ASTR100 (Spring 2008) Introduction to Astronomy Newton’s Laws of Motion

1. ASTR100 (Spring 2008) Introduction to AstronomyNewton’s Laws of Motion Prof. D.C. Richardson Sections 0101-0106

2. Newton’s 1st Law of Motion • An object moves at constant velocity unless a net force acts to change its speed or direction.

3. Newton’s 2nd Law of Motion • Force = mass × acceleration.

4. Newton’s 3rd Law of Motion • For every force, there is always an equal and opposite reaction force.

5. Is the force the Earth exerts on you larger, smaller, or the same as the force you exert on it? • Earth exerts a larger force on you. • You exert a larger force on Earth. • You and Earth exert equal and opposite forces on each other.

6. Is the force the Earth exerts on you larger, smaller, or the same as the force you exert on it? • Earth exerts a larger force on you. • You exert a larger force on Earth. • You and Earth exert equal and opposite forces on each other.

7. A Toyota Prius and a Ford Explorer have a head-on collision. Are the following true or false? • The force of the car on the SUV is equal and opposite to the force of the SUV on the car. • The momentum transferred from the SUV to the car is equal and opposite to the momentum transferred from the car to the SUV. • The change of velocity of the car is the same as the change of velocity of the SUV. TRUE TRUE FALSE

8. ASTR100 (Spring 2008) Introduction to AstronomyConservation Laws and Gravity Prof. D.C. Richardson Sections 0101-0106

9. Conservation Laws • Conservation of momentum. • Conservation of angular momentum. • Conservation of energy. These laws are embodied in Newton’s laws, but offer a different and sometimes more powerful way to consider motion.

10. What keeps a planet orbiting the Sun? • Conservation of angular momentum. Bigger r, smaller v Smaller r, bigger v

11. Angular momentum conservation also explains why objects rotate faster as they shrink in radius:

12. Where do objects get their energy? • Energy makes matter move. • Energy is conserved, but it can… • …transfer from one object to another; • …change in form.

13. Basic Types of Energy • Kinetic (motion) • Radiative (light) • Stored or potential Energy can change type but cannot be destroyed.

15. Thermal Energy • The collective kinetic energy of many particles (e.g., in rock, in air, in water). • Thermal energy is related to temperature but is NOT the same. • Temperature is the average kinetic energy of the particles in a substance. lower temp. higher temp.

16. Temperature Scales

17. Thermal energy is a measure of the total kinetic energy of all the particles in a substance. Depends on both temperature AND density…

18. Gravitational Potential Energy • On Earth, depends on: • Object’s mass (m). • Strength of gravity (g). • Distance object could potentially fall.

19. Gravitational Potential Energy • In space, an object or gas cloud has more gravitational energy when it is spread out than when it contracts. • A contracting cloud converts gravitational potential energy to thermal energy.

20. Mass-Energy E = mc2 • Mass itself is a form of potential energy. • A small amount of mass can release a great deal of energy…

21. Conservation of Energy • Energy can be neither created nor destroyed. • It can change form or be exchanged between objects. • The total energy content of the Universe was determined in the Big Bang and remains the same today.

22. The Universal Law of Gravitation • Every mass attracts every other mass. • The force of attraction is directly proportional to product of masses. • Attraction is inversely proportional to square of distance between centers.

23. How does Newton’s law of gravity extend Kepler’s laws? • Kepler’s first two laws apply to all orbiting objects, not just planets. • Ellipses are not the only orbital paths. • Orbits can be: • Bound (ellipse). • Unbound… • Parabola. • Hyperbola.

24. Newton’s Form of Kepler’s 3rd Law • If a small object orbits a larger one, and you measure the orbital period (p) and the average orbital distance (a), then you can calculate the mass of the larger object. • Examples: • Calculate Sun’s mass from Earth’s orbital period (1 yr) and average distance (1 AU). • Calculate Earth’s mass from orbital period and distance of a satellite. • Calculate Jupiter’s mass from orbital period and distance of one of its moons.

25. Newton’s Form of Kepler’s 3rd Law p = orbital period a = average orbital distance (between centers) (M1 + M2) = sum of object masses

26. How do gravity and energy together allow us to understand orbits? • Total orbital energy (gravitational + kinetic) stays constant if there is no external force. • Orbits cannot change spontaneously. More gravitational energy; Less kinetic energy Less gravitational energy; More kinetic energy Total orbital energy stays constant.

27. Changing an Orbit • So what can make an object gain or lose orbital energy? • Thrust. • Friction or atmospheric drag. • A gravitational encounter.

28. If an object gains enough orbital energy, it escapes (goes from bound to unbound orbit). Escape speed from Earth = 11.2 km/s from sea level (about 40,000 km/hr).

30. Escape and orbital speeds don’t depend on the mass of the cannonball…

31. How does gravity cause tides? • The Moon’s gravity pulls harder on near side of Earth than on far side. • The difference in the Moon’s gravitational pull stretches the Earth.

32. Size of tides depends on the phase of the Moon.

33. Special Topic: Why does the Moon always show the same face to Earth? Moon rotates in the same amount of time that it orbits… But why?

34. Tidal Friction • Tidal friction gradually slows Earth rotation (and makes Moon get farther from Earth). • Similarly, Moon probably rotated much faster long ago; tidal friction caused it to “lock” in synchronous rotation.