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Consider any two internal states, s1 and s2, of an atom. Let s2 be the higher-energy state, so that Es2-Es1=ϵ for some positive constant. If the atom is currently in state s2, then there is a certain probability per unit time for it to spontaneously decay down to state s1, emitting a photon with energy e. This probability per unit time is called the Einstein A coefficient:

A = probability of spontaneous decay per unit time.

On the other hand, if the atom is currently in state s1 and we shine light on it with frequency f=ϵ/h, then there is a chance that it will absorb photon, jumping into state s2. The probability for this to occur is proportional not only to the amount of time elapsed but also to the intensity of the light, or more precisely, the energy density of the light per unit frequency, u(f). (This is the function which, when integrated over any frequency interval, gives the energy per unit volume within that frequency interval. For our atomic transition, all that matters is the value of u(f)atf=ϵ/h) The probability of absorbing a photon, per unit time per unit intensity, is called the Einstein B coefficient:

B=probability of absorption per unit timeu(f)

Finally, it is also possible for the atom to make a stimulated transition from s2down to s1, again with a probability that is proportional to the intensity of light at frequency f. (Stimulated emission is the fundamental mechanism of the laser: Light Amplification by Stimulated Emission of Radiation.) Thus we define a third coefficient, B, that is analogous to B:

B'=probability of stimulated emission per unit timeu(f)

As Einstein showed in 1917, knowing any one of these three coefficients is as good as knowing them all.

(a) Imagine a collection of many of these atoms, such that N1 of them are in state s1 and N2 are in state s2. Write down a formula for dN1/dt in terms of A, B, B', N1, N2, and u(f).

(b) Einstein's trick is to imagine that these atoms are bathed in thermal radiation, so that u(f) is the Planck spectral function. At equilibrium, N1and N2 should be constant in time, with their ratio given by a simple Boltzmann factor. Show, then, that the coefficients must be related by

B'=BandAB=8Ï€hf3c3

Short Answer

Expert verified

Therefore, the formula isdN1dt=AN2+N2B'u(f)-N1Bu(f)

Step by step solution

01

Given information

Consider any two internal states, s1 and s2, of an atom. Let s2 be the higher-energy state, so that Es2-Es1=ϵfor some positive constant. If the atom is currently in state s2, then there is a certain probability per unit time for it to spontaneously decay down to state s1, emitting a photon with energy e. This probability per unit time is called the Einstein A coefficient:

02

Explanation

(a) Consider N1 and N2 atoms in state s1 and s2, respectively. The probability of atoms decaying to state s1 equals the coefficient A, and the rate of atoms per unit time equals the number of atoms in this state N2 multiplied by the constant A, resulting in:

AN2

Second, when we shine a light with energy e, there is a chance that the atoms in state s1 will absorb the photons and jump to state s2. The probability of this action occurring equals the constant B multiplied by the energy density of the beam u(f), so the rate per unit time of the atoms jumping to the second state equals the negative sign of the probability multiplied by the number of the first state, that is:

-N1Bu(f)

Finally, we have stimulated emission from state s2 to state s1, which has a probability of the constant B' multiplied by the energy density of the beam u(f), so the rate per unit time of atoms jumped to the second state equals the probability multiplied by the number of atoms in the first state, i.e.

N2B'u(f)

The total rate dN1/dtequals to the sum of these rates:

role="math" localid="1647754521419" dN1dt=AN2+N2B'u(f)-N1Bu(f)(1)

03

Explanation

(b) Because the number of atoms N1 and N2 in the equilibrium is independent of time, therefore

dN1dt=0AN2+N2B'u(f)-N1Bu(f)=0AN2+N2B'-N1Bu(f)=0(2)

the ratio of the number of atoms can be written in terms of Boltzmann factor, as:

N2N1=e-Es2/kTe-Es1/kTN2N1=e-Es2-Es1/kT

But the energy difference between the levels is ϵ=hf, therefore

N2N1=e-hf/kT(3)

Equation 7.83 is :

UV=8π(hc)3∫0∞ϵ3eϵ/kT-1dϵ

Let ϵ=hf→dϵ=hdf, then

UV=8π(hc)3∫0∞(hf)3ehf/kT-1hdfUV=8πhc3∫0∞f3ehf/kT-1dfu(f)=8πhc3f3ehf/kT-1

Substitute this into (2)

AN2+N2B'-N1B8Ï€hc3f3ehf/kT-1=0

Divide both sides by N1and substitute from (3)

Ae-hf/kT+B'e-hf/kT-B8Ï€hc3f3ehf/kT-1=0

Multiply both sides by ehf/kT

A+B'-Behf/kT8Ï€hc3f3ehf/kT-1=0A=Behf/kT-B'8Ï€hc3f3ehf/kT-1

The constant A is temperature independent, as are the constants B and B'. This indicates that the RHS must be temperature independent, thus the temperature portion must cancel out. This only happens when B = B', so we get:

A=Behf/kT-18Ï€hc3f3ehf/kT-1A=B8Ï€hf3c3

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Most popular questions from this chapter

The sun is the only star whose size we can easily measure directly; astronomers therefore estimate the sizes of other stars using Stefan's law.

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