1. Chapter 5: Light

2. Light! Measuring the speed of light
Early attempts to measure the speed of light were done in 1638 by an apprentice of Galileo
Hilltop to hilltop around Padua Italy using hand lanterns “The speed of light is at least 10 times faster than the speed of sound.”

3. Rømer estimates the speed of light
1676…Olaus Rømer Eclipses of Io by Jupiter. Found speed to be finite but very large (didn’t know diameter of Earth’s orbit)

4. 1850…Fizeau & Foucault measure speed to be about 300,000 km/s
By the 1800’s two Frenchmen were able to measure the speed of light with some accuracy
1850…Fizeau & Foucault measure speed to be about 300,000 km/s

5. The Speed of Light in vacuum is a fundamental constant of the universe
The speed of light in vacuum is the same for all observers everywhere in the universe regardless of their circumstances. We define the speed of light to be
c = m/s exactly.
For most calculations, though, we can use 3.00 x108 m/s

6. We can use the speed of light to define distances
The meter is defined as
The lightyear is defined as
The year used in the definition is the sidereal year: 365 days 6 hours 9 minutes and 9.5 seconds

7. When light travels through anything other than vacuum it moves slower
We define the index of refraction of a material to be the ratio of the speed of light in vacuum to the speed of light in the material

8. What is light?

9. Just as a cork bobbing in water creates waves in the water, charges “bobbing” in space create electric and magnetic waves

10. “Light” is an Electromagnetic Wave

11. Basic Properties of Waves
Wavelength = l in meters Frequency = f in cycles per second or Hertz (Hz) Speed = v in meters per second

12. Each “color” is characterized by its wavelength
Using c = lf we can see that the frequency of visible light is in the 1014 Hz range

13. Watch ClassAction Light & Spectra module EM Spectrum Module animation
Visible light is only a very small part of the Electromagnetic Spectrum
Watch ClassAction Light & Spectra module EM Spectrum Module animation

14. Photon Torpedoes Away!
Light also behaves like a particle: a photon
c = speed of light n = frequency l = wavelength
But didn’t we say that light was a wave? What’s going on? How can it be both?

15. To understand how light can be both a wave and a particle, we need new physics
Quantum Mechanics deals with the very small like atoms, molecules, subatomic particles and light particles.

16. The Bohr Atom
An early model of the atom. Like a mini-solar system, the electrons orbit around tiny nucleus
The Nucleus: Protons, Neutrons and 99.98% of the mass
The problem is, it doesn’t work! According to electromagnetic theory, the electron will radiate away all its energy and collapse into the nucleus in a fraction of a second.

17. The Quantum Mechanical Atom
The Heisenberg Uncertainty Principle of quantum mechanics says you can’t tell where the electron is, only the probability of where it might be. The electron is “delocalized”.

18. The energy associated with the electron is quantized

19. Light comes from Electron Transitions
The energy of the emitted photon is exactly equal to the difference in energy between the two states

20. A hot gas will emit specific wavelengths

21. An atom can also absorb a photon if it has the right energy

22. Most atoms have many emission lines

23. Absorption and emission lines have the same wavelengths
The same states are involved in emission and absorption. The only difference between emission and absorption is the way the electron is changing. For emission the electron loses energy and thus goes from a high energy state to a low energy state. For absorption, the electron gains energy and so goes from a low energy state to a high energy state.
Three Views Spectrum Demonstrator in ClassAction Light & Spectra module

24. The Solar Spectrum has lots of absorption lines
All the naturally occurring elements are present in the Sun

25. The Doppler Effect
The light is redshifted if the source is moving away from the observer, blueshifted if it is moving towards
+ If the source is moving away from the observer
- If the source is moving towards the observer

26. What do we mean when we say something is hot?
On a microscopic scale, temperature is a measure of how fast things are moving

27. In astronomy, we use the absolute temperature scale
Absolute zero is the temperature at which all motion stops. Quantum mechanics says that isn’t possible so you can never reach absolute zero

28. All objects emit light according to their temperature: Blackbody Radiation

29. Hotter objects glow brighter and become bluer

30. The Blackbody Spectrum
The hotter the object is, the shorter the wavelength of maximum intensity. The hotter the object is, the greater the total intensity of the light it emits is.

31. Objects reach equilibrium between energy absorbed and energy emitted

32. There is more to the temperature of a planet than just sunlight absorbed and blackbody emission

33. What can be learned from the light of a planet or star?
Surface Temperature…Blackbody Spectrum
Elemental Composition…Emission/Absorption
Radial Motion…Doppler Effect
Rotation…Doppler Line Broadening
Surface Pressure/Density…Pressure Broadening