1. 4.1 and 4.2 Describing Motion, Newton and Galileo Speed, velocity and acceleration (skip momentum) Galileo’s experiments with falling objects: g = 9.8 m/sec2 Objects fall together Inertia (motion in absence of force) Newton’s Laws: 1.3 laws of motion: a. Inertia b. F=ma c. Action = Reaction 2.Gravitation: F= GM 1 M 2 /R 2 (Inverse-square law) 4.3 (Thermal Energy only) 4.4 The force of Gravity The Strength of Gravity ■ Newton and Kepler Orbits: 1. Closed: circles (circular velocity) & ellipses (v > v c ) 2. Open: parabolas and hyperbolas (escape velocity, v > v e ) Tides: Lunar and Solar End of Ch 4 Motion and Gravity (soap opera’s final episode)

2. The tides due to the Moon affect: a) Only the Oceans b) The whole Earth c) Only the night side of Earth d) None of the other answers is correct Question

3. The tides due to the Moon affect: a) Only the Oceans b) The whole Earth c) Only the night side of Earth d) None of the other answers is correct Question

4. Tides Gravitational force decreases with (distance) 2 –The Moon’s pull on Earth is strongest on the side facing the Moon, and weakest on the opposite side. The Earth gets stretched along the Earth-Moon line. The oceans rise relative to land at these points.

5. Tides vary with the phase of the Moon:

7. 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?

8. Tidal friction… Tidal friction gradually slows Earth rotation (and makes Moon get farther from Earth). Moon once orbited faster (or slower); tidal friction caused it to “lock” in synchronous rotation with its orbit around Earth.

9. How does Newton’s law of gravity allow us to extend Kepler’s laws? Applies to other objects, not just planets. Includes unbound orbit shapes: parabola, hyperbola We can now measure the mass of other systems. What have we learned? What determines the strength of gravity? Directly proportional to the product of the masses (M x m) Inversely proportional to the square of the separation d

10. What have we learned? How do gravity and energy together allow us to understand orbits? Gravity determines orbits Orbiting object cannot change orbit without energy transfer Enough energy -> escape velocity -> object leaves. How does gravity cause tides? Gravity stretches Earth along Earth-Moon line because the near side is pulled harder than the far side.

11. Chapter 5 Light: The Cosmic Messenger

12. 5.1Basic Properties of Light and Matter Light: electromagnetic waves 1. Velocity (c = speed of light), wavelength and frequency (colors), energy. 2. Electromagnetic spectrum, visible spectrum, atmospheric windows Matter: Atoms. How do light and matter interact? 5.2Learning from Light: Origin of Starlight (some not in book) 1. How photons are produced 2. Relation temperature  motion of atoms 3. Blackbody Radiation (hot iron example). Wien’s Law: hotter  brighter, cooler  dimmer hotter  bluer, cooler  redder ( max ~1/T) 4. Colors of Stars: redder are cooler, bluer are hotter 5. Types of spectra (Kirchhoff’s 3 laws ): Continuous, Absorption and Emission 6. Radial Velocity: Doppler effect 5.3Telescopes: reflecting and refracting, ground, airborne, space. Outline Ch 5 Light: The Cosmic Messenger

13. 5.1 Basic Properties of Light and Matter Our goals for learning What is light? What is matter? How do light and matter interact?

14. What is light?

15. Light is an electromagnetic wave Light is also a particle Photons: “pieces” of light, each with precise wavelength, frequency, and energy. Speed of light “c” is a constant in a vacuum = 300,000 km/sec

16. The Electromagnetic Spectrum

19. Atmospheric “Windows” 1.Visible Window (plus some UV and some infrared) 2.Radio Window

20. Question The higher the photon energy… a)the longer its wavelength. b)the shorter its wavelength. c)energy is independent of wavelength.

21. The higher the photon energy… a)the longer its wavelength. b)the shorter its wavelength. c)energy is independent of wavelength.

22. What is matter? Atomic structure:

23. Atomic Terminology Atomic Number = # of protons in nucleus Atomic Mass Number = # of protons + neutrons

24. Atomic Terminology Isotope: same # of protons but different # of neutrons ( 4 He, 3 He) Molecules: consist of two or more atoms (H 2 O, CO 2 )

25. How do light and matter interact? Emission Absorption Transmission Reflection or Scattering Terminology: Transparent: transmits light Opaque: blocks (absorbs) light

26. Interactions of light and matter

27. Question Why is the rose red? a)The rose absorbs red light. b)The rose transmits red light. c)The rose emits red light. d)The rose reflects red light.

28. Why is the rose red? a)The rose absorbs red light. b)The rose transmits red light. c)The rose emits red light. d)The rose reflects red light.

29. What have learned? What is light? Light is an electromagnetic wave that also comes in individual “pieces” called photons. Each photon has a precise wavelength, frequency and energy. Forms of light are: radio waves, microwaves, infrared, visible light, ultraviolet, X-rays and gamma rays

30. What have we learned? What is matter? Ordinary matter is made of atoms, which are made of protons, neutrons and electrons. How do light and matter interact? Matter can emit light, absorb light, transmit light or reflect light

31. 5.2. Learning from Light Our goals for learning What types of light spectra can we observe? How does light tell us what things are made of? How does light tell the temperatures of planets and stars? How does light tell us the speed of a distant object?

32. 5.2Learning from Light: Origin of Starlight (much of 5.2 not in book) 1. How photons are produced 2. Relation temperature  motion of atoms 3. Blackbody Radiation (hot iron example). Wien’s Law: hotter  brighter, cooler  dimmer hotter  bluer, cooler  redder ( max ~1/T) 4. Colors of Stars: redder are cooler, bluer are hotter 5. Types of spectra (Kirchhoff’s 3 laws ): Continuous, Absorption and Emission a.Model of atoms: energy levels b.Continuous spectrum c.Emission lines and absorption lines 6. Radial Velocity: Doppler effect

33. 5.2.1 How photons are produced? When the motion of an electron is disturbed 5.2.2 Relation temperature  motion of atoms (from Ch.4) The higher the temperature the faster the atoms in a substance will be moving As atoms collide the electrons collide and their motion is disturbed When the motion of electrons gets disturbed they produce photons The higher the temperature, the more collisions, the more photons

34. Temperature Scales (from Ch.4)

35. 5.2Learning from Light: Origin of Starlight 1. How photons are produced 2. Relation temperature  motion of atoms 3. Blackbody Radiation (hot iron example). Wien’s Law: hotter  brighter, cooler  dimmer hotter  bluer, cooler  redder ( max ~1/T)

36. How does light tell us the temperatures of planets and stars? Cooler Hotter

37. Properties of Blackbody Radiation: 1.Hotter objects emit more light (per unit area) at all wavelengths. i.e. hotter  brighter, cooler  dimmer 2.Hotter objects emit photons with a higher average energy. i.e. hotter  bluer, cooler  redder

38. 3.Wein’s Law ( max ~1/T) i.e., if we can measure the maximum radiation emitted by an object we can determine its temperature Maximum emission max2 max1 max3 Properties of Blackbody Radiation:

39. 5.2Learning from Light: Origin of Starlight 1. How photons are produced 2. Relation temperature  motion of atoms 3. Blackbody Radiation (hot iron example). Wien’s Law: hotter  brighter, cooler  dimmer hotter  bluer, cooler  redder ( max ~1/T) 4. Colors of Stars: redder are cooler, bluer are hotter Stars behave like “blackbodies” so we can use their colors to determine their temperatures

40. 5.2Learning from Light: Origin of Starlight 1. How photons are produced 2. Relation temperature  motion of atoms 3. Blackbody Radiation (hot iron example). Wien’s Law: hotter  brighter, cooler  dimmer hotter  bluer, cooler  redder ( max ~1/T) 4. Colors of Stars: redder are cooler, bluer are hotter 5. Types of spectra( Kirchhoff’s 3 laws ): Continuous, Absorption and Emission (page 118 of book) a.Model of atoms: energy levels b.Continuous spectrum c.Emission lines and absorption lines

41. What types of light spectra can we observe?

43. This process produces an emission spectrum

45. This process produces an absorption spectrum

46. 1.Continuous Spectrum (thermal radiation spectrum) 2.Emission Spectrum 3.Absorption spectrum Kirchhoff’s Laws (p117-119 in book) 13 2

48. Continuous Spectrum

50. Emission Spectrum

53. Absorption Spectrum

56. Solar Spectrum

58. How does light tell us what things are made of? Electrons in atoms have distinct energy levels. Each chemical element, ion, molecule, has a unique set of energy levels. We can identify the chemicals in gas by their fingerprints in the spectrum. Distinct energy levels lead to distinct emission or absorption lines.

60. If the temperature of a star goes from 6000 K to 5000 K, what happens to its light? A.1. It becomes brighter B.2. It becomes bluer C.3. It becomes fainter D.4. It becomes redder E.5. It remains constant The correct answer is: A.A. 3 only B.B. 4 only C.C. 5 only D.D. 1 and 2 E.E. 3 and 4 Question 1

61. Can one use the visible color of the Moon to determine its temperature? A.Yes, because the Moon is similar to stars B.Yes, because the Moon does not reflect light C.Yes, because the Moon orbits Earth D.None of the above are correct Question 2

62. Which is hotter? a)A blue star. b)A red star. c)A planet that emits only infrared light.

63. Which is hotter? a)A blue star. b)A red star. c)A planet that emits only infrared light.

64. Question Why don’t we glow in the dark? a)People do not emit any kind of light. b)People only emit light that is invisible to our eyes. c)People are too small to emit enough light for us to see. d)People do not contain enough radioactive material.

65. Why don’t we glow in the dark? a)People do not emit any kind of light. b)People only emit light that is invisible to our eyes (infrared light). c)People are too small to emit enough light for us to see. d)People do not contain enough radioactive material.

66. Radial Velocity Approaching stars: more energy, Receding stars: less energy, 5.2.6 Doppler Effect