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Doppler/ Sunspots/ Interior

Doppler/ Sunspots/ Interior. Lab notes. “ Sunspots ” lab discussion today after class. Telescope Lab next week. Constellation Lab coming up. Picture How to find it Interesting objects History/Mythology Participation. What is the speed of light?. A) 3x10 5 B) 3x10 8

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Doppler/ Sunspots/ Interior

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  1. 1

  2. Doppler/ Sunspots/ Interior 2

  3. Lab notes • “Sunspots” lab discussion today after class. • Telescope Lab next week. • Constellation Lab coming up. • Picture • How to find it • Interesting objects • History/Mythology • Participation 3

  4. What is the speed of light? A) 3x105 B) 3x108 C) Not enough information in A or B. 4

  5. The Doppler Effect • One more tool… 5

  6. A source of light is approaching us at 3,000 km/s. All its waves are: A) Red shifted by 1% B) Blue shifted by 1% C) Not affected, as c is constant in all reference frames. D) Red shifted out of the visible into the infrared E) Blue shifted out of the visible into the ultraviolet 6

  7. Figure 2.22Doppler Effect 7

  8. The Doppler Effect • A “red” shift to longer wavelengths occurs when an object moves away from you. • A “blue” shift to shorter wavelengths occurs when an object moves towards from you. • Transverse velocities have no effect. 8

  9. The Doppler Effect A Note on police radar • Pulses are emitted, and the change in frequency of the echo pulse is what is measured - NOT a shift in the wavelength of the return pulse. 9

  10. Figure 2.23Doppler Shift • For EM waves (astronomical purposes) wave speed = c • c = 3 x 108 m/s 10

  11. A source of light is approaching us at 3,000 km/s. All its waves are: • Discuss what you think the effect will be on the spectral lines. • Does frequency appear higher or lower? • By how much? • Recall: 11

  12. A source of light is approaching us at 3,000 km/s. All its waves are: A) Red shifted by 1% B) Blue shifted by 1% C) Not affected, as c is constant in all reference frames. D) Red shifted out of the visible into the infrared E) Blue shifted out of the visible into the ultraviolet 12

  13. A source of light is approaching us at 3,000 km/s. All its waves are: A) Red shifted by 1% B) Blue shifted by 1% C) Not affected, as c is constant in all reference frames. D) Red shifted out of the visible into the infrared E) Blue shifted out of the visible into the ultraviolet 13

  14. Chapter 9 The Sun 14

  15. The temperature of the photosphere of the Sun is about: A) 4500 K B) 5800 K C) 11000 K D) 1 million K E) 15 million K 15

  16. The temperature of the photosphere of the Sun is about: A) 4500 K B) 5800 K C) 11000 K D) 1 million K E) 15 million K 16

  17. What is the meaning of the solar constant? A) The regularity of the 11 year sunspot cycle. B) The fact that features on the Sun appear to never change. C) The stability of the Sun’s luminosity during its existence. D) The amount of energy received at the Earth’s surface per unit area and unit time. E) The fact that the amount of hydrogen turning into Helium in the core is fixed. 17

  18. What is the meaning of the solar constant? A) The regularity of the 11 year sunspot cycle. B) The fact that features on the Sun appear to never change. C) The stability of the Sun’s luminosity during its existence. D) The amount of energy received at the Earth’s surface per unit area and unit time. E) The fact that the amount of hydrogen turning into Helium in the core is fixed. 18

  19. http://science.nasa.gov/science-news/science-at-nasa/2003/17jan_solcon/http://science.nasa.gov/science-news/science-at-nasa/2003/17jan_solcon/ • http://www.nasa.gov/mission_pages/sdo/main/index.html 19

  20. Chapter 9 Sunspots 20

  21. Figure 9.15Sunspots 21

  22. Figure 9.16Sunspots, Up Close • Darker (cooler) places on the Sun. • Typically about the size of Earth (~10,000 km) • Umbra - dark center (~4500K) • Penumbra - lighter surrounding region (~5500 K) 22

  23. Sunspot Magnetism • Zeeman effect - a slitting of spectral lines from magnetic fields. If you can measure the “splitting”, then you can determine the magnetic field. • Magnetic field in sunspots • Typically ~1000x greater than that in the surrounding region. • Field lines typically perpendicular to surface (either N or S) • Magnetic field disrupts the convective flow. (Hot stuff in the interior can’t “percolate” to the surface.) 23

  24. Sunspot Magnetism • Sunspots typically occur in pairs • A N-S pair will follow each other in the direction of the suns rotation. • Ordering (N-S or S-N) will be opposite in northern and southern hemispheres. • Direction reverses every 11 years. 24

  25. Figure 9.17Sunspot Magnetism 25

  26. Solar Rotation • The sun rotates differentially • Equator – 25.1 days • 60° latitude - 30.8 days • Poles - 36 days • Interior - 26.9 days 26

  27. Figure 9.18Solar Rotation 27

  28. Solar Rotation • Rope demonstration • Every 11 years, the polarity of the magnetic fields reverse. • Number of sunspots follows this 11 year cycle. • Most recent maximum was in 2001. • Solar Cycle - Two complete reversals of the magnetic field. Two sunspot cycles, or 22 years. 28

  29. Figure 9.19Sunspot Cycle 29

  30. Figure 9.20Maunder Minimum 30

  31. Active Regions • Sites of explosive events on the photosphere. • Most associated with sunspots (magnetic fields) • Prominences - loops or sheets of glowing gas ejected from an active region. • Flares - more violent; may cause pressure waves • Coronal Mass Ejection - “bubbles” of ionized gas that separate and escape from the corona. If these hit Earth, they disrupt Earth’s magnetic field. 31

  32. Figure 9.21Solar Prominences - ionized gas follows field lines 32

  33. Figure 9.22Solar Flare - more violent; may cause pressure waves 33

  34. Figure 9.23Coronal Mass Ejection - view from SOHO (Solar and Heliospheric Observatory.) 34

  35. As the Sun rotates, an individual sunspot can be tracked across its face. From Eastern to Western limb, this takes about: A) 12 hours B) A week C) Two weeks D) A month E) 5.5 years 35

  36. As the Sun rotates, an individual sunspot can be tracked across its face. From Eastern to Western limb, this takes about: A) 12 hours B) A week C) Two weeks D) A month E) 5.5 years 36

  37. Solar Interior/ Nuclear Fusion 37

  38. What about the internal structure? 38

  39. Solar Composition 39

  40. Figure 9.2Solar Structure 40

  41. What about the internal structure? • Core - • temperatures hot enough for nuclear reactions • Radiation Zone - • Temperatures cooler, so no nuclear reactions. • Hot enough so everything is ionized. • Atoms can’t absorb photons. • Convection Zone - • Temperature cooler. • Atoms form and can absorb radiation. 41

  42. Figure 9.6Solar Interior 42

  43. How do we know what is inside the Sun? 43

  44. How do we know what is inside the Sun? • Standard model 44

  45. Figure 9.4Stellar Balance 45

  46. Figure 9.5Solar Oscillations 46

  47. Figure 9.7Solar Convection 47

  48. Figure 9.8Solar Granulation 48

  49. Figure 9.11Solar Spicules 49

  50. Typically, a granule in the photosphere of the sun is about the size of? A) A city, ~20-30 kilometers across. B) Texas, ~1000 km across. C) The Earth, ~12,000 km across. D) Jupiter, ~100,000 km across. 50

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