An Introduction to Solar System Astronomy
Prof. Richard Pogge, MTWThF 2:30
Lecture 22: Light the Messenger
- Light is Electromagnetic Radiation
- Light as Waves or Photons
- Light carries energy at the speed of light
- Waves, or
- Particles (Photons)
- The Electromagnetic Spectrum
- Sequence of photon energies
- Luminosity vs. Apparent Brightness
- Inverse Square Law of Brightness
- Doppler Effect
- Due to relative motion between source & observer
- Way to measure speeds at a distance
Light is Electromagnetic Radiation, a self-propagating
Electromagnetic disturbance that carries energy at the speed of light
Two complementary ways to describe light
- Electromagnetic Waves
- Photons (particles of light)
Wave Nature of Light
Light can be described as Electromagnetic Waves
The speed of light (c) is the same for all light waves:
- Periodic (repeating) changes in the strengths of coupled electric and
- Electromagnetic waves travel through a vacuum at the speed of light.
- Doesn't need a medium to "wave" in.
- c = 299,792.458 km/sec
This speed is independent of the wavelength or frequency of the
Particle Nature of Light
We can also describe light as a stream of particles or Photons.
- Massless particles that carry energy at the speed of light.
Photons are characterized by their Energy, which is
proportional to their Frequency, f.
where: f = frequency of the light, and h = Planck's
- E = hf
- Higher Frequencies mean Higher Energies
Note: Energy, E, is a "particle property", whereas frequency, f,
is a "wave property". They are related through Planck's Constant, h.
Planck's constant is one of the "Fundamental Constants" of Nature
(another one we've met in this lecture is the speed of light, c). One
can think of Planck's constant as serving as the "link" between the wave
and particle natures of light, and indeed h is the fundamental constant
in "quantum mechanics", the modern view of matter and radiation as
entities ("quanta") that have the properties of both waves and
The Electromagnetic Spectrum
The sequence of photon energies running from low energy to high
energy is called the Electromagnetic Spectrum
- low energy = low frequency = long wavelength
- Examples of low-energy photons: Radio Waves, Infrared
- high energy = high frequency = short wavelength
- Examples of high-energy photons: Ultraviolet, X-rays, Gamma Rays
Major Divisions of the Electromagnetic Spectrum
|Type of Radiation
|700-105 nm (0.1 mm)
The Visible Spectrum
This is all forms of light we can see with our eyes.
- Wavelengths: 400 - 700 nanometers (nm)
- Frequencies: 7.5x1014 - 4.3x1014 waves/second
We sense visible light of different energies as different colors.
The basic colors of the visible spectrum are defined roughly as follows,
in order of increasing photon energy:
You can remember the order of these colors from lowest to highest
energy using the famous mnemonic: ROY G. BIV
[22.2 - note about colors and wavelengths]
How "Bright" is a Light Source?
We need to quantify how bright a light source is. The most convenient
way is using the photon picture for light:
There are two ways to quantify this:
- "Brightness" measures the number of photons per second emitted by the
- Luminosity (L):
- Measure of the total energy output:
- L is measured in Power Units (energy/sec) like Watts
- L is independent of distance
- Luminosity is an intrinsic property of the light source.
- Apparent Brightness (B):
- Measures how bright an object appears to be as seen from
- B is measured in Flux Units (energy/sec/area)
- B depends on the distance to the source
- Brightness is what we actually measure (an observable property).
As light travels away from its source, the photons get spread
out over increasingly greater areas. The more the light is spread
out, the fainter it appears in any given patch of area (for
example, the small patch of area covered by the opening in your
This means that the Apparent Brightness, B of a light source
with intrinsic Luminosity L will get fainter as the
square of our distance from the source:
- Apparent Brightness is inversely proportional to the
square of the distance to the source
This law is extremely important to us in astronomy.
- If the source is 2x closer, it appears 4x brighter.
- If the source is 2x farther away, it appears 4x fainter.
The observed wavelength of a wave will change when the source of the
waves and the observer are moving either towards or away from each other.
The amount of the shift and its sign depends on
- Sound Waves (Siren or Train Horn)
- Light Waves
- relative speed of the source & observer
- direction of motion (together or apart)
Doppler Effect in Sound
Two cats are sitting between a windup mouse toy that emits an electronic
squeak. The mouse is moving towards the left towards the first cat and
away from the second:
The mouse emitted a squeak when it was at the location of each of the
green dots. The sound wave ("squeak!") moves outward spherically from
each point of emission. Because the mouse is moving, the sound waves
have different emission centers. Those waves ahead of its motion
(towards the left) are are scrunched together, while those behind are
- The cat on the left hears a higher-pitched squeak because the waves
have a shorter wavelength (scrunched together by the mouse's motion).
- The cat on the right hears a lower-pitched squeak because the waves
have a longer wavelength (spread out by the mouse's motion).
Doppler Effect in Light
The Doppler Effect in light works the same way as it does for sound:
- Light source moving away from the observer, the
observed wavelength will get longer, and hence
- Light source moving towards the observer, the observed
wavelength will get shorter, and hence BLUESHIFTED
A Way to Measure Speeds
Observe the wavelength
lobs of a
light source with a known emitted wavelength
The difference between the observed and emitted wavelengths is
directly proportional to the speed of the source towards or away from
you (v), given by the Doppler Formula:
Here c is the speed of light.
- The size of the shift gives the speed of the source
- The color of the shift (Red or Blue) gives the direction of motion
(away or towards you).
The Doppler Effect in Practice
The Doppler Effect in light is used by astronomers to measure the speeds
of objects moving towards or away from the Earth.
But, we also use the Doppler Effect in light in everyday settings. Some
- Traffic Radar Guns:
- Radar gun bounces a pulse of microwaves (or infrared laser light)
of a known wavelength off a car or truck, measure the wavelength
reflected back. The Doppler shift gives the vehicle's speed.
- Doppler Weather Radar:
- Similar principle, bounce microwave radar signals of known
wavelength off of clouds, measure the wavelength reflected back. The
Doppler shift and its sign (blue or red) gives the speed and direction
of the clouds. The strength of the returned signal also gives the
amount of rain or snow falling.
Light the Messenger
The properties of light give us a way to bridge the vast distances
between us and astronomical objects.
The light "encodes" important information about the source of the light
To learn more from light, however, we need to understand how light and
matter interact, which is the subject of next few lectures.
- Luminosity measures how much energy the object emits in the
form of light.
- Doppler Shift tells us how fast it is moving towards or away from us
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Updated: 2007 October 19
Copyright © Richard W. Pogge,
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