1. Copyright © 2010 Pearson Education, Inc. Lecture Outline Chapter 2 Light and Matter

2. Copyright © 2010 Pearson Education, Inc. Chapter 2 Light and Matter

3. Copyright © 2010 Pearson Education, Inc. Units of Chapter 2 Information from the Skies Waves in What? The Electromagnetic Spectrum Thermal Radiation Spectroscopy The Formation of Spectral Lines The Doppler Effect Summary of Chapter 2

4. Copyright © 2010 Pearson Education, Inc. Lunar eclipse 27 Sept 2015

5. Copyright © 2010 Pearson Education, Inc. 2.1 Information from the Skies Electromagnetic radiation: Transmission of energy through space without physical connection through varying electric and magnetic fields Example: Light This is the only way we can learn about astronomical objects beyond our physical reach

6. Copyright © 2010 Pearson Education, Inc. 2.1 Information from the Skies Wave motion: Transmission of energy without the physical transport of material

7. Copyright © 2010 Pearson Education, Inc. 2.1 Information from the Skies Example: Water wave Water just moves up and down. Wave travels and can transmit energy.

8. Copyright © 2010 Pearson Education, Inc. 2.1 Information from the Skies Frequency: Number of wave crests that pass a given point per second Period: Time between passage of successive crests Relationship: Period = 1 / Frequency

9. Copyright © 2010 Pearson Education, Inc. 2.1 Information from the Skies Wavelength: Distance between successive crests Velocity: Speed at which crests move Relationship: Velocity = Wavelength / Period

10. Copyright © 2010 Pearson Education, Inc. 2.2 Waves in What? Diffraction: The bending of a wave around an obstacle Interference: The sum of two waves; may be larger or smaller than the original waves

11. Copyright © 2010 Pearson Education, Inc. **: 2.2 Waves in What? Water waves, sound waves, and so on, travel in a medium (water, air, …). Electromagnetic waves need no medium. Created by accelerating charged particles

12. Copyright © 2010 Pearson Education, Inc. 2.2 Waves in What? Magnetic and electric fields are inextricably intertwined. A magnetic field, such as the Earth’s shown here, exerts a force on a moving charged particle.

13. Copyright © 2010 Pearson Education, Inc. 2.2 Waves in What? Electromagnetic waves: Oscillating electric and magnetic fields; changing electric field creates magnetic field, and vice versa

14. Copyright © 2010 Pearson Education, Inc. 2.3 The Electromagnetic Spectrum The visible spectrum is only a small part of the total electromagnetic spectrum. Different colors of light are distinguished by their frequency and wavelength.

15. Copyright © 2010 Pearson Education, Inc. 2.3 The Electromagnetic Spectrum Different parts of the full electromagnetic spectrum have different names, but there is no limit on possible wavelengths.

16. Copyright © 2010 Pearson Education, Inc. 2.3 The Electromagnetic Spectrum Note that the atmosphere is only transparent at a few wavelengths – the visible, the near infrared, and the part of the radio spectrum with frequencies higher than the AM band. This means that our atmosphere is absorbing a lot of the electromagnetic radiation impinging on it, and also that astronomy at other wavelengths must be done above the atmosphere. Also note that the horizontal scale is logarithmic – each tick is a factor of 10 smaller or larger than the next one. This allows the display of the longest and shortest wavelengths on the same plot.

17. Copyright © 2010 Pearson Education, Inc. 22 sept: 2.4 Thermal Radiation Blackbody spectrum: Radiation emitted by any object depends only on its temperature, and that radiation is across a range of frequencies (colors) for a given temperature Compare the campfire coals to the sun.

18. Copyright © 2010 Pearson Education, Inc. More Precisely 2-1: The Kelvin Temperature Scale Kelvin temperature scale: All thermal motion ceases at 0 K. Water freezes at 273 K and boils at 373 K.

19. Copyright © 2010 Pearson Education, Inc. 2.4 Thermal Radiation Radiation laws: 1. Peak wavelength is inversely proportional to temperature. Look at http://phet.colorado.edu/e n/simulation/blackbody- spectrum for nice view of blackbody changes http://phet.colorado.edu/e n/simulation/blackbody- spectrum

20. Copyright © 2010 Pearson Education, Inc. 2.4 Thermal Radiation Radiation laws: 2. Total energy emitted is proportional to fourth power of temperature.

21. Copyright © 2010 Pearson Education, Inc. Spectroscopy is key to astronomy Spectroscope: Splits light into component colors

22. Copyright © 2010 Pearson Education, Inc. 2.5 Spectroscopy Emission lines: Single frequencies emitted by particular atoms

23. Copyright © 2010 Pearson Education, Inc. Emission spectrum can be used to identify elements. It is a unique “fingerprint”. 2.5 Spectroscopy

24. Copyright © 2010 Pearson Education, Inc. Absorption spectrum: If a continuous spectrum passes through a cool gas, atoms of the gas will absorb the same frequencies they emit. 2.5 Spectroscopy

25. Copyright © 2010 Pearson Education, Inc. 2.5 Spectroscopy Absorption spectrum of the Sun in 48 rows. And this is only the visible spectrum. There’s more! Helium was discovered for the first time, in 1868. It was discovered on the sun using spectral lines.

26. Copyright © 2010 Pearson Education, Inc. Kirchhoff’s laws: Luminous solid, liquid, or dense gas produces continuous spectrum. Low-density hot gas produces emission spectrum. Continuous spectrum incident on cool, thin gas produces absorption spectrum. 2.5 Spectroscopy

27. Copyright © 2010 Pearson Education, Inc. Kirchhoff’s laws illustrated 2.5 Spectroscopy Just know there are 2 separate ways to gain info from a material, and 3 ways from a light source.

28. Copyright © 2010 Pearson Education, Inc. Existence of spectral lines required new model of atom, so that only certain amounts of energy could be emitted or absorbed. Bohr model had certain allowed orbits for electron. 2.6 The Formation of Spectral Lines

29. Copyright © 2010 Pearson Education, Inc. Emission energies correspond to energy differences between allowed levels. Modern model has electron “cloud” rather than orbit. 2.6 The Formation of Spectral Lines

30. Copyright © 2010 Pearson Education, Inc. Atomic excitation leads to emission. (a) Direct decay (b) Cascade 2.6 The Formation of Spectral Lines

31. Copyright © 2010 Pearson Education, Inc. Absorption spectrum: Created when atoms absorb photons of right energy for excitation Multielectron atoms: Much more complicated spectra, many more possible states Ionization changes energy levels. 2.6 The Formation of Spectral Lines

32. Copyright © 2010 Pearson Education, Inc. Molecular spectra are much more complex than atomic spectra, even for hydrogen. (a) Molecular hydrogen(b) Atomic hydrogen 2.6 The Formation of Spectral Lines

33. Copyright © 2010 Pearson Education, Inc. Quiz 2014 1.Explain what is spectroscopy? Give an example. 2.Explain how opacity in the atmosphere affects electromagnetic waves from space. 3.Consider the whole electromagnetic spectrum and answer these: a)The range visible to humans is (narrow or wide) b)High energy waves are on the (left or right)

34. Copyright © 2010 Pearson Education, Inc. Quiz 2013 October 1.Fill in the blanks for the various categories of EM waves: Radio*Microwave* _______*visible* _______* x-ray*________ 2.Name 3 types of information we can learn about a star from our telescopes. 3.Circle the names of people who became famous because they used a telescope: Brahe, Kepler, Aristotle, Newton, Galileo, Captain Hook, Dr. Fisher

35. Copyright © 2010 Pearson Education, Inc. 29 Sept: 2.7 The Doppler Effect If one is moving toward a source of radiation, the wavelengths seem shorter; if moving away, they seem longer. Relationship between frequency and speed:

36. Copyright © 2010 Pearson Education, Inc. Depends only on the relative motion of source and observer 2.7 The Doppler Effect A good physlet http://www.lon- capa.org/~mmp/app list/doppler/d.htm http://www.lon- capa.org/~mmp/app list/doppler/d.htm

37. Copyright © 2010 Pearson Education, Inc. 2.7 The Doppler Effect The Doppler effect shifts an object’s entire spectrum either toward the red or toward the blue.

38. Copyright © 2010 Pearson Education, Inc. Doppler effect for practical use So, that’s 1.0 x 10 8 m/s which is only 220,000,000 mph.

39. Copyright © 2010 Pearson Education, Inc. Things we learn from the spot of light in the sky 1.Position in the sky and motion relative to other stars 2.Intensity or brightness 3.Frequency of the light, “color” Wavelengths of the light peaks 4.Movement of the object toward or away from us (doppler) 5.Spectroscopic composition info of the object 6.Spectroscopic composition of any cloud of gas near the object 7.Temperature of the object

40. Copyright © 2010 Pearson Education, Inc. Summary of Chapter 2 Wave: period, wavelength, amplitude Electromagnetic waves created by accelerating charges Visible spectrum is different wavelengths of light. Entire electromagnetic spectrum: includes radio waves, infrared, visible light, ultraviolet, X-rays, gamma rays can tell the temperature of an object by measuring its blackbody radiation

41. Copyright © 2010 Pearson Education, Inc. Summary of Chapter 2, cont. Spectroscope splits light beam into component frequencies. Continuous spectrum is emitted by solid, liquid, and dense gas. Hot gas has characteristic emission spectrum. Continuous spectrum incident on cool, thin gas gives characteristic absorption spectrum.

42. Copyright © 2010 Pearson Education, Inc. Summary of Chapter 2, cont. Spectra can be explained using atomic models, with electrons occupying specific orbitals. Emission and absorption lines result from transitions between orbitals. Doppler effect can change perceived frequency of radiation. Doppler effect depends on relative speed of source and observer.