1. Chapter 4: Making Sense of the Universe Understanding Motion, Energy, and Gravity
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2. How do we describe motion?
Precise definitions to describe motion:
Speed: Rate at which object moves
Example: speed of 10 m/s
Velocity: Speed and direction Example: 10 m/s, due east
Acceleration: Any change in velocity; units of distance/time2 (m/s2)
Basic vocabulary of motion. Emphasize that turning, slowing, and speeding up are all examples of acceleration.
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3. Acceleration of Gravity
All falling objects accelerate at the same rate (not counting friction of air resistance).
On Earth, g ≈ 10 m/s2: speed increases 10 m/s with each second of falling.
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4. Acceleration of Gravity (g)
Galileo showed that g is the same for all falling objects, regardless of their mass.
When you show this video clip, be sure to point out what is going on since it is not easy to see… Also, remind them that g on the moon is not the same as g on the Earth.
Apollo 15 demonstration
Feather and Hammer Drop
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5. Momentum and Force Momentum = mass x velocity. (p = mv)
A net force changes momentum, which generally means an acceleration (change in velocity).
The rotational momentum of a spinning or orbiting object is known as angular momentum.
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6. Thought Question
Is a net force acting on each of the following? (Answer yes or no.)
A car coming to a stop
A bus speeding up
An elevator moving up at constant speed
A bicycle going around a curve
A moon orbiting Jupiter
Use to check if students can figure out where a net force is acting. For bonus questions, ask if they can identify the forces.
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7. Thought Question
Is a net force acting on each of the following? (Answer yes or no.)
A car coming to a stop: Yes
A bus speeding up: Yes
An elevator moving up at constant speed: No
A bicycle going around a curve: Yes
A moon orbiting Jupiter: Yes
Use to check if students can figure out where a net force is acting. For bonus questions, ask if they can identify the forces.
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8. How is mass different from weight?
Mass—the amount of matter in an object
Weight—the force that acts on an object
You are weightless in free-fall!
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9. Thought Question On the Moon,
your weight is the same; your mass is less.
your weight is less; your mass is the same.
your weight is more; your mass is the same.
your weight is more; your mass is less.
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10. Thought Question On the Moon,
your weight is the same; your mass is less.
your weight is less; your mass is the same.
your weight is more; your mass is the same.
your weight is more; your mass is less.
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11. Why are astronauts weightless in space?
There is gravity in space.
Weightlessness is due to a constant state of free-fall.
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12. What have we learned? How do we describe motion? Speed = distance/time
Speed and direction => velocity
Change in velocity => acceleration
Momentum = mass x velocity
Force causes change in momentum, producing acceleration.
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13. What have we learned? How is mass different from weight?
Mass = quantity of matter
Weight = force acting on mass
Objects are weightless in free-fall.
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14. 4.2 Newton's Laws of Motion
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15. How did Newton change our view of the universe?
He realized the same physical laws that operate on Earth also operate in the heavens:
one universe
He discovered laws of motion and gravity.
Much more: Experiments with light; first reflecting telescope, calculus…
Sir Isaac Newton (1642–1727)
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16. What are Newton's three laws of motion?
Newton's first law of motion: An object moves at constant velocity unless a net force acts to change its speed or direction.
You may wish to discuss the examples in the book on P. 83–84.
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17. Newton's second law of motion: Force = mass x acceleration.
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18. Newton's third law of motion: For every force, there is always an equal and opposite reaction force.
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19. Thought Question
Is the force that 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.
Earth and you exert equal and opposite forces on each other.
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20. Thought Question
Is the force that 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.
Earth and you exert equal and opposite forces on each other.
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21. Thought Question
A compact car and a large truck have a head-on collision. Are the following true or false?
The force of the car on the truck is equal and opposite to the force of the truck on the car.
The momentum transferred from the truck to the car is equal and opposite to the momentum transferred from the car to the truck.
The change of velocity of the car is the same as the change of velocity of the truck.
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22. Thought Question
A compact car and a large truck have a head-on collision. Are the following true or false?
The force of the car on the truck is equal and opposite to the force of the truck on the car. T
The momentum transferred from the truck to the car is equal and opposite to the momentum transferred from the car to the truck. T
The change of velocity of the car is the same as the change of velocity of the truck. F
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23. 4.3 Conservation Laws in Astronomy
Conservation of Linear Momentum
Conservation of Angular Momentum
Conservation of Energy
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24. Conservation of Linear Momentum
The total momentum of interacting objects cannot change unless an external force is acting on them.
Interacting objects exchange momentum through equal and opposite forces.
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25. Conservation of Angular Momentum
angular momentum = mass x velocity x radius
L = (m) x (v) x (r) – {magnitude}
The angular momentum of an object cannot change unless an external twisting force (torque) is acting on it.
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26. What keeps a planet rotating and orbiting the Sun?
You may wish to go over this figure in some detail to be sure the idea is clear.
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27. Angular momentum conservation also explains why objects rotate faster as they shrink in radius.
Discuss astronomical analogs: disks of galaxies, disks in which planets form, accretion disks…
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28. 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.
Begin by defining energy…
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29. Basic Types of Energy Kinetic (motion) Radiative (light)
Stored or potential
Energy can change type but cannot be destroyed.
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30. Thermal Energy:
The collective kinetic energy of many particles (for example, in a rock, in air, in water) Thermal energy is related to temperature but it is NOT the same. Temperature is the average kinetic energy of the many particles in a substance.
Students sometimes get confused when we've said there are three basic types of energy (kinetic, potential, radiative) and then start talking about subtypes, so be sure they understand that we are now dealing with subcategories.
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31. Temperature Scales Use this figure to review temperature scales.
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32. Thermal energy is a measure of the total kinetic energy of all the particles in a substance. It therefore depends on both temperature AND density. Example:
We've found this example of the oven and boiling water to be effective in explaining the difference between temperature and thermal energy. You may then wish to discuss other examples. You might also want to note that the temperature in low-Earth orbit is actually quite high, but astronauts get cold because of the low density.
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33. Gravitational Potential Energy
On Earth, it depends on…
an object's mass (m).
the strength of gravity (g).
the distance an object could potentially fall.
We next discuss two subcategories of potential energy that are important in astronomy: gravitational potential energy (this and next slide) and mass-energy.
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34. 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.
We next discuss two subcategories of potential energy that are important in astronomy: gravitational potential energy and mass-energy.
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35. Mass-Energy Mass itself is a form of potential energy.
A small amount of mass can release a great deal of energy.
Concentrated energy can spontaneously turn into particles (for example, in particle accelerators).
E = mc2
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36. 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.
You might wish to go through the example tracing the energy of a baseball back through time, as described on p. 97 of the text.
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37. What have we learned?
What keeps a planet rotating and orbiting the Sun?
Conservation of angular momentum
Where do objects get their energy?
Conservation of energy: Energy cannot be created or destroyed but only transformed from one type to another.
Energy comes in three basic types: kinetic, potential, and radiative.
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38. 4.4 The Force of Gravity
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39. What determines the strength of gravity?
The Newton’s Universal Law of Gravitation:
Every mass attracts every other mass.
Attraction is directly proportional to the product of their masses.
Attraction is inversely proportional to the square of the distance between their centers.
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40. 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 (ellipses)
unbound
parabola
hyperbola
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41. Newton generalized Kepler's third law:
Newton's version of Kepler's third law:
If a small object orbits a larger one and you measure the orbiting object‘s orbital period AND average
orbitaldistance ,THEN you can calculate the mass of the larger object.
Examples:
Calculate the mass of the Sun from Earth's orbital period (1 year) and average distance (1 AU).
Calculate the mass of Earth from orbital period and distance of a satellite.
Calculate the mass of Jupiter from orbital period and distance of one of its moons.
Emphasize that this law allows us to measure the masses of distant objects—an incredibly powerful tool.
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42. Newton's version of Kepler's third law
p = orbital period a = average orbital distance (between centers) (M1 + M2) = sum of object masses
Optional: Use this slide if you wish to introduce the equation for Newton's version of Kepler's third law.
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43. 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.
The concept of orbital energy is important to understanding orbits.
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44. Changing an Orbit
So what can make an object gain or lose orbital energy?
Friction or atmospheric drag
A gravitational encounter
Examples worth mentioning:
Satellites in low-Earth orbit crashing to Earth due to energy loss to friction with atmosphere
Captured moons like Phobos/Deimos or many moons of Jupiter: not easy to capture, and must have happened when an extended atmosphere or gas cloud allowed enough friction for the asteroid to lose significant energy
Gravitational encounters have affected comets like Halley's; also used by spacecraft to boost orbits…
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45. Escape Velocity
If an object gains enough orbital energy, it may escape (change from a bound to unbound orbit).
Escape velocity from Earth ≈ 11 km/s from sea level (about 40,000 km/hr).
Can use this to discuss how adding velocity can make a spacecraft move to a higher orbit or ultimately to escape on an unbound orbit.
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46. Relationship Between Cannonball's Mass and Orbital Trajectory
Use this tool from the Orbits and Kepler's laws tutorial to discuss escape velocity.
Escape and orbital velocities don't depend on the mass of the cannonball.
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47. 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 Earth.
Use this figure to explain the origin of the tidal bulges.
Gravitational pull decreases with (distance)2, so the Moon's pull on Earth is strongest on the side facing the Moon, weakest on the opposite side.
The Earth gets stretched along the Earth–Moon line.
The oceans rise relative to land at these points.
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48. Tides and Phases Size of tides depends on the phase of the Moon. Tides
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49. Tidal Friction
Optional special topic. You might wish to perform the demonstration shown in the figure…
Tidal friction gradually slows Earth's rotation (and makes the Moon get farther from Earth).
Moon once orbited faster (or slower); tidal friction caused it to "lock" in synchronous rotation.
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50. Why does the moon always show us the same face?
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51. End of Chapter 4: Questions?
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