Difference between revisions of "Einstein Coefficients"

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\section*{ Einstein Coefficients}
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\title{ Einstein Coefficients}
  
\subsection*{ Einstein Coefficients}
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Einstein coefficients describe the absorption and emission of photons via electronic transitions in atoms.  There are three coefficients:
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\begin{figure}\centering
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\includegraphics[width=2in]{b12.png}
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\includegraphics[width=2in]{a21.png}
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\includegraphics[width=2in]{b21.png}
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\caption{Left: Photon absorption is described by $B_{12}$.  Center: Spontaneous photon emission is described by $A_{21}$.  Right: Stimulated photon emission is described by $B_{21}$.}
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Derivation identical to Rybicki's.  We should memorize these.\par
 
Derivation identical to Rybicki's.  We should memorize these.\par

Revision as of 11:53, 18 September 2014

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Einstein Coefficients

Einstein coefficients describe the absorption and emission of photons via electronic transitions in atoms. There are three coefficients:

B12.png A21.png B21.png
Left: Photon absorption is described by . Center: Spontaneous photon emission is described by . Right: Stimulated photon emission is described by .

Derivation identical to Rybicki’s. We should memorize these.

These coefficients govern the interaction of radiation with discrete energy levels. Say we have 2 energy levels with a difference . There is some uncertainty associated with , but we’ll say it’s small for now.

There are 3 coefficients:

  • governs decay from 2 to 1, and is the transition probability per unit time. The probability of spontaneous de-excitation and release of photon is Poisson-distributed with mean rate . So is the mean lifetime of the excited state. e.g. For (n=3 to n=2): .
  • governs absorptions causing transitions . The transition probability per unit time is , where is the probability constant, and is:

It depends on (the intensity), but it does not depend on direction, so we integrate over all angles. The is a normalization constant which makes the mean intensity, instead of the total intensity. However, we have to remember that there are uncertainties in the energy-level separations. is called the line profile function. It describes some (maybe gaussian) distribution of absorption around (the absorption frequency), and is subject to the requirement that:

Say that is the width of the distribution around . is affected by many factors: (the natural, uncertainty-based broadening of at atom in isolation), (the thermal, Doppler-based broadening), and (collisional broadening, a.k.a. pressure broadening). So really, the transition probability per unit time is:

  • governs stimulated emission. In this example, we are in energy state 2, and an incoming photon causes a transition to energy level 1 and the emission of 2 photons. The transition per unit time is .

Einstein Relations among coefficients

Assume we have many atoms with 2 energy states, and is the # density in state 1, ditto for . Assume we are in thermal, steady-state equilibrium, so:

This is because as many atoms need to be going from energy state 1 to 2 as visa versa. A second relation is: . Using that :

In thermal equilibrium :

Combining this with earlier, we get:

and

Rewriting in terms of Einstein coeffs

In a small volume :

We can express in terms of the Einstein coefficients. The excitation probability per time is , and the energy lost in crossing the small volume (it is the probability per time per volume of going by absorbing from a cone of solid angle and frequency range ). Thus, the energy is given by:

Recognizing that :

Correcting for stimulated emission, we get:

Estimating Cross-Sections

The absorption coefficient, written in terms of Einstein constants is:

Thus, the cross-section of an atom for absorption of a photon is:

To estimate , we use the fact that, ignoring g’s, , and . Then using the approximation that that , we get:

In a single atom, , so .