PPT - JOHANNES KEPLER Presentatiton.pptx

Physical Science

1. GOOD MORNING STUDENTS PRESENTED BY: WILIEMAR P. DELOS REYES

2. 4 PICS 1 WORD

3. WHAT IS THIS? O _ B _ T

4. WHAT IS THIS? O R B I T

5. WHAT IS THIS? M _ T _ O _

6. WHAT IS THIS? M O T I O N

7. WHAT IS THIS? C _ L _ U _ A _ I _ N

8. WHAT IS THIS? C A L C U L A T I O N

9. WHAT IS THIS? A _ _ A

10. WHAT IS THIS? A R E A

11. WHAT IS THIS? T _ _ E

12. WHAT IS THIS? T I M E

13. NumbLetWord In this activity, the teacher gives participants puzzle pieces describing each law and Kepler’s short information about his life (mixed up) to every group in the envelope. The student’s task is to arrange the puzzle pieces to form a definition of each law and information about Johannes Kepler within 3 minutes.

14. Guided Questions: 1. Was the activity difficult and interesting? 2. What phrases did you create? 3. What did you observe during our activity?

15. Johannes Kepler generated his three laws of planetary motion: law of ellipses (first law), the law of equal areas (second law), and the law of periods (third law).

16. • First law of planetary motion states the orbit of planet is an ellipse, with the sun located at one of the foci (sing. focus). - The shape of an ellipse is describe by its eccentricity, which is measure of how deviated the elliptical orbit is from being a circle. The point at which the planet is farthest from the sun is called aphelion , while the point at which the planet is nearest to the sun is called perihelion.

17. • Second law of planetary motion states that the imaginary line segment connecting a planet to the sun sweeps out equal time intervals. - The second law also implies that the motion of the planet moves fastest at the perihelion and slowest at the aphelion.

18. Third law of planetary motion states that the square of the time it takes for the planet to make one revolution around the sun ( also called the orbital period )is directly proportional to the cube of the semimajor axis of the planet’s elliptical orbit. Where T represents the orbital period of a planet (1 or 2) and a refers to the length of the semimajor axis.

19. Calculate the distance of unknown planet having the same eccentricity as that of Earth. Its orbital period is 20 years. Given: Let T1 represent Earth’s orbital period; T1 = 1 year. Let a1 represent the distance of Earth from the sun; a1 = 1.496x1011 m. The orbital period of the unknown planet can be written as = .  

20. For example:

21. QUESTION! Why is Johannes Kepler's contribution to astronomy still important today?

22. Directions: Read very carefully the following statements and choose the best answer from the given choices. 1. According to Kepler’s First Law, what is the shape of a planet’s orbit around the Sun? A) Circular B) Elliptical C) Spiral D) Rectangular 2. Kepler’s Second Law states that a planet moves fastest when it is ______. A) Farthest from the Sun (aphelion) B) Closest to the Sun (perihelion) C) Moving in a straight line D) Orbiting in a perfect circle

23. 3. Kepler’s Third Law relates which two properties of a planet’s orbit? A) Speed and distance B) Mass and gravity C) Orbital period and average distance from the Sun D) Temperature and brightness 4. What is the mathematical relationship expressed in Kepler’s Third Law? A) T² = R³ B) F = ma C) E = mc² D) V = IR 5. How did Kepler’s laws contribute to modern science? A) They helped prove the Earth is the center of the universe. B) They explained the motion of planets and supported Newton’s laws of gravity. C) They suggested planets move in unpredictable paths. D) They replaced Galileo’s discoveries entirely.

24. Assignment: [email protected] [phone] WWW.REALLYGREATSITE.COM Instructions: Answer the following equation based on Kepler’s third law of planetary motion. Write your answer on ½ sheet of yellow paper. Compute the constant of proportionality of Kepler's third law (T^2/a^3 ) in terms of Earth's semimajor axis and period. Earth's semimajor axis is 1.496x1011 m. Predict the time for Mars to orbit the sun if the average orbital distance of Mars is 1.52 times Earth's average orbital distance.

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