The Movement of planet I (hukun kepler).pptx

Penjelasan ttg Hukun Kepler, Hukum Newton dan aplikasinya

1. The Movement of Planet I (Kepler’s Law, Newton’s Law, and It’s Aplication)

2. Group V Ni Luh Putu Novidyantari NIM. 1613021005 Gusti Ayu Putu Ulan Parwati NIM. 1213021023 Ni Kadek Risma Windi Sulastri NIM. 1213021033 Ida Ayu Diah Cahya Utami NIM. 1213021048 The Movement of Planet I (Kepler’s Law, Newton’s Law, and It’s Aplication)

3. Newton's Law of Motion and Gravity Kepler’s I Law Kepler’s II Law Kepler’s III Law General Gravity Law

4. Figure. cone slices

5. Kepler’s I Law AC = a = half of the long axis CD = b = half of the short axis A = luas elips = ab The formula :

6. Kepler’s II Law

7. for very small displacements :

8. Kepler’s III Law According to Newton II law, the magnitude of force is F = m. A. From these two equations we get:

9. When the planet's orbital period is T and velocity v, this means is fixed so that equation can be written to be: For a certain planet the price

10. General Gravity Law Where G is a constant called general gravity. By entering the price k of equation

11. Next the equation of Kepler’s III Law we can written

12. Geocentric and Heliocentric Views

13. ptolomecus view which views the earth as the center of nature the universe is called the geocentric view. According to geocentric theory, Earth is the center of the universe that is in a state of silence. While the planets, the Sun, and other heavenly bodies move around it.

14. The idea of ​​this heliocentric theory emerged around the year (1473-1543) by Nicolaus Copernicus, a Polish astronomer. According to the theory of solar heliocentris is the center of the solar system where the stars are located on the spacecraft and spin around the sun. Among the Stars and the Sun there are planets including the Earth that also revolve around the Sun in each of its orbits by a circular orbit of the path, as shown in FIG

15. But Tycho brahe (1546-1601), opposes the heliocentric view of copernicus , and returns to a geocentric view. Tycho considers that when the earth and the planet circulate around the sun there will be symptoms of star's paraklasis , but he has never observed any symptom of paraklasis of stars, therefore he opposes the heliocentric theory. In fact, Tycho's failure to observe parallax is due to the lack of a reflection of the tools used at that time.

16. Applications Of Kepler's Law And Newton's Law

17. Measuring Earth-Sun Distance The latest way to determine the distance of the earth to the sun is done by measuring the distance of Venus by using radar waves. The average distance of the earth-sun is called an astronomical unit or with 1 SA. Suppose the orbit of Venus and the earth is a circle. From the observation has been known that the period of Earth orbit T = 365.25 days with period Venus T = 224.70 days. Geometrically can be derived according to Kepler III law as shown below. θ a v d a B

18. Since the period of Earth and Venus are known then the value of aB can be calculated. From the picture above seen angle θ is the angle of distance of Venus to the sun seen from the earth. Magnitude angle θ can be determined at any time by using theodolite. To determine the aB price of the above equation we only specify the price d ie the Earth-Venus distance, which is usually determined by measuring the reflection of radar waves sent to Venus. From the observation result, the average distance of earth-sun is 1.49x1011 m or 1 SA = 1,5 x 1011 m.

19. Determining the Sun Mass From the equation, if R and T are known then we can calculate the mass of the sun. By taking: Earth period T = 1 year = 3.16 x 107 second; Earth-sun distance R = 150 x 106 km = 1.5 x 1011m; and G = 6.67 x 10-11 Nm2 / kg2. Then M sun = (4π2 / T2) R3 M sun = 2.0 x 1030 kg. Determining the Earth Mass By knowing: month period Tm = 27.3 days = 2.36x106s Earth-moon distance Rm = 384 x 103km = 3.84 x 108m Then the mass of the earth Mbumi can be searched from the formula M earth = (4π2 / T2) R3 By entering the prices of G, Rm , and Tc into this equation, the earth mass is obtained M earth 6.02 x1024kg

20. ORBIT SPEED

21. A. AREA VELOCITY AND ENERGY EQUATION To determine the velocity of a planet at any point in its orbit, this can be seen from the elliptical motion of the planet's orbit.

22.   T P   P’   S F Gambar X  t

23.   SPP’ = h =1/2 PP’.ST     AREAL SPEED IN P IS      

24.   By entering the equation into the equation above then This equation is called the energy equation   When the energy equation is multiplied by ½ m, it will be obtained:  

25. This energy equation can also be viewed from a two mass system that revolves around a common mass center such as on a solar-planet system.     r B r2 A A’ B’ m M  

26. When the orbit velocity m and M is V1 and V2, then the magnitude of the centripetal force at m is   And for the object M the magnitude of the centrifugal force is   if both equations are added then  

27. For the period of planet T then   Then the equation of Kepler II law is obtained   Or  

28. Then obtain the energy equation as follows   For the earth-sun where m the mass and the sun mass M can be viewed m<<M so that M can be ignored, the energy equation will return to equation This applies to any orbiting object system whose mass is much smaller than the mass of the object around it.  

29. B. CIRCULAR ORBIT AND SPEED OFF being   When the parabola orbit then so  

30. Because then   Thus the orbital shape of an object being launched is like a satellite, ballistic missile or a spacecraft will depend on its speed. Suppose a celestial body at distance r speed v, then when: V< Vc orbit will be an ellipse V= Vc the orbit will be a circle V< Ve the orbit will be a parabola V> Ve orbit will be a hyperbola

31. Picture above is the motion of a rocket fired from a height b from the face of the earth at velocity v: a.The ellipse falls to earth b.Circle c. Elliptical orbit, and d. Parabola d c BUMI b V C V e

32. By taking the earth’s r then obtained freelance speed on earth is