THE STEFANBOLTZMANN LAW
Electromagnetic radiation absorbed and emitted by any substance is dependent on the temperature of the substance. Josef Stefan showed experimentally in 1879 that for a perfect emitter (a 'black body') the rate at which energy is emitted is related to the object's temperature by
, [1]
where e equals 1 for a perfect blackbody, A is the surface area of the radiator, and s is known as the StefanBoltzmann constant. This relation was subsequently derived theoretically by Ludwig Boltzmann, who had been a student assistant of Stefan's at the University of Vienna, and later succeeded to Stefan's professorial post there. In 1900 Max Planck showed that the spectral distribution of energy density in a blackbody could be described with what we call the Planck radiation formula:
[2]
This expression required the use of the quantum hypothesis and marked the first appearance of the quantum of energy, hf. If we integrate over the range of frequencies from 0 to ¥ we should get the total energy density (per volume), U, which is related to the emissivity,E=P/A, by E=cU/4.
LIBRARY RESEARCH:
Find out more about the following: blackbodies, StefanBoltzmann's (T^{4}) law, Wien's law.
THEORY:
Integrate the expression in Eq. 2, and multiply by c/4 to get the StefanBoltzmann law (Eq. 1), for an emissivity of 1. Verify that the constants multiplying your factor of T^{4} equal the accepted value of the StefanBoltzmann constant, σ. (Hint: use the dimensionless quantity x=hf/kT to simplify the integral. Look up the value of the resulting definite integral in x. (HINT: do not try to solve it analytically.))
EXPERIMENT:
You will use a radiation sensor to measure the intensity of thermal radiation. The sensing element, a miniature thermopile, produces a voltage proportional to the intensity of the radiation. (Look on the sensor to find out the conversion between its reading and power radiation.) When using the sensor, be careful not to change its position. Instead of opening and closing the aperture for every measurement, leave the aperture open and place a piece of insulating foam between the source and the sensor. Make measurements quickly so that the sensor does not heat up when exposed to the source.
You will be measuring the radiation emitted by two sources. The 'high temperature' source is a tungstenfilament lamp. The temperature of the filament can be calibrated to the resistance of the filament using an optical pyrometer. The 'low temperature' source is a thermal radiation cube a "Leslie cube"). This is a cube of nearly uniform external temperature, heated from inside by a light bulb. The sides of the cube are black, white, shiny metallic, and dull metallic ("gray").
A. STEFANBOLTZMANN LAW AT HIGH TEMPERATURES.
Set up the circuit as shown. In order to determine the resistance of the filament and the power dissipated at various temperatures, you will record V and I at different voltage levels.
Before you do that, though, measure the roomtemperature resistance of the bulb to three digits using a fourwire ohmmeter. (Ask your instructor to show you how.) We will use this quantity, called R_{300K} later in our calculations. Measure this resistance with enough precision that you can see the resistance change as you warm the bulb in your hand. Starting at half the voltage of where the filament first begins to glow, record V and I every 5V up to about 110V.
Record V and I at each voltage level on a spreadsheet. Calculate R, R/R_{300K}, and temperature, using the tungsten resistivity data table below, and P=VI at each voltage. Plot the power you have measured vs T^{4} (Use Kelvin temperature values!!). Do your data support the StefanBoltzmann law?
TUNGSTEN RESISTANCE VS TEMPERATURE
R (Ohm) 
R/R_{300 } 
Temperature (K) 

1.00 1.43 1.87 2.34 2.85 3.36 3.88 4.41 4.95 5.48 6.03 6.58 
300 400 500 600 700 800 900 1000 1100 1200 1300 1400 

R (Ohm) 
R/R_{300 } 
Temperature (K) 

7.14 7.71 8.28 8.86 9.44 10.03 10.63 11.24 11.84 12.46 13.08 13.72 
1500 1600 1700 1800 1900 2000 2100 2200 2300 2400 2500 2600 

R (Ohm) 
R/R_{300 } 
Temperature (K) 

14.34 14.99 15.63 16.29 16.95 17.62 18.28 18.97 19.66 20.35  2700 2800 2900 3000 3100 3200 3300 3400 3500 3600  
B. STEFANBOLTZMANN LAW AT LOW TEMPERATURES.
With the thermal radiation cube set to its highest setting, measure the power emitted by each of its surfaces as a function of temperature for the entire temperature range of the cube. (Be sure to have the sensors the same distance from each surface.)
You will use the internal thermistor temperature sensor of the cube, the resistance of which changes with temperature. The calibration is on the side of the cube. Measure the thermistor's temperature at each temperature!! Do all the surfaces emit with the same power rate? (Why or why not?) Remember that at low temperatures, energy loss to the surroundings is significant. The net energy transfer goes as T^{4}  T_{o}^{4}, where T_{o} is room temperature. (You should be able to explain why that is.) Use Kelvin temperature values!!
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