qThe single factor that
determine how much energy is emitted
by a blackbody is its temperature.
qThe intensity of energy
radiated by a blackbody increases
according to the fourth power of its absolute temperature.
qThis relationship is
called the Stefan-Boltzmann Law.
E =
radiation emitted in W/m2
s= 5.67 x 10-8 W/m2 * K *sec
T = temperate
(K ß Kelvin degree)