1. © 2010 Pearson Education, Inc. 1. The Sun appears bright orange because of the extremely hot fires that are constantly burning carbon. TRUE or FALSE 2. Gravitational contraction (shrinking Sun) is responsible for the heat and light given off by the sun. TRUE or FALSE 3. Solar power output is measured in _____. a. solar unitsb. amperesc. luminosity 4. The equation discovered by Einstein that relates mass and potential energy is _____. a. PE = mg hb. E = 1/2mv^ 2c. E=mc ^ 2 5. The outermost layer of the Sun’s atmosphere which is not usually visible is the _____. a. coronab. convective zonec. core

3. © 2010 Pearson Education, Inc. Our goals for learning:  Why was the Sun’s energy source a major mystery?  Why does the Sun shine?  What is the Sun’s structure?

4. © 2010 Pearson Education, Inc.

5. Is it on FIRE?

6. Luminosity ~ 10,000 years Chemical energy content

7. Is it on FIRE? … NO! Luminosity ~ 10,000 years Chemical energy content

8. Is it CONTRACTING? Insert TCP 6e Chapter 14 opener

9. © 2010 Pearson Education, Inc.

10. It can be powered by NUCLEAR ENERGY! (E = mc 2 ) Luminosity ~ 10 billion years Nuclear potential energy (core)

11. Weight of upper layers compresses lower layers. Insert TCP 6e Figure 14.1

12. Gravitational equilibrium: Energy supplied by fusion maintains the pressure that balances the inward crush of gravity.

13. © 2010 Pearson Education, Inc. Insert TCP 6e Figure 14.3

14. Radius: 6.9  10 8 m (109 times Earth) Mass: 2  10 30 kg (300,000 Earths) Luminosity: 3.8  10 26 watts

16. http://www.pbs.org/wgbh/nova/labs/lab/sun/1/1/

17. Solar wind: A flow of charged particles from the surface of the Sun

18. Corona: Outermost layer of solar atmosphere ~1 million K

19. Chromosphere: Middle layer of solar atmosphere ~ 10 4 –10 5 K

20. Photosphere: Visible surface of Sun ~ 6000 K

21. Convection Zone: Energy transported upward by rising hot gas

22. Radiation Zone: Energy transported upward by photons

23. Core: Energy generated by nuclear fusion ~ 15 million K

24. © 2010 Pearson Education, Inc.  Why was the Sun’s energy source a major mystery?  Chemical and gravitational energy sources could not explain how the Sun could sustain its luminosity for more than about 25 million years.  Why does the Sun shine?  The Sun shines because gravitational equilibrium keeps its core hot and dense enough to release energy through nuclear fusion.

25. © 2010 Pearson Education, Inc.  What is the Sun’s structure?  From inside out, the layers are:  Core  Radiation zone  Convection zone  Photosphere  Chromosphere  Corona

26. © 2010 Pearson Education, Inc. Our goals for learning:  How does nuclear fusion occur in the Sun?  How does the energy from fusion get out of the Sun?  How do we know what is happening inside the Sun?

27. © 2010 Pearson Education, Inc.

28. Fission Big nucleus splits into smaller pieces. (Example: nuclear power plants) Fusion Small nuclei stick together to make a bigger one. (Example: the Sun, stars)

29. High temperatures enable nuclear fusion to happen in the core.

30. The Sun releases energy by fusing four hydrogen nuclei into one helium nucleus.

31. The proton–proton chain is how hydrogen fuses into helium in Sun.

32. IN 4 protons OUT 4 He nucleus 2 gamma rays 2 positrons 2 neutrinos Total mass is 0.7% lower.

33. © 2010 Pearson Education, Inc. What would happen inside the Sun if a slight rise in core temperature led to a rapid rise in fusion energy? A. The core would expand and heat up slightly. B. The core would expand and cool. C. The Sun would blow up like a hydrogen bomb.

34. © 2010 Pearson Education, Inc. What would happen inside the Sun if a slight rise in core temperature led to a rapid rise in fusion energy? A. The core would expand and heat up slightly. B. The core would expand and cool C. The Sun would blow up like a hydrogen bomb. The solar thermostat keeps burning rate steady.

35. © 2010 Pearson Education, Inc. Decline in core temperature causes fusion rate to drop, so core contracts and heats up. Rise in core temperature causes fusion rate to rise, so core expands and cools down.

36. © 2010 Pearson Education, Inc.

37. Energy gradually leaks out of radiation zone in form of randomly bouncing photons.

38. Convection (rising hot gas) takes energy to surface.

39. Bright blobs on photosphere show where hot gas is reaching the surface.

40. © 2010 Pearson Education, Inc.

41.  making mathematical models  observing solar vibrations  observing solar neutrinos

42. Patterns of vibration on the surface tell us about what the Sun is like inside.

43. Data on solar vibrations agree very well with mathematical models of solar interior.

44. Neutrinos created during fusion fly directly through the Sun. Observations of these solar neutrinos can tell us what’s happening in core.

45. Solar neutrino problem: Early searches for solar neutrinos failed to find the predicted number. More recent observations find the right number of neutrinos, but some have changed form.

46. © 2010 Pearson Education, Inc.  How does nuclear fusion occur in the Sun?  The core’s extreme temperature and density are just right for nuclear fusion of hydrogen to helium through the proton–proton chain.  Gravitational equilibrium acts as a thermostat to regulate the core temperature because fusion rate is very sensitive to temperature.

47. © 2010 Pearson Education, Inc.  How does the energy from fusion get out of the Sun?  Randomly bouncing photons carry energy through the radiation zone.  Rising of hot plasma carries energy through the convection zone to photosphere.  How do we know what is happening inside the Sun?  Mathematical models agree with observations of solar vibrations and solar neutrinos.

48. © 2010 Pearson Education, Inc. Our goals for learning:  What causes solar activity?  How does solar activity affect humans?  How does solar activity vary with time?

49. © 2010 Pearson Education, Inc.

50.  Sunspots  Solar flares  Solar prominences All these phenomena are related to magnetic fields.

51. Sunspots Are cooler than other parts of the Sun’s surface (4000 K) Are regions with strong magnetic fields

52. Loops of bright gas often connect sunspot pairs.

53. Magnetic activity causes solar flares that send bursts of X rays and charged particles into space. Solar Flares classified from lowest to highest: B class C class M class X class

54. Magnetic activity also causes solar prominences that erupt high above the Sun’s surface.

55. © 2010 Pearson Education, Inc.

56. Coronal mass ejections send bursts of energetic charged particles out through the solar system.

57. Charged particles streaming from the Sun can disrupt electrical power grids and can disable communications satellites.

58. © 2010 Pearson Education, Inc.

59. The number of sunspots rises and falls in an 11-year cycle. Insert TCP 6e Figure 14.21a unannotated Insert TCP 6e Figure 14.21b unannotated

60. The calm sun on the left (Oct. 2010) is contrasted with a much more active sun on the right as it approaches solar maximum. http://youtu.be/oOXVZo7KikE

61. © 2010 Pearson Education, Inc.  What causes solar activity?  Stretching and twisting of magnetic field lines near the Sun’s surface cause solar activity.  How does solar activity affect humans?  Bursts of charged particles from the Sun can disrupt radio communication and electrical power generation and damage satellites.  How does solar activity vary with time?  Activity rises and falls with an 11-year period.