In Einstein's rate picture , the Einstein coefficients B 12 , B 21 and A 21 are used to calculate the spontaneous and stimulated (induced) emission and absorption. In addition to statistical physics u. a. used in spectroscopy and laser physics and was introduced by Albert Einstein in 1916 .
Einstein distinguishes three processes in the radiation equilibrium:
- by absorbing a photon from an electromagnetic field , an excited state occurs e.g. B. an atom .
- an n -fold occupied mode of an electromagnetic field stimulates the emission of a further photon in this mode, whereby the atom changes from the excited to the ground state. Same mode means same direction, frequency and phase .
- The atom spontaneously - without external influence - emits a photon in an unoccupied mode (in free space this means in particular: in any direction).
In the following we refer to the ground state as state 1 and the excited state as state 2. The probability of the three processes obviously depends on the number of atoms in the outgoing state. In addition, the stimulated processes depend on the occupation of the modes of the electromagnetic field ( spectral radiance ). Einstein introduced the coefficients B 12 , B 21 and A 21 as initially indeterminate proportionality constants , so that
- the likelihood of absorption through
- the probability of stimulated emission by and
- the probability of spontaneous emission through
The increase in the number of particles in the ground state and the decrease in the number of particles in the excited state is then given by:
In thermodynamic equilibrium this sum is zero:
Equating and resolving the spectral radiance yields:
By comparing coefficients with Planck's law of radiation or Rayleigh-Jeans law - in the latter case using the boundary conditions and a series expansion of the exponential function - the following relationships are obtained between the three Einstein coefficients:
If the states are not degenerate, then so is .
The Einstein coefficients depend not on the temperature from. The temperature dependence of the energy distribution of the thermal radiation is instead a consequence of the temperature dependence of the occupation probabilities N 1 and N 2 , which is usually described by the Boltzmann distribution .
- A. Einstein : On the quantum theory of radiation . Physikalische Zeitschrift 18 (1917) 121-128; First printed in the communications of the Physikalische Gesellschaft Zürich 18 (1916)
- Detailed derivation: H. Haken / HC Wolf: Atom- und Quantenphysik , 8th edition, Springer-Verlag, Berlin Heidelberg New York, 2004, ISBN 3540026215 , p. 59, limited preview in the Google book search
- Walter J. Moore, Dieter O. Hummel: Physical chemistry. 4th edition, Walter de Gruyter, Berlin New York, 1986, ISBN 3-11-010979-4 , pp. 893-896