1. Chapter 3 Gravity and Motion Copyright (c) The McGraw-Hill Companies, Inc. Permission required for reproduction or display.

2. Gravity Gravity gives the Universe its structure –It is a universal force that causes all objects to pull on all other objects everywhere. Even Dark Matter. –It holds objects together –It is responsible for holding the Earth in its orbit around the Sun, the Sun in its orbit around the Milky Way, and the Milky Way in its path within the Local Group

3. The Problem of Astronomical Motion Astronomers of antiquity did not connect gravity and astronomical motion Galileo investigated this connection with experiments using projectiles and balls rolling up & down planks He put science on a course to determine laws of motion and to develop the scientific method

4. Inertia Galileo established the idea of inertia –A body at rest tends to remain at rest –A body in motion tends to remain in motion –Through experiments with inclined planes, Galileo demonstrated the idea of inertia and the importance of forces (friction)

5. Inertia and Newton’s First Law This concept was incorporated in Newton’s First Law of Motion: A body continues in a state of rest or uniform motion in a straight line unless made to change that state by forces acting on it

6. The Moving Earth Even before Galileo, Copernicus proposed that Earth was moving. This idea was refuted by people. Example: If Earth moved, how can a bird swoop from a branch to catch a worm? Solution: As it swoops, due to inertia, it continues to go sideways at the speed of Earth along with the tree, worm, etc.

7. http://upload.wikimedia.org/wikipedia/commons/3/30/Globespin.gif At the equator, earth rotates at about 1000mph. Earth rotates to the east. Jump up near a western wall. Why doesn’t the wall smack me in the face? Answer: because before, during and after you jump you are going the same speed as the earth. Gravity only affects our vertical motion.

8. You are riding in an jet plane at a steady speed of 550 mph and toss a coin up. Where will the coin land? A.behind you B.ahead of you C.back in your hand D.There is not enough information. A Moving Plane

9. You are riding in a jet at a steady speed of 550 mph and toss a coin up. Where will the coin land? A.behind you B.ahead of you C.back in your hand D.There is not enough information. A Moving Plane Explanation: The coin has inertia. It continues moving with the jet and your hand and lands back in your hand.

10. Newton’s First Law Important ideas of Newton’s First Law –Force: A push or a pull –The force referred to is a net force –The law implies that if an object is not moving with constant velocity, then a nonzero net force must be present

11. Astronomical Motion As seen earlier, planets move along curved (elliptical) paths, or orbits. Speed and direction is changing. (Kepler’s 2nd Law) Must there be a force at work? Yes!

12. Kepler’s 2nd Law The closer a planet is to the Sun, the faster it moves

13. Gravity is that force! If the string breaks here, what path will the ball take? A, B or C.

14. Gravity is that force!

15. Orbital Motion and Gravity Although not the first to propose gravity as being responsible for celestial motion, Newton was the first to: –Spell out the properties of gravity –Write the equations of gravity-induced motion Newton deduced that: –The Moon’s motion could be explained by the existence of a force (to deviate the Moon from a straight inertial trajectory) and that such a force decreased with distance –Orbital motion could be understood as a projectile moving “parallel” to the Earth’s surface at such a speed that its gravitational deflection toward the surface is offset by the surface’s curvature away from the projectile

16. Thought Experiment: A Cannon on a Mountain

17. Orbital Motion Using Newton’s First Law A cannonball fired at slow speed experiences one force – gravity, pulling it downward A cannonball fired at a higher speed feels the same force, but goes farther

18. Orbital Motion Using Newton’s First Law At a sufficiently high speed, the cannonball travels so far that the ground curves out from under it. The cannonball literally misses the ground! The ball, now in orbit, still experiences the pull of gravity!

19. Newton’s Second Law: Motion Motion –An object is said to be in uniform motion if its speed and direction remain unchanged –An object in uniform motion is said to have a constant velocity –A force will cause an object to have non- uniform motion, a changing velocity –Acceleration is defined as a change in velocity

20. Newton’s 2nd Law: Acceleration Acceleration –An object increasing or decreasing in speed along a straight line is accelerating (or decelerating) –An object with constant speed moving in a curved path is accelerating –Acceleration is produced by a force and experiments show the two are proportional

21. Newton’s Second Law: Mass Mass –Mass is the amount of matter an object contains –Technically, mass is a measure of an object’s inertia –Mass is generally measured in kilograms –Mass should not be confused with weight, which is a force related to gravity – weight may change from place to place, but mass does not

22. Newton’s Second Law of Motion F = ma

24. Newton’s Third Law of Motion When two objects interact, they create equal and opposite forces on each other This is true for any two objects, including the Sun and the Earth!

25. A Rocket Accelerates by Newton’s 3 rd law A relatively small mass of gas accelerates at high speed out the back each second with a force to accelerate the relatively large mass rocket to a relatively smaller speed. Gas Force out the back = Rocket Force of the front F fuel = F rocket mA| back = Ma| front

26. Newton’s Law of Universal Gravity Everything attracts everything else!!

27. Measuring an Object’s Mass Using Orbital Motion

28. Measuring an Object’s Mass Using Orbital Motion Method of Solution –Equate F = mv 2 /r to F = GMm/r 2 and solve for v: v = (GM/r) 1/2 –One can also solve for M: M = (v 2 r)/G –v can be expressed in terms of the orbital period (P) on the small mass and its orbital radius: v = 2  r/P –Combining these last two equations: M = (4  2 r 3 )/(GP 2 ) –This last equation in Kepler’s modified third law and is often used to calculate the mass of a large celestial object from the orbital period and orbital radius of a much smaller mass. –Used to compute the mass of exoplanets and the Sun (see pg. 80).

29. Kepler’s 3 rd Law This law implies that a planet with a larger average distance from the Sun, which is the semimajor axis distance, will take longer to circle the Sun Third law hints at the nature of the force holding the planets in orbit M = (4  2 r 3 )/(GP 2 ) or MGP 2 = 4π 2 r 3 (metric system) r r

30. Surface Gravity Surface gravity is the acceleration a mass undergoes at the surface of a celestial object (e.g., an asteroid, planet, or star) Surface gravity: –Determines the weight of a mass at a celestial object’s surface –Influences the shape of celestial objects –Influences whether or not a celestial object has an atmosphere –Small objects as asteroids are not spherical because the gravitational pull at their surface is too weak to crush them into round shapes.

31. Surface Gravity Calculations Surface gravity is determined from Newton’s Second Law and the Law of Gravity: ma = GMm/R 2 where M and R are the mass and radius of the celestial object, and m is the mass of the object whose acceleration a we wish to know The surface gravity, denoted by g, is then: g = GM/R 2 Notice dependence of g on M and R, but not m g Earth = 9.8 m/s 2 g Earth /g Moon = 5.6 Bowling Ball-Feather Drop in Vacuum

32. Escape Velocity To overcome a celestial object’s gravitational force and escape into space, a mass must obtain a critical speed called the escape velocity Escape velocity: –Determines if a spacecraft can move from one planet to another –Influences whether or not a celestial object has an atmosphere –Relates to the nature of black holes where even the velocity of light is too slow to escape the pull of a black hole.

33. Escape Velocity The escape velocity is the speed an object must have to be able to move away from a body and not be drawn back by its gravity. Throw an object upward. The faster the object is tossed upward, the higher it goes and the longer it takes to fall back. Escape velocity is the speed an object needs so that it will never fall back.

34. Escape Velocity

35. (a)A satellite is put into orbit by giving it a tangential speed of 7.6 km/s at an altitude of 500km (b)At an altitude of 500km, 7.6km/s for circular orbit. Between 7.6 and 11km/s, in an elliptical orbit. Greater than 11km/s satellite escapes earths gravity and goes off into space.

36. Escape Velocity Calculation The escape velocity, V esc, is determined from Newton’s laws of motion and the Law of Gravity and is given by: V esc = (2GM/R) 1/2 where M and R are the mass and radius of the celestial object from which the mass wishes to escape Notice dependence of V esc on M and R, but not m V esc,Earth = 11 km/s, V esc,Moon = 2.4 km/s = 6.83 miles/s = 24,606 miles/hr

37. Escape Velocity