The Nature of Light

1.1 The Propagation of Light – University Physics Volume 3 | OpenStax

  1. Key Terms
  2. Key Equations
  3. Summary
  4. Conceptual Questions
  5. Problems
  6. Additional Problems
3

Interference
  1. Introduction
  2. 3.1 Young’s Double-Slit Interference
  3. 3.2 Mathematics of Interference
  4. 3.3 Multiple-Slit Interference
  5. 3.4 Interference in Thin Films
  6. 3.5 The Michelson Interferometer
  7. Chapter Review
    1. Key Terms
    2. Key Equations
    3. Summary
    4. Conceptual Questions
    5. Problems
    6. Additional Problems
    7. Challenge Problems
4

Diffraction
  1. Introduction
  2. 4.1 Single-Slit Diffraction
  3. 4.2 Intensity in Single-Slit Diffraction
  4. 4.3 Double-Slit Diffraction
  5. 4.4 Diffraction Gratings
  6. 4.5 Circular Apertures and Resolution
  7. 4.6 X-Ray Diffraction
  8. 4.7 Holography
  9. Chapter Review
    1. Key Terms
    2. Key Equations
    3. Summary
    4. Conceptual Questions
    5. Problems
    6. Additional Problems
    7. Challenge Problems

Modern Physics
  1. 5

    Relativity
    1. Introduction
    2. 5.1 Invariance of Physical Laws
    3. 5.2 Relativity of Simultaneity
    4. 5.3 Time Dilation
    5. 5.4 Length Contraction
    6. 5.5 The Lorentz Transformation
    7. 5.6 Relativistic Velocity Transformation
    8. 5.7 Doppler Effect for Light
    9. 5.8 Relativistic Momentum
    10. 5.9 Relativistic Energy
    11. Chapter Review
      1. Key Terms
      2. Key Equations
      3. Summary
      4. Conceptual Questions
      5. Problems
      6. Additional Problems
  2. 6

    Photons and Matter Waves
    1. Introduction
    2. 6.1 Blackbody Radiation
    3. 6.2 Photoelectric Effect
    4. 6.3 The Compton Effect
    5. 6.4 Bohr’s Model of the Hydrogen Atom
    6. 6.5 De Broglie’s Matter Waves
    7. 6.6 Wave-Particle Duality
    8. Chapter Review
      1. Key Terms
      2. Key Equations
      3. Summary
      4. Conceptual Questions
      5. Problems
      6. Additional Problems
  3. 7

    Quantum Mechanics
    1. Introduction
    2. 7.1 Wave Functions
    3. 7.2 The Heisenberg Uncertainty Principle
    4. 7.3 The Schrӧdinger Equation
    5. 7.4 The Quantum Particle in a Box
    6. 7.5 The Quantum Harmonic Oscillator
    7. 7.6 The Quantum Tunneling of Particles through Potential Barriers
    8. Chapter Review
      1. Key Terms
      2. Key Equations
      3. Summary
      4. Conceptual Questions
      5. Problems
      6. Additional Problems
      7. Challenge Problems
  4. 8

    Atomic Structure
    1. Introduction
    2. 8.1 The Hydrogen Atom
    3. 8.2 Orbital Magnetic Dipole Moment of the Electron
    4. 8.3 Electron Spin
    5. 8.4 The Exclusion Principle and the Periodic Table
    6. 8.5 Atomic Spectra and X-rays
    7. 8.6 Lasers
    8. Chapter Review
      1. Key Terms
      2. Key Equations
      3. Summary
      4. Conceptual Questions
      5. Problems
      6. Additional Problems
  5. 9

    Condensed Matter Physics
    1. Introduction
    2. 9.1 Types of Molecular Bonds
    3. 9.2 Molecular Spectra
    4. 9.3 Bonding in Crystalline Solids
    5. 9.4 Free Electron Model of Metals
    6. 9.5 Band Theory of Solids
    7. 9.6 Semiconductors and Doping
    8. 9.7 Semiconductor Devices
    9. 9.8 Superconductivity
    10. Chapter Review
      1. Key Terms
      2. Key Equations
      3. Summary
      4. Conceptual Questions
      5. Problems
      6. Additional Problems
      7. Challenge Problems
  6. 10

    Nuclear Physics
    1. Introduction
    2. 10.1 Properties of Nuclei
    3. 10.2 Nuclear Binding Energy
    4. 10.3 Radioactive Decay
    5. 10.4 Nuclear Reactions
    6. 10.5 Fission
    7. 10.6 Nuclear Fusion
    8. 10.7 Medical Applications and Biological Effects of Nuclear Radiation
    9. Chapter Review
      1. Key Terms
      2. Key Equations
      3. Summary
      4. Conceptual Questions
      5. Problems
      6. Additional Problems
      7. Challenge Problems
  7. 11

    Particle Physics and Cosmology
    1. Introduction
    2. 11.1 Introduction to Particle Physics
    3. 11.2 Particle Conservation Laws
    4. 11.3 Quarks
    5. 11.4 Particle Accelerators and Detectors
    6. 11.5 The Standard Model
    7. 11.6 The Big Bang
    8. 11.7 Evolution of the Early Universe
    9. Chapter Review
      1. Key Terms
      2. Key Equations
      3. Summary
      4. Conceptual Questions
      5. Problems
      6. Additional Problems
      7. Challenge Problems

A | UnitsB | Conversion FactorsC | Fundamental ConstantsD | Astronomical DataE | Mathematical FormulasF | ChemistryG | The Greek Alphabet

Answer Key
  1. Chapter 1
  2. Chapter 2
  3. Chapter 3
  4. Chapter 4
  5. Chapter 5
  6. Chapter 6
  7. Chapter 7
  8. Chapter 8
  9. Chapter 9
  10. Chapter 10
  11. Chapter 11

Index

Learning Objectives

By the end of this section, you will be able to:

  • Determine the index of refraction, given the speed of light in a medium
  • List the ways in which light travels from a source to another location

The speed of light in a vacuum c is one of the fundamental constants of physics. As you will see when you reach Relativity, it is a central concept in Einstein’s theory of relativity. As the accuracy of the measurements of the speed of light improved, it was found that different observers, even those moving at large velocities with respect to each other, measure the same value for the speed of light. However, the speed of light does vary in a precise manner with the material it traverses. These facts have far-reaching implications, as we will see in later chapters.

The Speed of Light: Early Measurements

The first measurement of the speed of light was made by the Danish astronomer Ole Roemer (1644–1710) in 1675. He studied the orbit of Io, one of the four large moons of Jupiter, and found that it had a period of revolution of 42.5 h around Jupiter. He also discovered that this value fluctuated by a few seconds, depending on the position of Earth in its orbit around the Sun. Roemer realized that this fluctuation was due to the finite speed of light and could be used to determine c.

Roemer found the period of revolution of Io by measuring the time interval between successive eclipses by Jupiter. Figure 1.2(a) shows the planetary configurations when such a measurement is made from Earth in the part of its orbit where it is receding from Jupiter. When Earth is at point A, Earth, Jupiter, and Io are aligned. The next time this alignment occurs, Earth is at point B, and the light carrying that information to Earth must travel to that point. Since B is farther from Jupiter than A, light takes more time to reach Earth when Earth is at B. Now imagine it is about 6 months later, and the planets are arranged as in part (b) of the figure. The measurement of Io’s period begins with Earth at point A′A′ and Io eclipsed by Jupiter. The next eclipse then occurs when Earth is at point B′B′, to which the light carrying the information of this eclipse must travel. Since B′B′ is closer to Jupiter than A′A′, light takes less time to reach Earth when it is at B′B′. This time interval between the successive eclipses of Io seen at A′A′ and B′B′ is therefore less than the time interval between the eclipses seen at A and B. By measuring the difference in these time intervals and with appropriate knowledge of the distance between Jupiter and Earth, Roemer calculated that the speed of light was 2.0×108m/s,2.0×108m/s, which is 33% below the value accepted today.


The figure illustrates the orbits and positions of the earth about the sun and of Io about Jupiter when using Roemer’s method. Two configurations are shown. In both, Jupiter is between Io and the sun. In figure a, the Earth, Jupiter, and Io are aligned and the earth is moving away from Jupiter when the earth is at location A, and again at a slightly later location in earth’s orbit, B, so that A is somewhat closer to Io than B. In figure b, two similar locations of the earth but on the opposite side of its orbit from those shown in figure a, when Earth, Jupiter, and Io are again aligned but the earth is moving toward Jupiter, are labeled. The first of these locations is labeled as location A prime, and the later location as B prime, so that A prime is somewhat farther from Io than B prime. The light rays from Io to locations A, B, A prime, and B prime are shown.

Figure
1.2


Roemer’s astronomical method for determining the speed of light. Measurements of Io’s period done with the configurations of parts (a) and (b) differ, because the light path length and associated travel time increase from A to B (a) but decrease from A′A′ to B′B′ (b).

The first successful terrestrial measurement of the speed of light was made by Armand Fizeau (1819–1896) in 1849. He placed a toothed wheel that could be rotated very rapidly on one hilltop and a mirror on a second hilltop 8 km away (Figure 1.3). An intense light source was placed behind the wheel, so that when the wheel rotated, it chopped the light beam into a succession of pulses. The speed of the wheel was then adjusted until no light returned to the observer located behind the wheel. This could only happen if the wheel rotated through an angle corresponding to a displacement of (n+½)(n+½) teeth, while the pulses traveled down to the mirror and back. Knowing the rotational speed of the wheel, the number of teeth on the wheel, and the distance to the mirror, Fizeau determined the speed of light to be 3.15×108m/s,3.15×108m/s, which is only 5% too high.


The figure is an illustration of the set up for Fizeau’s method. A rotating toothed wheel is between a light source (shown as a light bulb in the illustration) and a mirror. The mirror and wheel are parallel to each other and perpendicular to the light beam. The light passes between the teeth on the way to the mirror, but is blocked by a tooth of the wheel when returning from the mirror.

Figure
1.3


Fizeau’s method for measuring the speed of light. The teeth of the wheel block the reflected light upon return when the wheel is rotated at a rate that matches the light travel time to and from the mirror.

The French physicist Jean Bernard Léon Foucault (1819–1868) modified Fizeau’s apparatus by replacing the toothed wheel with a rotating mirror. In 1862, he measured the speed of light to be 2.98×108m/s,2.98×108m/s, which is within 0.6% of the presently accepted value. Albert Michelson (1852–1931) also used Foucault’s method on several occasions to measure the speed of light. His first experiments were performed in 1878; by 1926, he had refined the technique so well that he found c to be (2.99796±4)×108m/s.(2.99796±4)×108m/s.

Today, the speed of light is known to great precision. In fact, the speed of light in a vacuum c is so important that it is accepted as one of the basic physical quantities and has the value

c=2.99792458×108m/s≈3.00×108m/sc=2.99792458×108m/s≈3.00×108m/s

1.1

where the approximate value of 3.00×108m/s3.00×108m/s is used whenever three-digit accuracy is sufficient.

Speed of Light in Matter

The speed of light through matter is less than it is in a vacuum, because light interacts with atoms in a material. The speed of light depends strongly on the type of material, since its interaction varies with different atoms, crystal lattices, and other substructures. We can define a constant of a material that describes the speed of light in it, called the index of refraction n:

n=cvn=cv

1.2

where v is the observed speed of light in the material.

Since the speed of light in matter is always less than c in matter and equals c only in a vacuum, the index of refraction is always greater than or equal to one; that is, n≥1n≥1. Table 1.1 gives the indices of refraction for some representative substances. The values are listed for a particular wavelength of light, because they vary slightly with wavelength. (This can have important effects, such as colors separated by a prism, as we will see in Dispersion.) Note that for gases, n is close to 1.0. This seems reasonable, since atoms in gases are widely separated, and light travels at c in the vacuum between atoms. It is common to take n=1n=1 for gases unless great precision is needed. Although the speed of light v in a medium varies considerably from its value c in a vacuum, it is still a large speed.

Medium n
Gases at 0°C0°C, 1 atm
Air 1.000293
Carbon dioxide 1.00045
Hydrogen 1.000139
Oxygen 1.000271
Liquids at 20°C20°C
Benzene 1.501
Carbon disulfide 1.628
Carbon tetrachloride 1.461
Ethanol 1.361
Glycerine 1.473
Water, fresh 1.333
Solids at 20°C20°C
Diamond 2.419
Fluorite 1.434
Glass, crown 1.52
Glass, flint 1.66
Ice (at 0°C)0°C) 1.309
Polystyrene 1.49
Plexiglas 1.51
Quartz, crystalline 1.544
Quartz, fused 1.458
Sodium chloride 1.544
Zircon 1.923
Table
1.1

Index of Refraction in Various Media


For light with a wavelength of 589 nm in a vacuum

Example
1.1

Speed of Light in Jewelry

Calculate the speed of light in zircon, a material used in jewelry to imitate diamond.

Strategy

We can calculate the speed of light in a material v from the index of refraction n of the material, using the equation n=c/v.n=c/v.

Solution

Rearranging the equation n=c/vn=c/v for v gives us

v=cn.v=cn.

The index of refraction for zircon is given as 1.923 in Table 1.1, and c is given in Equation 1.1. Entering these values in the equation gives

v=3.00×108m/s1.923=1.56×108m/s.v=3.00×108m/s1.923=1.56×108m/s.

Significance

This speed is slightly larger than half the speed of light in a vacuum and is still high compared with speeds we normally experience. The only substance listed in Table 1.1 that has a greater index of refraction than zircon is diamond. We shall see later that the large index of refraction for zircon makes it sparkle more than glass, but less than diamond.

Check Your Understanding
1.1

Table 1.1 shows that ethanol and fresh water have very similar indices of refraction. By what percentage do the speeds of light in these liquids differ?

The Ray Model of Light

You have already studied some of the wave characteristics of light in the previous chapter on Electromagnetic Waves. In this chapter, we start mainly with the ray characteristics. There are three ways in which light can travel from a source to another location (Figure 1.4). It can come directly from the source through empty space, such as from the Sun to Earth. Or light can travel through various media, such as air and glass, to the observer. Light can also arrive after being reflected, such as by a mirror. In all of these cases, we can model the path of light as a straight line called a ray.


The figure has drawings illustrating the three methods for light to travel from a source to another location. Figure a shows light from the sun reaching the earth’s atmosphere, traveling in a straight line through space. Figure b shown light traveling through a window to reach an observer. Figure c shows light traveling from an object to a mirror and reflecting toward the observer.

Figure
1.4


Three methods for light to travel from a source to another location. (a) Light reaches the upper atmosphere of Earth, traveling through empty space directly from the source. (b) Light can reach a person by traveling through media like air and glass. (c) Light can also reflect from an object like a mirror. In the situations shown here, light interacts with objects large enough that it travels in straight lines, like a ray.

Experiments show that when light interacts with an object several times larger than its wavelength, it travels in straight lines and acts like a ray. Its wave characteristics are not pronounced in such situations. Since the wavelength of visible light is less than a micron (a thousandth of a millimeter), it acts like a ray in the many common situations in which it encounters objects larger than a micron. For example, when visible light encounters anything large enough that we can observe it with unaided eyes, such as a coin, it acts like a ray, with generally negligible wave characteristics.

In all of these cases, we can model the path of light as straight lines. Light may change direction when it encounters objects (such as a mirror) or in passing from one material to another (such as in passing from air to glass), but it then continues in a straight line or as a ray. The word “ray” comes from mathematics and here means a straight line that originates at some point. It is acceptable to visualize light rays as laser rays. The ray model of light describes the path of light as straight lines.

Since light moves in straight lines, changing directions when it interacts with materials, its path is described by geometry and simple trigonometry. This part of optics, where the ray aspect of light dominates, is therefore called geometric optics. Two laws govern how light changes direction when it interacts with matter. These are the law of reflection, for situations in which light bounces off matter, and the law of refraction, for situations in which light passes through matter. We will examine more about each of these laws in upcoming sections of this chapter.

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