1. Chapter 11 Surveying the Stars

2. I.Parallax and distance. II.Luminosity and brightness Apparent Brightness (ignore “magnitude system” in book) Absolute Brightness or Luminosity Inverse-Square Law III.Stellar Temperatures Color, Spectral lines, Spectral Classification:OBAFGKM IV.Stellar sizes (radius) V.Stellar Masses Outline of Chapter 11 Part I: Properties of Stars Not exactly like book

3. Properties of Stars Our Goals for Learning How far away are stars? How luminous are stars? How hot are stars? How massive are stars? How large (radius) are stars?

4. I. Parallax and distance. p = parallax angle in arcseconds d (in parsecs) = 1/p 1parsec= 3.26 light years

7. I. Parallax and distance. Nearest Star: Alpha Centauri d = 4.3 light years (since 1 parsec = 3.26 light years) distance in parsecs = 4.3/3.26 = 1.32 What is the parallax of this star? d=1/p hence p=1/d p for nearest star is

8. I. Parallax and distance. Nearest Star: Alpha Centauri d = 4.3 light years (since 1 parsec = 3.26 light years) distance in parsecs = 4.3/3.26 = 1.32 What is the parallax of this star? d=1/p hence p=1/d p for nearest star is 0.76 arcseconds All other stars will have a parallax angle smaller than 0.76 arcseconds

9. 1. The distance of a star whose parallax is 0.25 arc seconds is Question 1

10. 1. The distance of a star whose parallax is 0.25 arc seconds is A. 4 parsecs B.40 light-years C.100 astronomical units D.0.25 parsec Question 1

11. 1. The distance of a star whose parallax is 0.25 arc seconds is A. 4 parsecs B.40 light-years C.100 astronomical units D.0.25 parsec Question 1

12. 1.Apparent Brightness (how bright it looks in the sky) 2.Absolute Brightness or Luminosity (energy/sec) 3.Inverse-Square Law II. Luminosity and Brightness

13. Energy passing through each sphere is the same The further the observer the lower the apparent brightness proportional to 1/d 2

14. Energy passing through each sphere is the same The further the observer the lower the apparent brightness proportional to 1/d 2 How many times fainter will the Sun seem from Jupiter (5AU) than from Earth?

15. Energy passing through each sphere is the same The further the observer the lower the apparent brightness proportional to 1/d 2 How many times fainter will the Sun seem from Jupiter (5AU) than from Earth? 25 times

17. 1.Apparent Brightness (how bright it looks in the sky) 2.Absolute Brightness or Luminosity (energy/sec) 3.Inverse-Square Law apparent brightness=(absolute brightness)/d 2 4.Examples: light bulbs at different distances II. Luminosity and Brightness

18. 1.Apparent Brightness (how bright it looks in the sky) 2.Absolute Brightness or Luminosity (energy/sec) 3.Inverse-Square Law apparent brightness=(absolute brightness)/d 2 4.Examples of absolute brightness and apparent brightness: light bulbs at different distances a)10W, 1 meter away b)100W, 10 meters away c)20W, 2 meters away d)90W, 3 meters away II. Luminosity and Brightness

19. light bulbs at different distances a)10W, 1 meter away b)100W, 10 meters away c)20W, 2 meters away d)90W, 3 meters away Use formula: apparent brightness=(absolute brightness)/d 2 Which one is faintest? Brightest? II. Luminosity and Brightness

20. light bulbs at different distances a)10W, 1 meter away b)100W, 10 meters away c)20W, 2 meters away d)90W, 3 meters away Which one is faintest? b Brightest? a and d  Watts is a unit of energy/sec (power) II. Luminosity and Brightness

21. Review of distance, apparent brightness, absolute (intrinsic) brightness and luminosity Distance: If you know the parallax “p” (in arcseconds) you can calculate the distance “d” (in parsecs) d=1/p (1parsec= 3.26 lightyears) Apparent brightness: how bright a star looks in the sky The inverse-square Law: light from stars gets fainter as the inverse square of the distance (apparent brightness is proportional to 1/d 2). If we know the apparent brightness and the distance to a star we can calculate its absolute (intrinsic) brightness: apparent brightness = (absolute brightness)/d 2 Luminosity (energy/sec) is equivalent to absolute brightness (analogy with light bulbs: Watts)

22. 1. Two stars have parallaxes of 0.1 arc seconds and 0.01 arc seconds, respectively, if the stars are equally luminous, how much brighter will the near one appear than the farther one? Question 2

23. 1. Two stars have parallaxes of 0.1 arc seconds and 0.01 arc seconds, respectively, if the stars are equally luminous, how much brighter will the near one appear than the farther one? (Hint: calculate the distance first and then estimate the apparent brightness) Question 2

24. 1. Two stars have parallaxes of 0.1 arc seconds and 0.01 arc seconds, respectively, if the stars are equally luminous, how much brighter will the near one appear than the farther one? (Hint: calculate the distance first and then estimate the apparent brightness) A.100 B.1000 C.10,000 D.400 Question 2

25. I.Parallax and distance. II.Luminosity and brightness Apparent Brightness Absolute Brightness or Luminosity Inverse-Square Law III.Stellar Temperatures Color, Spectral lines, Spectral Classification:OBAFGKM IV.Stellar sizes (radius) V.Stellar Masses Outline of Chapter 11 Part I

26. How hot are stars?

27. 1.Color ( hotter > bluer; cooler > redder) 2.Spectral lines 3.Spectral Classification: OBAFGKM (from hottest to coldest) III. Stellar Temperatures

28. hotter  brighter, cooler  dimmer hotter  bluer, cooler  redder Laws of Thermal Radiation (from Ch. 5)

29. Hottest stars: blue Coolest stars: red (Sun’s surface is about 6,000 K)

30. Lines in a star’s spectrum correspond to a spectral type that reveals its temperature: O B A F G K M (Hottest) (Coolest)

31. Table 11.1

32. Luminosity is proportional to surface area (how large) x temperature (how hot): L= 4  R 2  T 4 If we can measure the Luminosity and the temperature of a star we can tell how large its raduis is. IV. Stellar sizes (radius)

33. Luminosity is proportional to surface area x temperature: L= 4  R 2  T 4 If we can measure the Luminosity and the temperature of a star we can tell how large its raduis is. IV. Stellar sizes (radius)

34. Summary of Ch 11 Part I Distance: If you know the parallax “p” (in arcseconds) you can calculate the distance “d” (in parsecs) d=1/p (1parsec= 3.26 lightyears) Apparent brightness: how bright a star looks in the sky The inverse-square Law: light from stars gets fainter as the inverse square of the distance (brightness  proportional to 1/d 2). If we know the apparent brightness and the distance to a star we can calculate its absolute (intrinsic) brightness: apparent brightness = (absolute brightness)/d 2 Luminosity (energy/sec) is equivalent to absolute brightness L = 4  R 2  T 4 If we can measure the luminosity and the temperature of a star we can tell how large it is. Binary stars allow us to determine stellar masses

35. Summary of Ch 11 Part I Distance: If you know the parallax “p” (in arcseconds) you can calculate the distance “d” (in parsecs) d=1/p (1parsec= 3.26 lightyears) Apparent brightness: how bright a star looks in the sky The inverse-square Law: light from stars gets fainter as the inverse square of the distance (brightness  proportional to 1/d 2). If we know the apparent brightness and the distance to a star we can calculate its absolute (intrinsic) brightness: apparent brightness = (absolute brightness)/d 2 Luminosity (energy/sec) is equivalent to absolute brightness L = 4  R 2  T 4 If we can measure the luminosity and the temperature of a star we can tell how large it is. Binary stars allow us to determine stellar masses

36. Binary Stars Definition Three main types of Binary Stars Visual Spectroscopic Eclipsing Stellar Masses and Densities

37. Definition: When two stars are in orbit around their center of mass Three main types of Binary Stars Visual: orbits Spectroscopic: Review of Doppler effect, spectral lines, double and single lines Eclipsing: masses and radii of stars Stellar Masses and Densities Binary Stars

38. Visual Binary

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

42. Approaching stars: more energy, spectral lines undergo a blue shift Receding stars: less energy, spectral lines undergo a red shift  / = v/c Radial Velocity

43. Spectroscopic Binary

44. We determine the orbit by measuring Doppler shifts

45. Eclipsing Binary We can measure periodic eclipses

46. Eclipsing Binary: Masses and Radii

47. Radii of Stars

48. Stellar Masses

49. Stellar Densities High Same as water Low

50. Properties of Stars Our Goals for Learning How far away are stars? How luminous are stars? How hot are stars? How massive are stars? How large (radius) are stars?

51. I.The Hertzprung-Russell (H-R) Diagram: Surface Temperature Luminosity Analogy: horsepower vs weight Where Stars plot is the H-R diagram Main Sequence: 90% of all stars Giants, Supergiants, White Dwarfs Outline of Ch 11 part 2: The H-R Diagram

52. Figure 11.5 Team Responsible for Stellar Classification in Late 1800s and Early 1900s