1. Chapter 11 Surveying the Stars

2. 11.1 Properties of Stars Our goals for learning: How do we measure stellar luminosities? How do we measure stellar temperatures? How do we measure stellar masses?

3. How do we measure stellar luminosities? And why do we care? Let’s say we want to find out how far away a star is… We can’t measure the distance directly But we can easily measure the brightness And brightness is related to distance and luminosity

4. Luminosity and distance are not so easy.

5. Luminosity and distance are not so easy. However…

6. if we can relate brightness, luminosity, and distance…

7. we can calculate any of them if we know the other two.

8. This is very important and useful.

9. This is very important and useful. But first…

10. What is luminosity?

11. Luminosity: Amount of power a star radiates (joules/sec = watts)

12. Luminosity: Amount of power a star radiates (joules/sec = watts) Example: A100 W light bulb has a luminosity of 100 W

13. Luminosity: Amount of power a star radiates (joules/sec = watts) This is different from brightness:

14. Luminosity: Amount of power a star radiates (joules/sec = watts) This is different from brightness: Amount of starlight that reaches Earth (watts/square meter)

15. Thought Question These two stars have about the same luminosity— which one appears brighter? A. Alpha Centauri B. The Sun

16. Thought Question These two stars have about the same luminosity— which one appears brighter? A. Alpha Centauri B. The Sun

17. How are luminosity and brightness related?

18. Luminosity passing through each sphere is the same How are luminosity and brightness related?

19. Luminosity passing through each sphere is the same But the area increases How are luminosity and brightness related?

20. Luminosity passing through each sphere is the same But the area increases Area of sphere = 4πR 2 How are luminosity and brightness related?

21. Luminosity passing through each sphere is the same But the area increases Area of sphere = 4πR 2 Divide luminosity by area to get apparent brightness. How are luminosity and brightness related?

22. The relationship between apparent brightness and luminosity depends on distance: The Inverse Square Law for Light

23. Thought Question How would the apparent brightness of Alpha Centauri change if it were three times farther away? A. It would be only 1/3 as bright. B. It would be only 1/6 as bright. C. It would be only 1/9 as bright. D. It would be three times as bright.

24. Thought Question How would the apparent brightness of Alpha Centauri change if it were three times farther away? A. It would be only 1/3 as bright. B. It would be only 1/6 as bright. C. It would be only 1/9 as bright. D. It would be three times as bright.

25. Thought Question How would the apparent brightness of Alpha Centauri change if it were three times farther away? A. It would be only 1/3 as bright. B. It would be only 1/6 as bright. C. It would be only 1/9 as bright. D. It would be three times as bright.

26. The relationship between apparent brightness and luminosity depends on distance: Measuring brightness is easy, so if we know how far away a star is, we can calculate its luminosity:

27. The relationship between apparent brightness and luminosity depends on distance: Measuring brightness is easy, so if we know how far away a star is, we can calculate its luminosity:

28. The relationship between apparent brightness and luminosity depends on distance: Measuring brightness is easy, so if we know how far away a star is, we can calculate its luminosity: Or if we know its luminosity, we can calculate its distance:

29. The relationship between apparent brightness and luminosity depends on distance: Measuring brightness is easy, so if we know how far away a star is, we can calculate its luminosity: Or if we know its luminosity, we can calculate its distance:

30. So how far away are these stars?

31. Parallax is the apparent shift in position of a nearby object against a background of more distant objects. Introduction to Parallax

32. Apparent positions of the nearest stars shift by only about an arcsecond as Earth orbits the Sun, and the shift is smaller for more distant stars. Parallax of a Nearby Star

33. Apparent positions of the nearest stars shift by only about an arcsecond as Earth orbits the Sun, and the shift is smaller for more distant stars. These very small angles explain why the Greeks were unable to detect parallax with their naked eyes. Parallax of a Nearby Star

34. Apparent positions of the nearest stars shift by only about an arcsecond as Earth orbits the Sun, and the shift is smaller for more distant stars. These very small angles explain why the Greeks were unable to detect parallax with their naked eyes. This inability helped delay the acceptance of the geocentric universe for more than 1500 years. Parallax of a Nearby Star

35. The parallax angle depends on distance. Parallax Angle as a Function of Distance

36. Parallax is measured by comparing snapshots taken at different times and measuring the angular size of the star’s shift in position. Measuring Parallax Angle

37. Parallax is measured by comparing snapshots taken at different times and measuring the angular size of the star’s shift in position. Measuring Parallax Angle

39. This is a right triangle

40. That means we can use trigonometry

42. For small angles: sinp ≈ p

43. So for small angles:

44. If you express p in arcseconds and d in parsecs…

45. Parallax and Distance

46. The apparent brightness of stars varies over a wide range

47. And there is also a wide range of luminosity

48. Range of luminosities Most luminous stars: 10 6 L Sun (L Sun is luminosity of Sun)

49. Range of luminosities Most luminous stars: 10 6 L Sun Least luminous stars: 10 −4 L Sun (L Sun is luminosity of Sun)

50. Range of luminosities This is a wide range

51. Range of luminosities This is a wide range To compress it, the magnitude scale was devised, originally by the Greeks

52. Range of luminosities The Greeks assigned stars six magnitudes numbered from 1 to 6

53. Range of luminosities The brightest stars had a magnitude of 1 and the dimmest had a magnitude of 6

54. Range of luminosities The magnitudes in between differed from each other by about a factor of two

55. Range of luminosities The modern magnitude scale is based on a magnitude 1 star being 100 times brighter than a magnitude 6 star, so magnitudes differ in brightness by about a factor of 2.5

56. The Magnitude Scale

58. End 14 April 2008 Lecture

59. 11.1 Properties of Stars Our goals for learning: How do we measure stellar luminosities? How do we measure stellar temperatures? How do we measure stellar masses?

60. How do we measure stellar temperatures?

61. Every object emits thermal radiation with a spectrum that depends on its temperature.

62. An object of fixed size grows more luminous as its temperature rises. Relationship Between Temperature and Luminosity

63. An object of fixed size grows more luminous as its temperature rises. The color of the light also changes Relationship Between Temperature and Luminosity

64. 1.Hotter objects emit more light per unit area at all frequencies. 2.Hotter objects emit photons with a higher average energy. Properties of Thermal Radiation

65. The surface temperature of an object can be determined from the peak of its thermal radiation curve using Wien’s Law:

66. Hottest stars: 50,000 K Coolest stars: 3,000 K (Sun’s surface is 5,800 K)

67. Solid Molecules Neutral Gas Ionized Gas (Plasma) Level of ionization also reveals a star’s temperature. 10 K 10 2 K 10 3 K 10 4 K 10 5 K 10 6 K

68. Absorption lines in a star’s spectrum tell us its ionization level.

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

70. Remembering Spectral Types Oh, Be A Fine Girl/Guy, Kiss Me

71. Thought Question Which of the stars below is hottest? A. M star B. F star C. A star D. K star

72. Thought Question Which of the stars below is hottest? A. M star B. F star C. A star D. K star

73. Pioneers of Stellar Classification Annie Jump Cannon and the “calculators” at Harvard laid the foundation of modern stellar classification.

74. How do we measure stellar masses?

75. Orbit of a binary star system depends on strength of gravity

76. Types of Binary Star Systems Visual binary Eclipsing binary Spectroscopic binary About half of all stars are in binary systems.

77. Visual Binary We can directly observe the orbital motions of these stars.

78. Eclipsing Binary We can measure periodic eclipses. Exploring the Light Curve of an Eclipsing Binary Star System

79. Spectroscopic Binary We determine the orbit by measuring Doppler shifts.

80. Isaac Newton We measure mass using gravity. Direct mass measurements are possible only for stars in binary star systems. p = period a = average separation p 2 = a 3 4π 2 G (M 1 + M 2 )

81. Need both p and a to determine mass 1.Orbital period (p) 2.Orbital separation (a or r = radius) 3.Orbital velocity (v) For circular orbits, v = 2  r / p r M v

82. Most massive stars: 100 M Sun Least massive stars: 0.08 M Sun (M Sun is the mass of the Sun.)

83. What have we learned? How do we measure stellar luminosities? — If we measure a star’s apparent brightness and distance, we can compute its luminosity with the inverse square law for light. — Parallax tells us distances to the nearest stars. How do we measure stellar temperatures? — A star’s color and spectral type both reflect its temperature.

84. What have we learned? How do we measure stellar masses? — Newton’s version of Kepler’s third law tells us the total mass of a binary system, if we can measure the orbital period (p) and average orbital separation of the system (a).

85. 11.2 Patterns Among Stars Our goals for learning: What is a Hertzsprung–Russell diagram? What is the significance of the main sequence? What are giants, supergiants, and white dwarfs?

86. What is a Hertzsprung– Russell diagram?

87. Temperature Luminosity An H-R diagram plots the luminosities and temperatures of stars.

88. Generating an H-R Diagram

89. Most stars fall somewhere on the main sequence of the H-R diagram.

90. Stars with lower T than main-sequence stars with the same L, or with higher L than main-sequence stars with the same T, must have larger radii Large radius

91. Stars with lower T than main-sequence stars with the same L, or with higher L than main-sequence stars with the same T, must have larger radii This is because more of the cooler surface is required to give the same luminosity as a hotter star Large radius

92. Stars with lower T than main-sequence stars with the same L, or with higher L than main-sequence stars with the same T, must have larger radii This is because more of the cooler surface is required to give the same luminosity as a hotter star These are giants and supergiants Large radius

93. Small radius Stars with higher T than main-sequence stars with the same L, or with lower L than main-sequence stars with the same T, must have smaller radii

94. Small radius Stars with higher T than main-sequence stars with the same L, or with lower L than main-sequence stars with the same T, must have smaller radii These are white dwarfs

95. A star’s full classification includes spectral type and luminosity class

96. A star’s full classification includes spectral type (based on spectral line identities) and luminosity class

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

98. A star’s full classification includes spectral type (based on spectral line identities) and luminosity class (based on spectral line shapes, which are related to the size of the star)

99. “Pressure Broadening” is the basis of luminosity classification increasing size, decreasing pressure Source: http://spiff.rit.edu/classes/phys440/lectures/lumclass/lumclass.html

100. “Pressure Broadening” is the basis of luminosity classification increasing size, decreasing pressure Why do you think increasing the size would decrease the pressure at the surface of the star? Source: http://spiff.rit.edu/classes/phys440/lectures/lumclass/lumclass.html

101. A star’s full classification includes spectral type (line identities) and luminosity class (line shapes, related to the size of the star): I— supergiant II — bright giant III — giant IV — subgiant V — main sequence Examples:Sun — G2 V Sirius — A1 V Proxima Centauri — M5.5 V Betelgeuse — M2 I

102. Temperature Luminosity H-R diagram depicts: Temperature Color Spectral type Luminosity Radius

103. Temperature Luminosity Which star is the hottest? A B C D

104. Temperature Luminosity Which star is the hottest? A B C D A

105. Temperature Luminosity Which star is the most luminous? A B C D

106. Temperature Luminosity Which star is the most luminous? C A B C D

107. Temperature Luminosity Which star is a main-sequence star? A B C D

108. Temperature Luminosity Which star is a main-sequence star? D A B C D

109. Temperature Luminosity Which star has the largest radius? A B C D

110. Temperature Luminosity Which star has the largest radius? C A B C D

111. What is the significance of the main sequence?

112. Main-sequence stars are fusing hydrogen into helium in their cores, like the Sun. Luminous main- sequence stars are hot (blue). Less luminous ones are cooler (yellow or red).

113. Mass measurements of main-sequence stars show that the hot, blue stars are much more massive than the cool, red ones. High-mass stars Low-mass stars

114. The mass of a normal, hydrogen- burning main- sequence star determines its luminosity and spectral type! High-mass stars Low-mass stars

115. The mass of a normal, hydrogen- burning main- sequence star determines its luminosity and spectral type! The reason is gravitational equilibrium, also called hydrostatic pressure High-mass stars Low-mass stars

116. The core pressure and temperature of a higher-mass star need to be higher in order to balance gravity. A higher core temperature boosts the fusion rate, leading to greater luminosity. Hydrostatic Equilibrium

117. Stellar Properties Review Luminosity: from brightness and distance 10 −4 L Sun –10 6 L Sun Temperature: from color and spectral type 3,000 K – 50,000 K Mass: from period (p) and average separation (a) of binary-star orbit 0.08 M Sun – 100 M Sun

118. Stellar Properties Review Luminosity: from brightness and distance 10 −4 L Sun – 10 6 L Sun Temperature: from color and spectral type 3,000 K – 50,000 K Mass: from period (p) and average separation (a) of binary-star orbit 0.08 M Sun – 100 M Sun (0.08 M Sun ) (100 M Sun ) (0.08 M Sun )

119. Mass and Lifetime Sun’s life expectancy until core hydrogen (10% of total) is used up: ~10 billion years

120. Mass and Lifetime Sun’s life expectancy until core hydrogen (10% of total) is used up: ~10 billion years Life expectancy of a 10 M Sun star:

121. Mass and Lifetime Sun’s life expectancy until core hydrogen (10% of total) is used up: ~10 billion years Life expectancy of a 10 M Sun star: 10 times as much fuel, uses it 10 4 times as fast:

122. Mass and Lifetime Sun’s life expectancy until core hydrogen (10% of total) is used up: ~10 billion years Life expectancy of a 10 M Sun star: 10 times as much fuel, uses it 10 4 times as fast: ~10 million years

123. Mass and Lifetime Sun’s life expectancy until core hydrogen (10% of total) is used up: ~10 billion years Life expectancy of a 10 M Sun star: 10 times as much fuel, uses it 10 4 times as fast: ~10 million years Life expectancy of a 0.1 M Sun star:

124. Mass and Lifetime Sun’s life expectancy until core hydrogen (10% of total) is used up: ~10 billion years Life expectancy of a 10 M Sun star: 10 times as much fuel, uses it 10 4 times as fast: ~10 million years Life expectancy of a 0.1 M Sun star: 0.1 times as much fuel, uses it 0.01 times as fast:

125. Mass and Lifetime Sun’s life expectancy until core hydrogen (10% of total) is used up: ~10 billion years Life expectancy of a 10 M Sun star: 10 times as much fuel, uses it 10 4 times as fast: ~10 million years Life expectancy of a 0.1 M Sun star: 0.1 times as much fuel, uses it 0.01 times as fast: ~100 billion years

126. Main-Sequence Star Summary High-mass: High luminosity Short-lived Large radius Blue Low-mass: Low luminosity Long-lived Small radius Red

127. What are giants, supergiants, and white dwarfs?

128. Off the Main Sequence Stellar properties depend on both mass and age: those that have finished fusing H to He in their cores are no longer on the main sequence.

129. Off the Main Sequence Stellar properties depend on both mass and age: those that have finished fusing H to He in their cores are no longer on the main sequence. All stars become larger and redder after exhausting their core hydrogen: giants and supergiants.

130. Off the Main Sequence Stellar properties depend on both mass and age: those that have finished fusing H to He in their cores are no longer on the main sequence. All stars become larger and redder after exhausting their core hydrogen: giants and supergiants. Most stars end up small and white after fusion has ceased: white dwarfs.

131. Relationship between Main-Sequence Stellar Masses and Location on H-R Diagram

132. Main-sequence stars (to scale)Giants, supergiants, white dwarfs

133. Temperature Luminosity Which star is most like our Sun? A B C D

134. Temperature Luminosity Which star is most like our Sun? B A B C D

135. Temperature Luminosity Which of these stars will have changed the least 10 billion years from now? A B C D

136. Temperature Luminosity Which of these stars will have changed the least 10 billion years from now? C A B C D

137. Temperature Luminosity Which of these stars can be no more than 10 million years old? A B C D

138. Temperature Luminosity Which of these stars can be no more than 10 million years old? A A B C D

139. What have we learned? What is a Hertzsprung–Russell diagram? — An H-R diagram plots the stellar luminosity of stars versus surface temperature (or color or spectral type). What is the significance of the main sequence? — Normal stars that fuse H to He in their cores fall on the main sequence of an H-R diagram. — A star’s mass determines its position along the main sequence (high mass: luminous and blue; low mass: faint and red).

140. What have we learned? What are giants, supergiants, and white dwarfs? — All stars become larger and redder after core hydrogen burning is exhausted: giants and supergiants. — Most stars end up as tiny white dwarfs after fusion has ceased.

142. 11.3 Star Clusters Our goals for learning: What are the two types of star clusters? How do we measure the age of a star cluster?

143. What are the two types of star clusters?

144. Open cluster: A few thousand loosely packed stars

145. Globular cluster: Up to a million or more stars in a dense ball bound together by gravity

146. How do we measure the age of a star cluster?

147. Massive blue stars die first, followed by white, yellow, orange, and red stars. Visual Representation of a Star Cluster Evolving

148. Pleiades now has no stars with life expectancy less than around 100 million years. Main-sequence turnoff

149. The main- sequence turnoff point of a cluster tells us its age.

150. To determine accurate ages, we compare models of stellar evolution to the cluster data. Using the H-R Diagram to Determine the Age of a Star Cluster

151. Detailed modeling of the oldest globular clusters reveals that they are about 13 billion years old.

152. What have we learned? What are the two types of star clusters? — Open clusters are loosely packed and contain up to a few thousand stars. — Globular clusters are densely packed and contain hundreds of thousands of stars. How do we measure the age of a star cluster? — A star cluster’s age roughly equals the life expectancy of its most massive stars still on the main sequence.