Stefan-Boltzmann Law
					E = radiation emitted in W/m2 s = 5.67 x 10-8 W/m2 * K *sec T = temperate (K ß Kevin degree)
			E = sT4
	q The single factor that determine how much energy is emitted by a blackbody is its temperature. q The intensity of energy radiated by a blackbody increases according to the fourth power of its absolute temperature. q This relationship is called the Stefan-Boltzmann Law.