Electromagnetic Radiation (Light)

At least 95% of the celestial information we receive is in the form of light. Because of this fact, astronomers have devised many techniques to decode as much as possible the messages that are encoded in the often extremely faint rays of light. These messages include information about the object's temperature, motion, chemical composition, gas density, surface gravity, shape, structure, and more! Roughly 85% of the information in light is uncovered by using spectroscopy---spreading the light out into its different constituent colors or wavelengths and analyzing the spectrum. The first part of this chapter covers the characteristics of all forms of light and the following sections cover spectroscopic analysis. The vocabulary terms are in boldface.

Electric and Magnetic Fields

Scientists have known since the early part of the 19th century that electrical fields and magnetic fields are intimately related to each other and applications of this connection are found all around you. Moving electric charge (electric current) creates a magnetic field. Coils of wire can be used to make the large electromagnets used in car junk yards or the tiny electromagnetics in your telephone receiver. Electric motors used to start your car or spin a computer's harddisk around are other applications of this phenomenon. In fact, ordinary magnets are produced from tiny currents at the atomic level.

A changing magnetic field creates electrical current---an electric field. This concept is used by power generators---large coils of wire are made to turn in a magnetic field (by falling water, wind, or by steam from the heating of water by burning coal or oil or the heat from nuclear reactions). The coils of wire experience a changing magnetic field and electricity is produced. Computer disks and audio and video tapes encode information in magnetic patterns of alternating magnetic directions and magnetic strengths. When the magnetic disk or tape material passes by small coils of wire, electrical currents (electric fields) are produced.

James Clerk Maxwell (lived 1831-1879) put these ideas together and proposed that if a changing magnetic field can make an electric field, then a changing electric field (from an oscillating electric charge, for example) should make a magnetic field. A consequence of this is that changing electric and magnetic fields should trigger each other and these changing fields should move at a speed equal to the speed of light. To conclude this line of reasoning, Maxwell said that light is an electromagnetic wave. Later experiments confirmed Maxwells's theory.

Electric and magnetic fields oscillate together but perpendicular to each other and the electromagnetic wave moves in a direction perpendicular to both of the fields.

Properties

We feel infrared light as heat and our radios pick up the messages encoded in radio waves emitted by radio stations. Ultraviolet light has high enough energy to damage our skin cells, so our bodies will produce a darker pigment in our skin to prevent exposure of the deeper skin cells to the UV (we tan as a defense mechanism). The special bulbs called "black lights" produce a lot of UV and were used by hospitals to kill bacteria, amoebas, and other micro-organisms. X-rays are produced by very hot things in space. X-rays have more energy than UV, so they can pass through skin, muscles, and organs. They are blocked by bones, so when the doctor takes your X-ray, the picture that results is the shadow image of the X-rays that passed through your body. Because X-rays have such high energy, they can damage or kill cells. A few brief exposures to low-intensity X-rays is okay. The X-ray technician would be exposed to thousands of X-ray exposures if s/he did not use some sort of shielding. Gamma rays are the most energetic form of electromagnetic radiation and are produced in nuclear reactions.

The form of electromagnetic radiation your eyes can detect is called "visible" or "optical". Astronomers have only recently (within the past few decades) been able to use the other forms of electromagnetic radiation or light. Every time technology has been developed to detect another form of light, a revolution in our understanding of the universe has occurred. The figure above shows all of the forms of electromagnetic radiation in order of INcreasing wavelength (given in nanometers (nm)) and DEcreasing energy. Notice how tiny the visible band is!

There are some general properties shared by all forms of electromagnetic radiation:

1. It can travel through empty space. Other types of waves need some sort of medium to move through: water waves need liquid water and sound waves need some gas, liquid, or solid material to be heard.

2. The speed of light is constant in space. All forms of light have the same speed of 299,800 kilometers/second in space (often abbreviated as c). From highest energy to lowest energy the forms of light are Gamma rays, X-rays, Ultraviolet, Visible, Infrared, Radio. (Microwaves are high-energy radio waves.)

3. A wavelength of light is defined similarly to that of water waves---distance between crests or between troughs. Visible light (what your eye detects) has wavelengths 4000-8000 Ångstroms. 1 Ångstrom = 10^-10 meter. Visible light is sometimes also measured in nanometers ("nm" in the figure above): 1 nanometer = 10^-9 meter = 10 Ångstroms, so in nanometers, the visible band is from 400 to 800 nanometers. Radio wavelengths are often measured in centimeters: 1 centimeter = 10^-2 meter = 0.01 meter. The abbreviation used for wavelength is the greek letter lambda: .

White light is made of different colors (wavelengths). When white light is passed through a prism or diffraction grating, it is spread out into all of its different colors. You see this happen every time you see a rainbow. Not all wavelengths of light from space make it to the surface. Only long-wave UV, Visible, parts of the IR and radio bands make it to surface. More IR reaches elevations above 9,000 feet (2765 meters) elevation. That is one reason why modern observatories are built on top of very high mountains. Fortunately, as far as life is concerned, our atmosphere shields us from the gamma rays, X-rays, and most of the UV. It also blocks most of the IR and parts of the radio. Astronomers were not able to detect these forms of energy from celestial objects until the space age, when they could put satellite observatories in orbit.

Besides using wavelength to describe the form of light, you can also use the frequency--the number of crests of the wave that pass by a point every second. Frequency is measured in units of hertz (Hz): 1 hertz = 1 wave crest/second. For light there is a simple relation between the speed of light (c), wavelength (), and frequency (f):

f = c/.

Some colors and their approximate wavelength, frequency and energy ranges are given in the table below. The unit of energy is the Joule (J). A Joule is how much energy you expend when you lift an object with 1 kilogram of mass (for example, a liter of water) about 1 meter above the ground. If you then let it go, the object hits the ground with that much energy. Sometimes light energy is also measured in "ergs", where 1 erg = 10^-7 Joule.

color	(Å)	f (*1014 Hz)	Energy (*10-19 J)
violet	4000 4600	7.5 6.5	5.0 4.3
indigo	4600 4750	6.5 6.3	4.3 4.2
blue	4750 4900	6.3 6.1	4.2 4.1
green	4900 5650	6.1 5.3	4.1 3.5
yellow	5650 5750	5.3 5.2	3.5 3.45
orange	5750 6000	5.2 5.0	3.45 3.3
red	6000 8000	5.0 3.7	3.3 2.5

Note the trends: bluer light has shorter , higher f, and more energy. Redder light has longer , lower f, and less energy.

At the beginning of the 20th century Max Planck (lived 1858--1947) discovered that if you consider light as packets of energy called photons, you can accurately explain the shape of continuous spectra. A photon is a particle of electromagnetic radiation. Bizarre though it may be, light is both a particle and a wave. Whether light behaves like a wave or like a particle depends on how the light is observed (it depends on the experimental setup)! A few years after Planck's discovery Albert Einstein (lived 1879--1955) found a very simple relationship between the energy of a light wave (photon) and its frequency:

Energy of light	=	h · f
Energy of light	=	(h · c)/,

Light can also behave as a particle and a wave at the same time. An example of light acting as both a particle and a wave is the digital camera---the lens refracts (bends and focusses) waves of light that hit a charge-coupled device (CCD). The photons kick electrons out of the silicon in the CCD. The electrons are detected by electronics that interpret the number of electrons released and their position of release from the silicon to create an image. Another example is when you observe the build-up of the alternating light and dark pattern from diffraction (a wave phenomenon) from light passing through a narrow slit. You see one bright spot (a photon), then another bright spot (another photon), then another... until the diffraction pattern is created from all of the accumulated photons. This happens so quickly that it is undetectable to the human eye.

To decode the information stored in light, you pass the light through a prism or diffraction grating to create a spectrum---any display of the intensity of light (EM radiation) at different wavelengths or frequencies (a picture or a graph of intensity vs. either wavelength or frequency). If white light is examined, then the spectrum will be a rainbow.

The term intensity has a particular meaning here: it is the number of waves or photons of light reaching your detector; a brighter object is more intense but not necessarily more energetic. Remember that a photon's energy depends on the wavelength (or frequency) only, not the intensity. The photons in a dim beam of X-ray light are much more energetic than the photons in an intense beam of infrared light.

The type of light produced by an object will depend on its temperature, so let's digress slightly to investigate what "temperature" is. Temperature is a measure of the random motion (or energy) of a group of particles. Higher temperature (T) means more random motion (or energy). A natural scale would have zero motion at zero degrees (absolute zero). This scale is the Kelvin scale. It scales exactly like the Celsius system, but it is offset by 273 degrees. Here is a comparison of the Kelvin, Celsius, and Fahrenheit temperature scales:

Formulae

1. Frequency and wavelength relation: f = c/.
2. Energy of a photon: E = h·f, where h is a constant of nature.
3. Energy of a photon: E = (h·c)/.

Review Questions

1. Why is light so very important to astronomy? What kinds of information can you get from it?
2. Why is light called electromagnetic radiation? Is radio a form of light?
3. Put the following forms of light in order of increasing frequency (lowest frequency first): ultraviolet, infrared, gamma rays, visible, radio, X-rays. Put them in order of increasing wavelength (shortest wavelength first). Put them in order of increasing energy (lowest energy first).
4. Do all forms of light travel at the same speed in a vacuum (empty space)? Why is it important that light can travel through empty space?
5. What forms of light can be observed from the ground (including high mountains)? What forms can be observed at high altitudes in our atmosphere? What forms must be observed in space?
6. Is electromagnetic radiation a wave or a particle? What determines if you will see light as a wave or a photon?
7. Which of these are a spectrum: plot of intensity vs. wavelength, plot of intensity vs. brightness, plot of frequency vs. wavelength, rainbow, plot of acceleration vs. time, plot of energy vs. frequency.
8. What is the difference between intensity and energy? If a particular CCD chip requires light energies of 4.2 · 10^-19 J to release electrons from the silicon, which will produce more electrons (and hence, a brighter computer image): an intense beam of yellow light or a dim beam of UV light? Explain your answer!
9. Why is the Kelvin scale preferred over the Celsius or the Fahrenheit scales?
10. Where is absolute zero on the three temperature scales? Where is the Sun's temperature on the three temperature scales?

Production of light

Tutorial index page

Is this page a copy of Strobel's Astronomy Notes?