1. Information about Midterm #1 Grades are posted on course website Average = 129/180, s.d. = 27 Highest 180/180 Scores below 100 => “serious concerns” Next midterm: Tuesday, November 15 (sec 3) or Wednesday, November 16 (sec 4) Pick up exams in labs, and keep for studying for midterm #2

2. Chapter 10 Our Star

3. Why does the Sun shine?

4. Is it on FIRE?

5. Luminosity ~ 10,000 years Chemical Energy Content

6. Is it on FIRE? … NO! Luminosity ~ 10,000 years Chemical Energy Content

7. Is it CONTRACTING?

8. Luminosity Gravitational Potential Energy Is it CONTRACTING? ~ 25 million years

9. Luminosity Gravitational Potential Energy Is it CONTRACTING? … NO! ~ 25 million years

10. It is powered by NUCLEAR ENERGY! Luminosity ~ 10 billion years Nuclear Potential Energy (core) E = mc 2 —Einstein, 1905

11. Weight of upper layers compresses lower layers

12. Gravitational equilibrium: Energy provided by fusion maintains the pressure.

13. Gravitational contraction… provided energy that heated the core as the Sun was forming. Contraction stopped when fusion began replacing the energy radiated into space.

14. What is the Sun’s structure?

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

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

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

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

19. Photosphere: Visible surface of Sun ~ 6,000 K Cut-away Section of the Sun

20. Convection zone: Energy transported upward by rising hot gas

21. Radiation zone: Energy transported upward by photons

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

23. How does nuclear fusion occur in the Sun?

24. Fission Big nucleus splits into smaller pieces (Nuclear power plants) Fusion Small nuclei stick together to make a bigger one (Sun, stars)

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

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

27. Proton–proton chain is how hydrogen fuses into helium in the Sun.

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

29. Thought Question 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.

30. Thought Question 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. Solar thermostat keeps burning rate steady

31. Solar Thermostat 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 Structure of the Sun

32. How does the energy from fusion get out of the Sun?

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

34. Convection (rising hot gas) takes energy to the surface.

35. Bright blobs on photosphere where hot gas reaches the surface

36. How do we know what is happening inside the Sun?

37. We learn about the inside of the Sun by … making mathematical models. observing solar vibrations. observing solar neutrinos.

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

40. Data on solar vibrations agree with mathematical models of solar interior.

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

42. Solar neutrino problem: Early searches for solar neutrinos failed to find the predicted number.

43. Solar neutrino problem: Early searches for solar neutrinos failed to find the predicted number. (Note: Ray Davis was awarded the 2002 Nobel Prize in Physics for making this observation)

44. Solar neutrino problem: Early searches for solar neutrinos failed to find the predicted number More recent observations also found a deficit of neutrinos. A new theory of the neutrino predicts that they have mass and can change form. This theory agrees with the observed neutrino numbers.

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. What causes solar activity?

47. Solar activity is like “weather” Sunspots Solar flares Solar prominences All are related to magnetic fields.

48. Sunspots… Are cooler than other parts of the Sun’s surface (4,000 K) Are regions with strong magnetic fields

49. Zeeman Effect We can measure magnetic fields in sunspots by observing the splitting of spectral lines

50. Charged particles spiral along magnetic field lines.

51. Loops of bright gas often connect sunspot pairs.

52. Magnetic activity causes solar flares that send bursts of X-rays and charged particles into space.

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

54. The corona appears bright in X-ray photos in places where magnetic fields trap hot gas.

55. How does solar activity affect humans?

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 disable communications satellites.

58. How does solar activity vary with time?

59. The number of sunspots rises and falls in 11-year cycles.

61. The sunspot cycle has something to do with the winding and twisting of the Sun’s magnetic field.