kepler’s first l aw: All planets move in elliptical orbits, with the sun at one focus (Law of Orbits). Kepler’s second law: A line that connects a planet to the sun sweeps out equal areas in equal times (Law of Areas). Kepler’s third l aw: The square of the period of any planet is directly proportional to the cube of the radius of its orbit (Law of Periods).
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KSSM PHYSICS FORM 4 67 CONTENT STANDARD LEARNING STANDARD NOTES 3.2.2 Express Kepler’s Third Law T 2 r 3 Note: Derivation of the relationship is required. Kepler’s third l aw, T 2 r 3 can be derived from: Centripetal Force, r mv F 2 Gravitational Force, 2 r mM G F and, T r 2 v Thus, 3 2 2 )r GM 4 ( T π T 2 = k r 3 where the constant, GM 4 k 2 π Therefore , Kepler’s thrid law is expressed as T 2 r 3 , where, M is mass of the Sun; for the Sun and planetary system M is mass of the Earth; for the Earth and satelite system
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KSSM PHYSICS FORM 4 68 CONTENT STANDARD LEARNING STANDARD NOTES 3.2.3 Solve problems using Kepler’s Third Law Note: F rom Kepler’s third l aw: 3 2 3 1 2 2 2 1 r r T T For a planet that orbits the Sun; r = the distance between the center of the planet and the center of the Sun. For satellites orbiting the Earth; r = R + h (distance between center of Earth and satellite center) R = Earth radius = 6370 km h = satellite elevation from Earth's surface
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KSSM PHYSICS FORM 4 69 CONTENT STANDARD LEARNING STANDARD NOTES 3.3 Man-made Satellites Pupils are able to: 3.3.1 Describe how an orbit of a satellite is maintained at a specific height by setting the necessary satellite’s velocity.
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  • Fall '18
  • DR. MOHAMAD MARZUQI BIN ABDUL RAHIM

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