Presentation Transcript

1. Chapter 13

   Universal Gravitation
2. Intro Prior to 1687- Vast amounts of data collected on planetary motion. Little understanding of the forces involved 1687 and after Newton publishes the PhilosophiæNaturalisPrincipiaMathematica Law of Gravity is applied “Universally”
3. 13.1 Newton’s Law of Universal Gravitation Newton’s Law of Universal gravitation was the first time “earthly” and “heavenly” motions were unified. The Law states- Every particle in the Universe attracts every other particle with a force that is directly proportional to the product of their masses and inversely proportional to the square of the distance between them.
4. 13.1 or G is the universal gravitational constant G = 6.673 x 10-11 N.m2 / kg2 The second equation indicates the force is attractive (opposite of the radial vector) One example of an “Inverse Square Law”
5. 13.1 Law of gravity describes an action reaction pair, both objects acted on by equal and opposite forces. Also for spherical mass distributions, the force of gravity is the same as if all mass was concentrated at the center.
6. 13.1 Quick Quizzes pg 392 Example 13.1
7. 13.2 Measuring the Gravitation Constant Henry Cavendish (1798) Two small masses attached by a rod, hung by a thin wire. Two large masses, in fixed positions. Light deflection from mirror is measured Repeated with different masses
8. 13.3 Free Fall Accleration On the surface of the earth the force of gravity is defined as Applying universal gravitation we can determine the free fall acceleration anywhere.
9. 13.3 Using earth for example, and the falling object as mass 2. Mass 2 cancels (as it should)
10. 13.3 And for Altitudes above the surface The force of gravity decreases with altitude. As RE + h approaches ∞, mg approaches zero. Quick Quiz pg 395 Examples 13.2, 13.3
11. 13.4 Kepler’s Laws and the Motion of Planets Observation of the moon, planets, and stars has taken place for thousands of years. Early astronomers considered the universe to be Geocentric, formalized in the Ptolemaic Model (Claudius Ptolemy, 100-170 AD).
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13. 13.4 In 1543, Nicolaus Copernicus (1473-1543) establishes the 1st comprehensive Heliocentric Model where the planets revolve about the sun. (The Copernican Model)
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15. 13.4 Tycho Brahe (1546-1601) set out to determine how the heavens were constructed, so developed a system to determine accurate locations for the visible planets and over 700 stars using only a sextant and a compass.
16. 13.4 Brahe died before he could finish his observations and fully develop the Tychonic System, but he passed on the volumes of data collected to his assistant, Johannes Kepler.
17. 13.4 Johannes Kepler(1571-1630) using Brahe’s data (specifically for Mars about the Sun) Developed a model for Planetary motion, stated in three simple laws.
18. 13.4 Kepler’s Laws All planets move in elliptical orbits with the sun at one focus. (Elliptical Orbits) The radius vector drawn from the sun to a planet sweeps out equal areas in equal time intervals. (Equal Area in Equal Time) The square of the orbital period of any planet is proportional to the cube of the semimajor axis of the elliptical orbit. (_______)
19. 13.4 Kepler’s 1st Law- Circular orbits are only a special case, elliptical are the general case. On ellipses- curved where the total distance to two Focal points in is a constant. (r1 + r2) = constant
20. 13.4 The long axis through the center and foci is the major axis (2a), and distance to the center is the semimajor axis (a). The short axis through the center is the minor axis (2b) and the distance to the center is the semiminor axis (b)
21. 13.4 The eccentricity of the ellipse is defined as Where c is the distance the focal points to the center. As b decreases, c increases. For circles, both foci are at the center, therefore, a = b, c = 0, and e = 0.
22. 13.4 Most of the planets have very low e orbits (nearly circular) with Pluto (not a planet anymore) having the highest eccentricity. epluto = 0.25 ehalley = 0.97
23. 13.4 For planetary orbits, the points closest and furthest from the sun are call the Perihelion and Aphelion respectively, (perigee and apogee for orbits around the earth). Perihelion distance = a - c Aphelion distance = a + c Bound objects must follow elliptical orbits Unbound objects either follow parabolic or hyperbolic paths.
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25. 13.4 Kepler’s 2nd Law- speaks about the changing speeds due the changing distances from the sun. Comes from the conservation of Angular Momentum (L) There is no net torque on an orbiting object, because force and lever arm are parallel.
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27. 13.4 Kepler’s 3rd Law (T2 ~ r3) can be verified with Universal Gravitation for Circular Orbits M2 cancels, and we have g = ac
28. 13.4 In for v, we can plug circumference/period Simplifying and rearranging
29. 13.4 For a circular orbit, the radius is the semimajor axis, we can apply to ellipses… Where K is a constant for the object being orbited. Conveniently, when discussing the sun, K = 1 when T is in Earth Years and a is in AU (astronomical unit = avg earth sun distance).
30. 13.4 Quick Quizzes p. 399 Examples 13.4-13.5
31. 13.5 Gravitational Field Gravitational Field- a method for explaining how objects can apply forces over a distance. Objects with mass create a “gravitational field” in the surrounding space. Object is called a source particle The field is equal to the force on a test particle in the field, divided by the mass of the test particle.
32. 13.5 The Gravitational Field is another way discussing the acceleration due to gravity felt by all objects in the field.
33. 13.6 Gravitational Potential Energy Remember Gravity is a conservative force. So work done by gravity = opposite change in potential energy. (ΔU = - W)
34. 13.6 We can integrate Fg over changes in r Becomes
35. 13.6 So we have
36. 13.6 Why is it negative? Gravity is an attractive force An external force must do positive work to increase the separation between objects. Ug = 0 at an infinite distance away. U becomes less negative as r increases. It is a potential well, or energy deficit.
37. 13.7 Energy Considerations in Planetary and Satellite Motion The total energy for a planet in orbit
38. 13.7 Using Universal Gravitation we can put Kinetic Energy in gravitational terms. Multiplying by r and dividing by 2 gives
39. 13.7 Sub in the previous energy equation. Becomes… Therefore…
40. 13.7 The energyof a circular orbit is a constant, just like angular momentum. It is negative, because the object in orbit is bound, The absolute value is the energy need to escape orbit (to have zero energy at r = ∞)
41. 13.7 Escape speed is the velocity required at a given distance from the gravitational center needed to reach infinity with zero velocity. The velocity that gives the system a total energy of zero (unbound).
42. 17.3 Quick Quiz p 406 Example 13.7, 13.8
43. 13.7 On black holes- Massive Stars, collapse under gravitational forces post Supernova. The highly dense material (singularity) has an extremely strong gravitational force. At (and inside) the critical (Schwarzschild) radius, the escape speed is equal to (and greater than) the speed of light (c = 3.0 x 108 m/s). This Spherical boundary is called the Event Horizon.
44. 13.7
45. 13.7 Binary System of a star and black hole.
46. 13.7 While nothing can escape from inside the event horizon, matter that is accreting experiences friction, increasing temperature, causing a release of high enery radiation (up to x-ray).