1. Blackbody Radiation PHY361, 2008-01-14
review: overview of Classical Statistical Mechanics
kinetic theory: HEAT is random kinetic energy (thermal motion) of atoms
IDEAL GAS law: PV = N kT
EQUIPARTITION theorem: 1/2 kT energy per DoF (degree of freedom)
k = heat capacity: amount of heat energy needed to raise the temperature
eg. Maxwell-Boltzman distribution of molecular velocity in a gas
density of states: g(E) # of states (momentum vectors, etc)
distribution function: f(E) # of particles in each state fB = exp(-E/kT)
blackbody radiation: ‘catastrophic failure of classical stat. mech.’
what is blackbody radiation?
Stefan-Boltzman law: R =  T4
Wien’s displacement law: mT = 2.898£10-3 m¢K
Rayleigh-Jeans equation: u() = 8kT  UV Catastrophe
Planck’s law: u() = 8 hc -5 / (exp(hc/ kT) -1) Planck’s constant ‘h’

4. IR heat lamp
‘red hot’
silver heat shield

6. Stefan-Boltzman law: R =  T4
Wien’s displacement law: mT = 2.898£10-3 m¢K
Rayleigh-Jeans equation: u() = 8kT  UV Catastrophe
Planck’s law: u() = 8 hc -5 / (exp(hc/ kT) -1)