1. Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing. Chapter 10 Our Star

2. Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing. Why does the Sun shine?

3. Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing. Is it on FIRE?

4. Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing. Is it on FIRE? Luminosity ~ 10,000 years Chemical Energy Content

5. Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing. Is it on FIRE? … NO! Luminosity ~ 10,000 years Chemical Energy Content

6. Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing. Is it CONTRACTING?

7. Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing. Luminosity Gravitational Potential Energy Is it CONTRACTING? ~ 25 million years

8. Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing. Luminosity Gravitational Potential Energy Is it CONTRACTING? … NO! ~ 25 million years

9. Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing. It is powered by NUCLEAR ENERGY! Luminosity ~ 10 billion years Nuclear Potential Energy (core) E = mc 2 —Einstein, 1905

10. Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing. Why does the Sun shine? —Chemical and gravitational energy sources could not explain how the Sun could sustain its luminosity for more than about 25 million years. —To shine for that long, the Sun must be fairly stable, balancing gravity pulling in with forces pushing out from light and heat.

11. Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing. Why does the Sun shine? —The balance of forces in and out is gravitational equilibrium —The Sun shines because gravitational equilibrium keeps its core hot and dense enough to release energy through nuclear fusion.

12. Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing. Weight of upper layers compresses lower layers

13. Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing. Gravitational equilibrium: Energy provided by fusion maintains the pressure.

14. Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing. What is the Sun’s structure?

15. Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing. What is the Sun’s structure? —From what we can see going outwards… Photosphere Chromosphere Corona These we CAN see – and measure with Visible-light, UV, and X-ray telescopes in orbit & on Earth

16. Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing. Radius: 6.9  10 8 m (109 times Earth) Mass: 2  10 30 kg (300,000 Earths) Luminosity: 3.8  10 26 watts

17. Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing. Photosphere: Visible surface ~ 6,000 K Seen in Visible Light Shows Dark “limb” Granules Sunspots! Absorption lines

18. Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing.

21. Chromosphere: Middle layer of solar atmosphere ~ 10 4 –10 5 K Seen in UV Light Shows emission lines Features: Prominences, Flares, Spicules

22. Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing. Credit: Chromosphere image courtesy Luc Viatour and Windows to the Universe, http://www.windows.ucar.eduhttp://www.windows.ucar.edu

23. Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing.

27. Corona: Outermost layer of solar atmosphere ~1 million K Seen in X-rays Shows emission lines + faint continuous spectrum

28. Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing. The Corona – Visible Light The Corona – X-ray Light

29. Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing.

30. Solar wind: A flow of charged particles (electrons, protons, some helium nuclei) from the surface of the Sun Creates Aurora

31. Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing.

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

33. Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing. What is the Sun’s structure? —Going *inwards* to layers we cannot see… Convection zone Radiation zone Core These we can’t see – we model with computer simulations, observations of surface features to suggest structure, and observations of neutrinos to hint at fusion reactions taking place in the core.

34. Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing.

35. Convection zone: Beneath Photosphere Creates granules we see Energy transported upward by rising hot gas

36. Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing. Bright blobs on photosphere where hot gas reaches the surface

37. Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing. Convection (rising hot gas) takes energy to the surface.

38. Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing. Patterns of vibration on the surface tell us about what the Sun is like inside.

39. Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing. Radiation zone: Energy transported upward by Gamma Ray & X-ray photons Determine extent based on computer models

40. Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing. Core: Energy generated by nuclear fusion ~ 15 million K Generates gamma rays Inner 10% of sun

41. Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing. Data on solar vibrations agree with mathematical models of solar interior.

42. Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing. How does nuclear fusion occur in the Sun? Fusion is the UNITING of light atomic nuclei into heavier nuclei, releasing binding energy in the form of gamma ray radiation and other particles

43. Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing. Fission Big nucleus splits into smaller pieces (Nuclear power plants) Fusion Small nuclei stick together to make a bigger one (Sun, stars)

44. Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing. High temperatures enable nuclear fusion to happen in the core.

45. Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing. Sun releases energy by fusing four hydrogen nuclei into one helium nucleus.

46. Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing. Proton–proton chain is how hydrogen fuses into helium in Sun

47. Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing. IN 4 protons OUT 4 He nucleus 2 gamma rays 2 positrons 2 neutrinos Total mass is 0.7% lower.

48. Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing. Neutrinos created during fusion fly directly through the Sun. Observations of these solar neutrinos can tell us what’s happening in the core.

49. Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing. Solar neutrino problem: Early searches for solar neutrinos failed to find the predicted number.

50. Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing. 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.

51. Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing. 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.

52. Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing. 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

53. Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing. 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

54. Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing. What causes solar activity?

55. Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing. Solar activity is like “weather” Sunspots Solar flares Solar prominences All are related to magnetic fields.

56. Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing. Sunspots… Are cooler than other parts of the Sun’s surface (4,000 K) Are regions with strong magnetic fields

57. Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing. Zeeman Effect We can measure magnetic fields in sunspots by observing the splitting of spectral lines

58. Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing. Charged particles spiral along magnetic field lines.

59. Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing. Loops of bright gas often connect sunspot pairs.

60. Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing. Magnetic activity causes solar flares that send bursts of X-rays and charged particles into space.

61. Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing. Magnetic activity also causes solar prominences that erupt high above the Sun’s surface.

62. Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing. The corona appears bright in X-ray photos in places where magnetic fields trap hot gas.

63. Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing. How does solar activity affect humans?

64. Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing. Coronal mass ejections send bursts of energetic charged particles out through the solar system.

65. Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing. Charged particles streaming from the Sun can disrupt electrical power grids and disable communications satellites.

66. Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing. How does solar activity vary with time?

67. Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing. The number of sunspots rises and falls in 11-year cycles.

68. Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing. The sunspot cycle has something to do with the winding and twisting of the Sun’s magnetic field.

69. Scott Hildreth – Chabot College – Adapted from Essential Cosmic Perspective 4 th ed. Copyright 2007 by Pearson Publishing. Hans Bethe Video Clips http://www.youtube.com/watch?v=apgB_N R59sshttp://www.youtube.com/watch?v=apgB_N R59ss http://www.youtube.com/watch?v=c7iJtT41 yy8http://www.youtube.com/watch?v=c7iJtT41 yy8 http://www.webofstories.com/play/4536?o= MShttp://www.webofstories.com/play/4536?o= MS