Next quiz: Monday, October 24

Transcription

1 No homework for Wednesday Read Chapter 8! Next quiz: Monday, October 24 1

2 Chapter 7 Atoms and Starlight

3 Types of Spectra: Pictorial Some light sources are comprised of all colors (white light). Other light sources contain just a few colors. Some are missing just a few colors. 3

4 Emission Spectrum: Graphical 4

5 Absorption Spectrum: Graphical Absorption lines 5

6 Atomic Structure An atom consists of an atomic nucleus (protons and neutrons) and a cloud of electrons surrounding it. Almost all of the mass is contained in the nucleus, while almost all of the space is occupied by the electron cloud. Grapeseed in the middle of 4.5 football fields!

7 Electron Orbits Electron orbits in the electron cloud are restricted to very specific radii and energies. These characteristic electron energies are different for each individual element.

8 Electron Orbits Electron orbits in the electron cloud are restricted to very specific radii and energies. r 1, E 1 These characteristic electron energies are different for each individual element.

9 Electron Orbits Electron orbits in the electron cloud are restricted to very specific radii and energies. r 2, E 2 r 1, E 1 These characteristic electron energies are different for each individual element.

10 Electron Orbits Electron orbits in the electron cloud are restricted to very specific radii and energies. r 3, E 3 r 2, E 2 r 1, E 1 These characteristic electron energies are different for each individual element.

11 Atomic Transitions An electron can be kicked into a higher orbit when it absorbs a photon with exactly the right energy. The photon is absorbed, and the electron is in an excited state. E ph = E 3 E 1 E ph = E 4 E 1 Wrong energy (Remember that E ph = h*f) All other photons pass by the atom unabsorbed.

12 Electron Orbits & Emission 9

13 Atomic Transitions Electrons spontaneously decay back down to ground state See animation at: 10

14 Continuous 11

15 Emission 12

16 Absorption threeviewsspectra.html 13

17 Kirchhoff s Laws of Radiation (1) 1. A solid, liquid, or dense gas at non-zero temperature will radiate at all wavelengths and thus produce a continuous spectrum.

18 Kirchhoff s Laws of Radiation (2) 2. A low-density gas excited to emit light will do so at specific wavelengths and thus produce an emission spectrum. Light excites electrons in atoms to higher energy states Transition back to lower states emits light at specific frequencies

19 Kirchhoff s Laws of Radiation (3) 3. If light comprising a continuous spectrum passes through a cool, low-density gas, the result will be an absorption spectrum. Light excites electrons in atoms to higher energy states Frequencies corresponding to the transition energies are absorbed from the continuous spectrum.

20 The Spectra of Stars

21 The Spectra of Stars The inner, dense layers of a star produce a continuous (blackbody) spectrum.

22 The Spectra of Stars The inner, dense layers of a star produce a continuous (blackbody) spectrum. Cooler surface layers absorb light at specific frequencies.

23 The Spectra of Stars The inner, dense layers of a star produce a continuous (blackbody) spectrum. Cooler surface layers absorb light at specific frequencies. => Spectra of stars are absorption spectra.

24 H He Ne Kr 18

25 Since pattern is unique for every element, the emission spectrum serves as an atomic fingerprint, telling us about the composition of celestial objects. H He Ne Kr 18

26 19

27 20

28 The specific wavelengths seen in an emission line spectrum are due to A) photons dropping to lower energy orbits. B) photons jumping to higher energy orbits. C) electrons dropping to lower energy orbits. 21

29 Below is a model 3-level hydrogen atom. Each of the circles represents an energy level/ orbit around the nucleus, from the ground state (n = 1) to the second excited state (n= 3). The spacing of each circle is proportional to the energy of each orbit. The arrows represent electron transitions. Which transition will result in the emission of the longest wavelength photon? A) A B) B C) C 22

30 Which transitions were responsible for each of these absorption lines? a) A: 1-2 B: 2-4 C: 1-4 b) A: 1-4 B: 2-4 C: 1-2 c) A: 4-1 B: 4-2 C:

31 Chapter 8 The Sun

32 Guidepost In this chapter, you can use the interaction of light and matter to reveal the secrets of the sun. Because the sun is a typical star, what you are about to learn are the secrets of the stars. This chapter will help you answer three essential questions: What do you see when you look at the sun? How does the sun make its energy? What causes sunspots and other forms of solar activity? The sun will give you a close-up look at a star.

33 Outline I. The Solar Atmosphere A. The Photosphere B. The Chromosphere C. The Solar Corona D. Helioseismology II. Nuclear Fusion in the Sun III. Solar Activity

34 Outline I. The Solar Atmosphere A. The Photosphere B. The Chromosphere C. The Solar Corona D. Helioseismology Today! II. Nuclear Fusion in the Sun III. Solar Activity

35 General Properties Average star

36 General Properties Average star Spectral type G2 - O B A F G K M

37 General Properties Average star Spectral type G2 - O B A F G K M Only appears so bright because it is so close.

38 General Properties Average star Spectral type G2 - O B A F G K M Only appears so bright because it is so close. 109 times Earth s diameter

39 General Properties Average star Spectral type G2 - O B A F G K M Only appears so bright because it is so close. 109 times Earth s diameter 333,000 times Earth s mass

40 General Properties Average star Spectral type G2 - O B A F G K M Only appears so bright because it is so close. 109 times Earth s diameter 333,000 times Earth s mass Consists entirely of gas (av. density = 1.4 g/cm 3 )

41 General Properties Average star Spectral type G2 - O B A F G K M Only appears so bright because it is so close. 109 times Earth s diameter 333,000 times Earth s mass Consists entirely of gas (av. density = 1.4 g/cm 3 ) Central temperature = 15 million K

42 General Properties Average star Spectral type G2 - O B A F G K M Only appears so bright because it is so close. 109 times Earth s diameter 333,000 times Earth s mass Consists entirely of gas (av. density = 1.4 g/cm 3 ) Central temperature = 15 million K Surface temperature = 5800 K

43 Very Important Warning: Never look directly at the sun through a telescope or binoculars!!!

44 Very Important Warning: Never look directly at the sun through a telescope or binoculars!!! This can cause permanent eye damage even blindness.

45 Very Important Warning: Never look directly at the sun through a telescope or binoculars!!! This can cause permanent eye damage even blindness. Use a projection technique or a special sun viewing filter.

46 The Solar Atmosphere

47 The Solar Atmosphere Only visible during solar eclipses

48 The Solar Atmosphere Only visible during solar eclipses Apparent surface of the sun

49 The Solar Atmosphere Only visible during solar eclipses Apparent surface of the sun Solar interior

50 The Solar Atmosphere Only visible during solar eclipses Apparent surface of the sun Solar interior Temp. incr. inward

51 The Solar Atmosphere Only visible during solar eclipses Apparent surface of the sun Heat Flow Solar interior Temp. incr. inward

52 The Photosphere Apparent surface layer of the sun

53 The Photosphere Apparent surface layer of the sun Depth 500 km

54 The Photosphere Apparent surface layer of the sun Depth 500 km Temperature 5800 o K

55 The Photosphere Apparent surface layer of the sun Depth 500 km Temperature 5800 o K Highly opaque (H - ions)

56 The Photosphere Apparent surface layer of the sun Depth 500 km Temperature 5800 o K Highly opaque (H - ions) Absorbs and re-emits radiation produced in the sun

57 The Photosphere Apparent surface layer of the sun Depth 500 km Temperature 5800 o K Highly opaque (H - ions) Absorbs and re-emits radiation produced in the sun The solar corona

58 Energy Transport in the Photosphere Energy generated in the sun s center must be transported outward.

59 Energy Transport in the Photosphere Energy generated in the sun s center must be transported outward. Near the photosphere, this happens through Convection:

60 Energy Transport in the Photosphere Energy generated in the sun s center must be transported outward. Near the photosphere, this happens through Convection: Bubbles of hot gas rising up

61 Energy Transport in the Photosphere Energy generated in the sun s center must be transported outward. Near the photosphere, this happens through Cool gas sinking down Convection: Bubbles of hot gas rising up

62 Energy Transport in the Photosphere Energy generated in the sun s center must be transported outward. Near the photosphere, this happens through Cool gas sinking down Convection: Bubbles of hot gas rising up 1000 km

63 Energy Transport in the Photosphere Energy generated in the sun s center must be transported outward. Near the photosphere, this happens through Cool gas sinking down Convection: Bubbles of hot gas rising up 1000 km Bubbles last for min

64 Granulation is the visible consequence of convection.

65 The Chromosphere

66 The Chromosphere Region of sun s atmosphere just above the photosphere

67 The Chromosphere Region of sun s atmosphere just above the photosphere Visible, UV, and X-ray lines from highly ionized gases

68 The Chromosphere Region of sun s atmosphere just above the photosphere Visible, UV, and X-ray lines from highly ionized gases Chromospheric structures visible in Hα emission (filtergram)

69 The Chromosphere Region of sun s atmosphere just above the photosphere Visible, UV, and X-ray lines from highly ionized gases Temperature increases gradually from 4500 o K to 10,000 o K, then jumps to 1 million o K Chromospheric structures visible in Hα emission (filtergram)

70 The Chromosphere Region of sun s atmosphere just above the photosphere Visible, UV, and X-ray lines from highly ionized gases Temperature increases gradually from 4500 o K to 10,000 o K, then jumps to 1 million o K Transition region Chromospheric structures visible in Hα emission (filtergram)

71 The Chromosphere Region of sun s atmosphere just above the photosphere Visible, UV, and X-ray lines from highly ionized gases Temperature increases gradually from 4500 o K to 10,000 o K, then jumps to 1 million o K Filaments Transition region Chromospheric structures visible in Hα emission (filtergram)

72 The Layers of the Solar Atmosphere

73 The Layers of the Solar Atmosphere Visible

74 The Layers of the Solar Atmosphere Visible Ultraviolet

75 The Layers of the Solar Atmosphere Visible Sun Spot Regions Ultraviolet

76 The Layers of the Solar Atmosphere Visible Sun Spot Regions Ultraviolet

77 The Layers of the Solar Atmosphere Visible Sun Spot Regions Ultraviolet Coronal activity, seen in visible light

78 The Layers of the Solar Atmosphere Visible Sun Spot Regions Ultraviolet Photosphere Coronal activity, seen in visible light

79 The Layers of the Solar Atmosphere Visible Sun Spot Regions Ultraviolet Photosphere Chromosphere Coronal activity, seen in visible light

80 The Layers of the Solar Atmosphere Visible Sun Spot Regions Ultraviolet Photosphere Corona Chromosphere Coronal activity, seen in visible light

81 The Magnetic Carpet of the Corona Corona contains very low-density, very hot (1 million o K) gas

82 The Magnetic Carpet of the Corona Corona contains very low-density, very hot (1 million o K) gas Coronal gas is heated through motions of magnetic fields anchored in the photosphere below ( magnetic carpet )

83 The Magnetic Carpet of the Corona Corona contains very low-density, very hot (1 million ok) gas Coronal gas is heated through motions of magnetic fields anchored in the photosphere below ( magnetic carpet ) Computer model of the magnetic carpet

84 What effect does the formation of negative hydrogen ions in the sun's photosphere have on solar observations? 1. We can view the sun's interior through special filters set to the wavelength of the absorption lines created by such ions. Concentrations of such ions form sunspots that allow us to track solar rotation. It divides the sun's atmosphere into three distinct, easily observable layers. The extra electron absorbs different wavelength photons making the photosphere opaque. These ions produce the "diamond ring" effect that is seen during total solar eclipses.

85 This diagram explains the structure of solar granules. Why is the center of a granule brighter than its edges? 1. The surface elevation is higher at the center. 2. The surface elevation is lower at the center. 3. The temperature is higher at the center. 4. The temperature is lower at the center. 5. The surface elevation is lower at the center.

86 The sun s atmospheric layers are all less dense than its interior. Based on this figure, which layer of the sun is responsible for the absorption lines in the solar spectrum? 1. Corona 2. Chromosphere 3. Photosphere 4. All the layers are responsible. 5. Both corona and chromosphere