View source for Interaction of an atom with an electromagnetic field

This section introduces the interaction of atoms with radiative modes of the electromagnetic field.

<categorytree mode=pages style="float:right; clear:right; margin-left:1ex; border:1px solid gray; padding:0.7ex; background-color:white;" hideprefix=auto>8.421</categorytree>
== Introduction: Spontaneous and Stimulated Emission ==

<span id="SEC_ERL"></span> 

Einstein's 1917 paper on the theory of radiation [EIN17a] provided seminal concepts for the quantum theory of radiation. It also anticipated devices such as the laser, and pointed the way to the field of laser-cooling of atoms. In it, he set out to answer two questions: 

1) How do the internal states of an atom that radiates and absorbs energy come into equilibrium with a thermal radiation field? (In answering this question Einstein invented the concept of spontaneous emission) 

2) How do the translational states of an atom in thermal equilibrium (i.e. states obeying the Maxwell-Boltzmann Law for the distribution of velocities) come into thermal equilibrium with a radiation field? (In answering this question, Einstein introduced the concept of photon recoil. He also demonstrated that the field itself must obey the Planck radiation law.) 

The first part of Einstein's paper, which addresses question 1), is well known, but the second part, which addresses question 2), is every bit as germane to contemporary atom/optical physics. Because the paper preceded the creation of quantum mechanics there was no way for him to calculate transition rates. However, his arguments are based on general statistical principles and provide the foundation for interpreting the quantum mechanical results. 

Einstein considered a system of <math>N</math> atoms in thermal equilibrium with a radiation field. The system has two levels (an energy level consists of all of the states that have a given energy; the number of quantum states in a given level is its multiplicity.) with energies <math>E_ b</math> and <math>E_ a</math>, with <math>E_ b > E_ a</math>, and <math>E_ b - E_ a =\hbar \omega </math>. The numbers of atoms in the two levels are related by <math>N_ b + N_ a = N</math>. Einstein assumed the Planck radiation law for the spectral energy density temperature. For radiation in thermal equilibrium at temperature <math>T</math>, the energy per unit volume in wavelength range <math>d\omega </math> is: 

{{EqL
|math=<math>\begin{align} \  \rho _ E (\omega )d\omega = \frac{\hbar \omega ^3}{\pi ^2 c^3} \frac{1}{{\rm exp} (\hbar \omega /kT) -1 }d\omega . \end{align}</math>
|num=erad1
}}

The mean occupation number of a harmonic oscillator at temperature <math>T</math>, which can be interpreted as the mean number of photons in one mode of the radiation field, is 

{{EqL
|math=<math>\begin{align} \  \bar{n} = \frac{1}{{\rm exp} (\hbar \omega /kT) -1}. \end{align}</math>
|num=erad2
}}

According to the Boltzmann Law of statistical mechanics, in thermal equilibrium the populations of the two levels are related by 

{{EqL
|math=<math>\begin{align} \  \frac{N_ b}{N_ a} = \frac{g_ b}{g_ a} e^{-(E_ b -E_ a)/kT} = \frac{g_ b}{g_ a} e^{-\hbar \omega /kT} . \end{align}</math>
|num=erad3
}}

Here <math>g_ b</math> and <math>g_ a</math> are the multiplicities of the two levels. The last step assumes the Bohr frequency condition, <math>\omega = (E_ b -E_ a)\  \hbar </math>. However, Einstein's paper actually derives this relation independently. 

According to classical theory, an oscillator can exchange energy with the radiation field at a rate that is proportional to the spectral density of radiation. The rates for absorption and emission are equal. The population transfer rate equation is thus predicted to be 

{{EqL
|math=<math>\begin{align} \  \dot{N}_ b = - { \rho _ E (\omega ) B_{ba}} N_ b + \rho _ E (\omega ) B_{ab} N_ a = -\dot{N}_ a . \end{align}</math>
|num=erad4
}}

This equation is incompatible with Eq. [[{{SUBPAGENAME}}#erad3|erad3]]. (This can be seen by setting <math>A_{ba}=0 </math> in Eq. [[{{SUBPAGENAME}}#erad5|erad5]] which then leads to <math>B_{ba}=B_{ab}=0</math>.) To overcome this problem, Einstein postulated that atoms in state b must spontaneously radiate to state a, with a constant radiation rate <math>A_{ba}</math>. Today such a process seems quite natural: the language of quantum mechanics is the language of probabilities and there is nothing jarring about asserting that the probability of radiating in a short time interval is proportional to the length of the interval. At that time such a random fundamental process could not be justified on physical principles. Einstein, in his characteristic Olympian style, brushed aside such concerns and merely asserted that the process is analagous to radioactive decay. With this addition, Eq. [[{{SUBPAGENAME}}#erad4|erad4]] becomes 

{{EqL
|math=<math>\begin{align}  \  \dot{N}_ b = - {\left[ \rho _ E (\omega ) B_{ba} + A_{ba} \right]} N_ b + \rho _ E (\omega ) B_{ab} N_ a = -\dot{N}_ a . \end{align}</math>
|num=erad5
}}

By combining Eqs. [[{{SUBPAGENAME}}#eq:plancklaw|eq:plancklaw]], [[{{SUBPAGENAME}}#eq:frac|eq:frac]], [[{{SUBPAGENAME}}#eq:rad2|eq:rad2]]  it follows that 

{{EqL
|math=<math>\begin{align}  \  g_ b B_{ba} & =&  g_ a B_{ab} \\ \frac{\hbar \omega ^3}{\pi ^2 c^3} B_{ba} & =&  A_{ba}  \\  \rho _ E (\omega ) B_{ba} & =&  \bar{n} A_{ba}  \\  \end{align}</math>
|num=EQ_ erl5
}}

Consequently, the rate of transition <math>b\rightarrow a</math> is 

{{EqL
|math=<math>\begin{align} \  B_{ba} \rho _ E (\omega ) + A_{ba} = (\bar{n} +1 )A_{ba}, \end{align}</math>
|num=EQ_ erl6
}}

while the rate of absorption is 

{{EqL
|math=<math>\begin{align} \  B_{ab} \rho _ E (\omega ) = \frac{g_ b}{g_ a} \bar{n} A_{ba} \end{align}</math>
|num=EQ_ erl7
}}

If we consider emission and absorption between single states by taking <math>g_ b = g_ a = 1</math>, then the ratio of rate of emission to rate of absorption is <math>(\bar{n} + 1) /\bar{n}</math>. 

This argument reveals the fundamental role of spontaneous emission. Without it, atomic systems could not achieve thermal equilibrium with a radiation field. Thermal equilibrium requires some form of dissipation, and dissipation is equivalent to having an irreversible process. Spontaneous emission is the fundamental irreversible process in nature. The reason that it is irreversible is that once a photon is radiated into the vacuum, the probability that it will ever be reabsorbed is zero: there are an infinity of vacuum modes available for emission but only one mode for absorption. If the vacuum modes are limited, for instance by cavity effects, the number of modes becomes finite and equilibrium is never truly achieved. In the limit of only a single mode, the motion becomes reversible. 

The identification of the Einstein <math>A</math> coefficient with the rate of spontaneous emission is so well established that we shall henceforth use the symbol <math>A_{ba}</math> to denote the spontaneous decay rate from state <math>b</math> to <math>a</math>. The radiative lifetime for such a transition is <math>\tau _{ba} = A_{ba}^{-1}</math>. 

Here, Einstein came to a halt. Lacking quantum theory, there was no way to calculate <math>A_{ba}</math>. 

<br style="clear: both" />

== Quantum Theory of Absorption and Emission ==

<span id="SEC_IAEF"></span> 

We shall start by describing the behavior of an atom in a classical electromagnetic field. Although treating the field classically while treating the atom quantum mechanically is fundamentally inconsistent, it provides a natural and intuitive approach to the problem. Furthermore, it is completely justified in cases where the radiation fields are large, in the sense that there are many photons in each mode, as for instance, in the case of microwave or laser spectroscopy. There is, however, one important process that this approach cannot deal with satisfactorily. This is spontaneous emission, which we shall treat later using a quantized field. Nevertheless, phenomenological properties such as selection rules, radiation rates and cross sections, can be developed naturally with this approach. 

<br style="clear: both" />
=== The classical E-M field ===

<span id="SEC_wd"></span> 

Our starting point is Maxwell's equations (S.I. units): 

{{EqL
|math=<math>\begin{align}  \  \nabla \cdot {\bf E} &  = &  \rho /\epsilon _0 \\  \nabla \cdot {\bf B} &  = &  0 \\  \nabla \times {\bf E} &  = &  - \frac{\partial {\bf B}}{\partial t} \\  \nabla \times {\bf B} &  = &  \frac{1}{c^2} \frac{\partial \bf { E}}{\partial t} + \mu _0 \bf {J} \end{align}</math>
|num=eq:Maxwell
}}

The charge density <math>\rho </math> and current density '''J''' obey the continuity equation 

{{EqL
|math=<math>\begin{align} \  \nabla \cdot {\bf J} + \frac{\partial \rho }{\partial t} = 0 \end{align}</math>
|num=EQ_ wd2
}}

Introducing the vector potential '''A''' and the scalar potential <math>\psi </math>, we have 

{{EqL
|math=<math>\begin{align} \  {\bf E} &  = &  - \nabla \psi - \frac{\partial {\bf A}}{\partial t} \\ {\bf B} &  = &  \nabla \times {\bf A}  \end{align}</math>
|num=EQ_ wd3
}}

We are free to change the potentials by a gauge transformation: 

{{EqL
|math=<math>\begin{align} \  {\bf A}^\prime = {\bf A} + \nabla \Lambda , ~ ~ ~ ~ ~ \psi ^\prime = \psi - \frac{\partial \Lambda }{\partial t} \end{align}</math>
|num=EQ_ wd4
}}

where <math>\Lambda </math> is a scalar function. This transformation leaves the fields invariant, but changes the form of the dynamical equation. We shall work in the <i>
Coulomb gauge
</i> (often called the radiation gauge), defined by 

{{EqL
|math=<math>\begin{align} \  \nabla \cdot {\bf A} = 0 \end{align}</math>
|num=EQ_ wd5
}}

In free space, '''A''' obeys the wave equation 

{{EqL
|math=<math>\begin{align} \  \nabla ^2 {\bf A} = \frac{1}{c^2} \frac{\partial ^2 {\bf A}}{\partial t^2} \end{align}</math>
|num=EQ_ wd6
}}

Because <math>\nabla \cdot {\bf A}= 0</math>, '''A''' is transverse. We take a propagating plane wave solution of the form 

{{EqL
|math=<math>\begin{align} \  {\bf A}(r, t) = A{\bf \hat{e}} \cos ({\bf k}\cdot {\bf r} -\omega t) = A{\bf \hat{e}} \frac{1}{2} \left[ e^{i({\bf k}\cdot {\bf r} -\omega t)} + e^{-i({\bf k}\cdot {\bf r} -\omega t)} \right], \end{align}</math>
|num=eq:A-field
}}

where <math>k^2 =\omega ^2 / c^2</math> and <math>{\bf \hat{e}}\cdot {\bf k}= 0</math>. For a linearly polarized field, the polarization vector <math>{\bf \hat{e}}</math> is real. For an elliptically polarized field it is complex, and for a circularly polarized field it is given by <math>{\bf \hat{e}} = ({\bf \hat{ x}} \pm i {\bf \hat{ y}} ) /\sqrt {2}</math> , where the + and <math>-</math> signs correspond to positive and negative helicity, respectively. (Alternatively, they correspond to left and right hand circular polarization, respectively, the sign convention being a tradition from optics.) The electric and magnetic fields are then given by 

{{EqL
|math=<math>\begin{align} \  {\bf E}(r, t) = \omega A{\bf \hat{e}} \sin ({\bf k}\cdot {\bf r} -\omega t) = - i \omega A {\bf \hat{e}} \frac{1}{2} \left[ e^{i({\bf k}\cdot {\bf r} -\omega t)} - e^{-i({\bf k}\cdot {\bf r} -\omega t)} \right]. \end{align}</math>
|num=eq:E-field
}}

{{EqL
|math=<math>\begin{align} \  {\bf B}(r, t) = k ({\bf \hat{k}} \times {\bf \hat{ e}}) \sin ({\bf k}\cdot {\bf r} -\omega t) = - i k A ({\bf \hat{k}} \times {\bf \hat{ e}}) \frac{1}{2} \left[ e^{i({\bf k}\cdot {\bf r} -\omega t)} - e^{-i({\bf k}\cdot {\bf r} -\omega t)} \right]. \end{align}</math>
|num=eq:B-field
}}

The time average Poynting vector is 

{{EqL
|math=<math>\begin{align} \  {\bf S} = \frac{ \epsilon _0 c^2}{2} ( {{\bf E} \times {\bf B}^* )} = \frac{\epsilon _0 c}{2} \omega ^2 A^2 {\bf \hat{k}} . \end{align}</math>
|num=EQ_ wd9
}}

The average energy density in the wave is given by 

{{EqL
|math=<math>\begin{align} \  u = \omega ^2 \frac{\epsilon _0 }{2} A^2 {\bf \hat{k}} . \end{align}</math>
|num=eq:energy-density
}}

<br style="clear: both" />

=== Interaction of an electromagnetic wave and an atom ===

<span id="SEC_INT"></span> 

The behavior of charged particles in an electromagnetic field is correctly described by Hamilton's equations provided that the canonical momentum is redefined: 

{{EqL
|math=<math>\begin{align} \  {\bf p}_{\rm can} = {\bf p}_{\rm kin} + q {\bf A} \end{align}</math>
|num=EQ_ int1
}}

The kinetic energy is <math>{\bf p}_{\rm kin}^2 /2 m</math>. Taking <math>q = - e</math>, the Hamiltonian for an atom in an electromagnetic field in free space is 

{{EqL
|math=<math>\begin{align} \  H = \frac{1}{2m} \sum _{j=1}^{N} {\left( {\bf p}_ j + e {\bf A} (r_ j )\right)^2} + \sum _{j=1}^{N} V ({\bf r}_ j ), \end{align}</math>
|num=EQ_ int2
}}

where <math>V ( {\bf r}_ j )</math> describes the potential energy due to internal interactions. We are neglecting spin interactions. 

Expanding and rearranging, we have 

{{EqL
|math=<math>\begin{align} \  H & =&  \sum _{j=1}^{N} \frac{{\bf p}_ j^2}{2m} + V ({\bf r}_ j ) + \frac{e}{2m} \sum _{j=1}^{N} {\left({\bf p}_ j \cdot {\bf A} ( {\bf r}_ j) + {\bf A} ({\bf r}_ j ) \cdot {\bf p}_ j \right)} + \frac{e^2}{2m} \sum _{j=1}^{N} A_ j^2 ({\bf r} ) \\ &  = &  H_0 + H_{\rm int} + H^{(2)} .  \end{align}</math>
|num=EQ_ int3
}}

Here, <math>{\bf p}_ j = - i\hbar \nabla _ j </math>. Consequently, <math>H_0</math> describes the unperturbed atom. <math>H_{\rm int}</math> describes the atom's interaction with the field. <math>H^{(2)}</math>, which is second order in '''A''', plays a role only at very high intensities. (In a static magnetic field, however, <math>H^{(2)}</math> gives rise to diamagnetism.) 

Because we are working in the Coulomb gauge, <math>\nabla \cdot {\bf A} =0</math> so that '''A''' and '''p''' commute. We have 

{{EqL
|math=<math>\begin{align} \  H_{\rm int} = \frac{eA}{m} \hat{\bf {e}} \cdot {\bf p} \cos ({\bf k}\cdot {\bf r} -\omega t) . \end{align}</math>
|num=EQ_ int4
}}

It is convenient to write the matrix element between states <math> | a \rangle </math> and <math> | b \rangle </math> in the form 

{{EqL
|math=<math>\begin{align} \  \langle b | H_{\rm int} | a \rangle = \frac{1}{2} H_{ba} e^{-i\omega t} + \frac{1}{2} H_{ba} e^{+i\omega t}, \end{align}</math>
|num=EQ_ int5
}}

where 

{{EqL
|math=<math>\begin{align} \  H_{ba} = \frac{eA}{m} {\bf \hat{e}} \,  \langle b |{\bf p} \,  e^{i {\bf k} \cdot {\bf r}} | a \rangle . \end{align}</math>
|num=EQ_ int6
}}

Atomic dimensions are small compared to the wavelength of radiation involved in optical transitions. The scale of the ratio is set by <math>\alpha \approx 1/137</math>. Consequently, when the matrix element in Eq. [[{{SUBPAGENAME}}#EQ_int6|EQ_int6]] is evaluated, the wave function vanishes except in the region where <math>{\bf k}\cdot {\bf r} = 2 \pi r /\lambda \ll 1</math>. It is therefore appropriate to expand the exponential: 

{{EqL
|math=<math>\begin{align} \  H_{ba} = \frac{eA}{m} {\bf \hat{e}} \cdot \langle b | {\bf p} (1 + i{\bf k} \cdot {\bf r} - 1/2 ({\bf k}\cdot {\bf r} )^2 + \cdots ) | a \rangle \end{align}</math>
|num=EQ_ int7
}}

Unless <math>\langle b | {\bf p} | a \rangle </math> vanishes, for instance due to parity considerations, the leading term dominates and we can neglect the others. For reasons that will become clear, this is called the dipole approximation. This is by far the most important situation, and we shall defer consideration of the higher order terms. In the dipole approximation we have 

{{EqL
|math=<math>\begin{align} \  H_{ba} = \frac{eA}{m} {\bf \hat{e}} \cdot \langle b | {\bf p} | a \rangle = \frac{-ieE}{m\omega } {\bf \hat{e}} \cdot \langle b | {\bf p} | a \rangle \end{align}</math>
|num=EQ_ int8
}}

where we have used, from Eq. [[{{SUBPAGENAME}}#eq:E-field|eq:E-field]], <math>A = -iE/\omega </math>. It can be shown (i.e. left as exercise) that the matrix element of '''p''' can be transfomred into a matrix element for <math>{\bf r}</math>: 

{{EqL
|math=<math>\begin{align} \  \langle b | {\bf p} | a \rangle = - i m \omega _{ab} \langle b | {\bf r} | a \rangle = + i m \omega _{ba} \langle b | {\bf r} | a \rangle \end{align}</math>
|num=EQ_ int9
}}

This results in 

{{EqL
|math=<math>\begin{align} \  H_{ba} = \frac{e E \omega _{ba}}{\omega } {\bf \hat{e}} \cdot \langle b | {\bf r} | a \rangle \end{align}</math>
|num=EQ_ int10
}}

We will be interested in resonance phenomena in which <math>\omega \approx \omega _{ba}</math>. Consequently, 

{{EqL
|math=<math>\begin{align} \  H_{ba} = + e {\bf E}_0 \cdot \langle b | {\bf r} | a \rangle = - {\bf d}_{ba} \cdot {\bf E} \end{align}</math>
|num=EQ_ int11
}}

where '''d ''' is the dipole operator, <math>{\bf d} = - e {\bf r}</math>. Displaying the time dependence explictlty, we have 

{{EqL
|math=<math>\begin{align} \  H_{ba}^\prime = - {\bf d}_{ba}\cdot {\bf E}_0 e^{-i\omega t}. \end{align}</math>
|num=EQ_ int12
}}

However, it is important to bear in mind that this is only the first term in a series, and that if it vanishes the higher order terms will contribute a perturbation at the driving frequency. 

<math>H_{ba}</math> appears as a matrix element of the momentum operator '''p''' in Eq. [[{{SUBPAGENAME}}#EQ_int8|EQ_int8]], and of the dipole operator '''r''' in Eq. [[{{SUBPAGENAME}}#EQ_int11|EQ_int11]]. These matrix elements look different and depend on different parts of the wave function. The momentum operator emphasizes the curvature of the wave function, which is largest at small distances, whereas the dipole operator evaluates the moment of the charge distribution, i.e. the long range behavior. In practice, the accuracy of a calculation can depend significantly on which operator is used. 

<br style="clear: both" />

== Quantization of the radiation field ==

<span id="SEC_QRD"></span> 

We shall consider a single mode of the radiation field. This means a single value of the wave vector '''k''', and one of the two orthogonal transverse polarization vectors <math>{\bf \hat{e}}</math>. The radiation field is described by a plane wave vector potential of the form Eq. [[{{SUBPAGENAME}}#eq:A-field|eq:A-field]]. We assume that '''k''' obeys a periodic boundary or condition, <math>k_ x L_ x = 2\pi n_ x</math>, etc. (For any '''k''', we can choose boundaries <math>L_ x , L_ y , L_ z</math> to satisfy this.) The time averaged energy density is given by Eq. [[{{SUBPAGENAME}}#eq:energy-density|eq:energy-density]], and the total energy in the volume V defined by these boundaries is 

{{EqL
|math=<math>\begin{align} \  U = \frac{\epsilon _0 }{2}\omega ^2 A^2 V, \end{align}</math>
|num=eq:energy-total
}}

where <math>A^2</math> is the mean squared value of <math>A</math> averaged over the spatial mode. We now make a formal connection between the radiation field and a harmonic oscillator. We define variables Q and P by 

{{EqL
|math=<math>\begin{align} \  A = \frac{1}{\omega } \sqrt {\frac{1}{\epsilon _ o V}} (\omega Q + iP ), ~ ~ A^* =\frac{1}{\omega }\sqrt {\frac{1}{\epsilon _ o V}} (\omega Q - iP ). \end{align}</math>
|num=EQ_ qrd5
}}

Then, from Eq. [[{{SUBPAGENAME}}#eq:energy-total|eq:energy-total]], we find 

{{EqL
|math=<math>\begin{align} \  U = \frac{1}{2} (\omega ^2 Q^2 + P^2 ). \end{align}</math>
|num=EQ_ qrd6
}}

This describes the energy of a harmonic oscillator having unit mass. We quantize the oscillator in the usual fashion by treating Q and P as operators, with 

{{EqL
|math=<math>\begin{align} \  P = - i\hbar \frac{\partial }{\partial Q}, ~ ~ ~ [Q,P] = i\hbar . \end{align}</math>
|num=EQ_ qrd7
}}

We introduce the operators <math>a</math> and <math>a^\dagger </math> defined by 

{{EqL
|math=<math>\begin{align} \  a = \frac{1}{\sqrt {2\hbar \omega }} (\omega Q + iP ) \end{align}</math>
|num=EQ_ qrd8
}}

{{EqL
|math=<math>\begin{align} \  a^\dagger = \frac{1}{\sqrt {2\hbar \omega }} (\omega Q - iP ) \end{align}</math>
|num=EQ_ qrd9
}}

The fundamental commutation rule is 

{{EqL
|math=<math>\begin{align} \  [a, a^\dagger ] = 1 \end{align}</math>
|num=EQ_ qrd10
}}

from which the following can be deduced: 

{{EqL
|math=<math>\begin{align} \  H = \frac{1}{2} \hbar \omega [a^\dagger a + a a^\dagger ] = \hbar \omega \left[a^\dagger a + \frac{1}{2} \right] = \hbar \omega \left[N+ \frac{1}{2} \right] \end{align}</math>
|num=EQ_ qrd11
}}

where the number operator <math>N = a^\dagger a </math> obeys 

{{EqL
|math=<math>\begin{align} \  N| n \rangle = n| n \rangle \end{align}</math>
|num=EQ_ qrd12
}}

We also have 

{{EqL
|math=<math>\begin{align}  \langle n-1| a | n \rangle & =&  \sqrt {n}  \\ \langle n+1| a^\dagger | n \rangle & =&  \sqrt {n +1}  \\ \langle n| a^\dagger a | n \rangle & =&  n  \\ \langle n |a a^\dagger | n \rangle & =&  n+1  \\ \langle n| H | n \rangle & =&  \hbar \omega \left(n+ \frac{1}{2} \right)  \\ \  \langle n| a | n \rangle & =&  \langle n | a^\dagger | n \rangle = 0 \end{align}</math>
|num=EQ_ qrd13
}}

The operators <math>a </math> and <math>a^\dagger </math> are called the annihilation and creation operators, respectively. We can express the vector potential and electric field in terms of <math>a</math> and <math>a^\dagger </math> as follows 

{{EqL
|math=<math>\begin{align} \  A = \frac{1}{ \omega \sqrt {\epsilon _ o V}} (\omega Q + iP) = \sqrt {\frac{2 \hbar }{ \omega \epsilon _ o V}} a \end{align}</math>
|num=EQ_ part1
}}

{{EqL
|math=<math>\begin{align} \  A^\dagger = \frac{1}{ \omega \sqrt {\epsilon _ o V}} (\omega Q - iP) = \sqrt {\frac{2 \hbar }{ \omega \epsilon _ o V}} a^\dagger \end{align}</math>
|num=EQ_ part2
}}

{{EqL
|math=<math>\begin{align} \  {\bf E} = - i \sqrt {\frac{ \hbar \omega }{2 \epsilon _ o V} } {\left[ a{\bf \hat{e}} e^{i({\bf k}\cdot {\bf r} - \omega t)} - a^\dagger {\bf \hat{e}}^* e^{-i({\bf k}\cdot {\bf r} -\omega t)}\right]} \end{align}</math>
|num=EQ_ part3
}}

In the dipole limit we can take <math>e^{i {\bf k}\cdot {\bf r}} = 1</math>. Then 

{{EqL
|math=<math>\begin{align} \  {\bf E} = - i \sqrt {\frac{ \hbar \omega }{2 \epsilon _ o V} } \left[ a {\bf \hat e} e^{-i \omega t}- a^\dagger {\bf {\hat e}}^* e^{i \omega t}\right] \end{align}</math>
|num=EQ_ part3
}}

The interaction Hamiltonian is, 

{{EqL
|math=<math>\begin{align} \  H_{\rm int}= -ie \sqrt {\frac{\hbar \omega }{2\epsilon _ o V}}{\bf r}\cdot {\left[ a{\bf \hat{e}} e^{-i\omega t} - a^\dagger {\bf \hat{e}}^* e^{+i\omega t}\right]}, \end{align}</math>
|num=EQ_ qrd16
}}

where we have written the dipole operator as <math>{\bf d} = - e {\bf r}</math>. 

<br style="clear: both" />

== Interaction of a two-level system and a single mode of the radiation field ==

<span id="SEC_vac"></span> 

We consider a two-state atomic system <math> | a \rangle </math>,  <math>| b \rangle </math> and a radiation field described by <math>| n \rangle ,\  n = 0,1,2 \dots </math> The states of the total system can be taken to be 

{{EqL
|math=<math>\begin{align} \  | I \rangle = | a,\  n \rangle = | a \rangle \  | n \rangle , ~ ~ ~  | F \rangle = | b,\  n^\prime \rangle = |b \rangle \   |n^\prime \rangle . \end{align}</math>
|num=EQ_ vac1
}}

We shall take <math>{\bf \hat{e}} = {\bf \hat{ z}} </math>. Then 

{{EqL
|math=<math>\begin{align} \  \langle F |H_{\rm int} | I \rangle = -i e z_{ab} \sqrt {\frac{2\pi \hbar \omega }{V}} \langle n^\prime | a e^{-i\omega t} - a^\dagger e^{i\omega t} | n \rangle e^{-i\omega _{ab} t} \end{align}</math>
|num=EQ_ vac2
}}

The first term in the bracket obeys the selection rule <math>n^\prime = n - 1</math>. This corresponds to loss of one photon from the field and absorption of one photon by the atom. The second term obeys <math>n^\prime = n + 1</math>. This corresponds to emission of a photon by the atom. Using Eq. [[{{SUBPAGENAME}}#EQ_qrd13|EQ_qrd13]], we have 

{{EqL
|math=<math>\begin{align} \  \langle F | H_{\rm int} | I \rangle = -i e z_{ab} \sqrt {\frac{2\pi \hbar \omega }{V}} {\left( \sqrt {n}\, \delta _{n\prime ,n-1} \  e^{-i \omega t} - \sqrt {n+1}\, \delta _{n\prime ,n+1} e^{+i\omega t} \right)} \  e^{-i\omega _{ab} t} \end{align}</math>
|num=EQ_ vac3
}}

Transitions occur when the total time dependence is zero, or near zero. Thus absorption occurs when <math>\omega =- \omega _{ab}</math>, or <math>E_ a + \hbar \omega = E_ b</math>. As we expect, energy is conserved. Similarly, emission occurs when <math>\omega = + \omega _{ab}</math>, or <math>E_ a - \hbar \omega = E_ b</math>. 

A particularly interesting case occurs when <math>n = 0</math>, i.e.  the field is initially in the vacuum state, and <math>\omega = \omega _{ab}</math>. Then 

{{EqL
|math=<math>\begin{align} \  \langle F | H_{\rm int} | I \rangle = i e z_{ab} \sqrt {\frac{2\pi \hbar \omega }{V}} \equiv H_{FI}^0 \end{align}</math>
|num=EQ_ vac4
}}

The situation describes a constant perturbation <math>H_{FI}^0</math> coupling the two states <math>I = | a , n = 0 \rangle </math> and <math>F = | b, n^\prime = 1 \rangle </math>. The states are degenerate because <math>E_ a = E_ b + \hbar \omega </math>. Consequently, <math>E_ a</math> is the upper of the two atomic energy levels. 

The system is composed of two degenerate eigenstates, but due to the coupling of the field, the degeneracy is split. The eigenstates are symmetric and antisymmetric combinations of the initial states, and we can label them as 

{{EqL
|math=<math>\begin{align} \  | \pm \rangle = \frac{1}{\sqrt {2}} (|I \rangle \pm | F \rangle ) = \frac{1}{\sqrt {2}} ( | a , 0 \rangle \pm | b, 1 \rangle ). \end{align}</math>
|num=EQ_ vac5
}}

The energies of these states are 

{{EqL
|math=<math>\begin{align} \  E_{\pm } = \pm | H_{FI}^0 | \end{align}</math>
|num=EQ_ vac6
}}

If at <math>t = 0</math>, the atom is in state <math>| a \rangle </math> which means that the radiation field is in state <math>| 0 \rangle </math> then the system is in a superposition state: 

{{EqL
|math=<math>\begin{align} \  \psi (0) = \frac{1}{\sqrt {2}} ( | + \rangle + | - \rangle ) . \end{align}</math>
|num=EQ_ vac7
}}

The time evolution of this superposition is given by 

{{EqL
|math=<math>\begin{align} \  \psi (t) = \frac{1}{\sqrt {2}} \left(| + \rangle e^{i\Omega /2t} + | - \rangle e^{-i\Omega /2t} \right) \end{align}</math>
|num=EQ_ vac8
}}

where <math>\Omega / 2 = | H_{FI}^0 | / \hbar = e z_{ab}\sqrt {\omega / (e \epsilon _ o V \hbar )}</math>. The probability that the atom is in state <math> | b \rangle </math> at a later time is 

{{EqL
|math=<math>\begin{align} \  P_ b = \frac{1}{2} (1 + \cos \Omega t ). \end{align}</math>
|num=EQ_ vac9
}}

The frequency <math>\Omega </math> is called the vacuum Rabi frequency. 

The dynamics of a 2-level atom interacting with a single mode of the vacuum were first analyzed in [JAC63] and the oscillations are sometimes called <i>
Jaynes-Cummings
</i> oscillations. 

The atom-vacuum interaction <math>H_{FI}^0</math>, Eq. [[{{SUBPAGENAME}}#EQ_vac4|EQ_vac4]], has a simple physical interpretation. The electric field amplitude associated with the zero point energy in the cavity is given by 

{{EqL
|math=<math>\begin{align} \  \epsilon _ o E^2 V = \frac{1}{2} \hbar \omega \end{align}</math>
|num=EQ_ vac10
}}

Consequently, <math>| H_{FI}^0 | = E d_{ab}= ez_{ab} E</math>. The interaction frequency <math>| H_{FI}^0 | / \hbar </math> is sometimes referred to as the vacuum Rabi frequency, although, as we have seen, the actual oscillation frequency is <math>2 \times H_{FI}^0 /\hbar </math>. 

Absorption and emission are closely related. Because the rates are proportional to <math>| \langle F | H_{\rm int} | I \rangle |^2</math>, it is evident from Eq. [[{{SUBPAGENAME}}#EQ_vac3|EQ_vac3]] that 

{{EqL
|math=<math>\begin{align} \  \frac{\rm Rate~ of~ emission}{\rm Rate~ of~ absorption} = \frac{n+1}{n} \end{align}</math>
|num=EQ_ vac11
}}

This result, which applies to radiative transitions between any two states of a system, is general. In the absence of spontaneous emission, the absorption and emission rates are identical. 

The oscillatory behavior described by Eq. [[{{SUBPAGENAME}}#EQ_vac8|EQ_vac8]] is exactly the opposite of free space behavior in which an excited atom irreversibly decays to the lowest available state by spontaneous emission. The distinction is that in free space there are an infinite number of final states available to the photon, since it can go off in any direction, but in the cavity there is only one state. The natural way to regard the atom-cavity system is not in terms of the atom and cavity separately, as in Eq. [[{{SUBPAGENAME}}#EQ_vac1|EQ_vac1]], but in terms of the coupled states <math>| + \rangle </math> and <math>| - \rangle </math> (Eq. [[{{SUBPAGENAME}}#EQ_vac5|EQ_vac5]]). Such states, called <i>
dressed atom
</i> states, are the true eigenstates of the atom-cavity system. 

<br style="clear: both" />

== Absorption and emission ==

<span id="SEC_abem"></span> 

In Chapter 6, first-order perturbation theory was applied to find the response of a system initially in state <math>|a\rangle </math> to a perturbation of the form <math>( H_{ba}/2 ) e^{-i\omega t}</math>. The result is that the amplitude for state <math>|b \rangle </math> is given by 

{{EqL
|math=<math>\begin{align} \  a_ b (t) = \frac{1}{2 i\hbar } \int _0^ t H_{ba} e^{-i(\omega - \omega _{ba} )t^\prime } dt^\prime = \frac{H_{ba}}{2\hbar } {\left[ \frac{e^{-i(\omega - \omega _{ba} )t} -1}{\omega - \omega _{ba}} \right]} \end{align}</math>
|num=EQ_ abem1
}}

There will be a similar expression involving the time-dependence <math>e^{+ i \omega t}</math>. The <math>- i \omega </math> term gives rise to resonance at <math>\omega = \omega _{ba}</math>; the <math>+ i \omega </math> term gives rise to resonance at <math>\omega = -\omega _{ab}</math>. One term is responsible for absorption, the other is responsible for emission. 

The probability that the system has made a transition to state <math>| b \rangle </math> at time <math>t</math> is 

{{EqL
|math=<math>\begin{align} \  W_{a\rightarrow b} = | a_ b (t)|^2 = \frac{| H_{ba}|^2}{4 \hbar ^2} \frac{\sin ^2 [(\omega - \omega _{ba} )t/2]}{((\omega - \omega _{ba} )t/2)^2}t^2 \end{align}</math>
|num=EQ_ abem2
}}

In the limit <math>\omega \rightarrow \omega _{ba}</math>, we have 

{{EqL
|math=<math>\begin{align} \  W_{a\rightarrow b} \approx \frac{| H_{ba}|^2}{4 \hbar ^2} t^2 . \end{align}</math>
|num=EQ_ abem3
}}

So, for short time, <math>W_{a\rightarrow b}</math> increases quadratically. This is reminiscent of a Rabi resonance in a 2-level system in the limit of short time. 

However, Eq. [[{{SUBPAGENAME}}#EQ_abem2|EQ_abem2]] is only valid provided <math>W_{a\rightarrow b} \ll 1</math>, or for time <math>T \ll \hbar /H_{ba}</math>. For such a short time, the incident radiation will have a spectral width <math>\Delta \omega \sim 1/T</math>. In this case, we must integrate Eq. [[{{SUBPAGENAME}}#EQ_abem2|EQ_abem2]] over the spectrum. In doing this, we shall make use of the relation 

{{EqL
|math=<math>\begin{align} \  \int _{-\infty }^{+\infty } \frac{\sin ^2 (\omega - \omega _{ba})t/2}{[(\omega - \omega _{ba})/2]^2} d \omega = 2t \int _{-\infty }^{+\infty } \frac{\sin ^2 (u - u_ o)}{(u - u_ o)^2} d u \rightarrow 2 \pi t \int _{-\infty }^{+\infty } \delta (\omega - \omega _{ba} ) d \omega . \end{align}</math>
|num=EQ_ abem4
}}

Eq. [[{{SUBPAGENAME}}#EQ_abem2|EQ_abem2]] becomes 

{{EqL
|math=<math>\begin{align} \  W_{a\rightarrow b} = \frac{| H_{ba}|^2}{\hbar ^2} 2\pi t \delta (\omega - \omega _{ba} ) \end{align}</math>
|num=EQ_ abem5
}}

The <math>\delta </math>-function requires that eventually <math>W_{a\rightarrow b}</math> be integrated over a spectral distribution function. Absorbing an <math> \hbar </math> into the delta function, <math>W_{a\rightarrow b}</math> can be written 

{{EqL
|math=<math>\begin{align} \  W_{a\rightarrow b} = \frac{| H_{ba}|^2}{\hbar} 2\pi t \delta (E_ b - E_ a - \hbar \omega ). \end{align}</math>
|num=EQ_ abem6
}}

Because the transition probability is proportional to the time, we can define the transition rate 

{{EqL
|math=<math>\begin{align} \  \Gamma _{ab} = \frac{d}{dt} W_{a\rightarrow b} = 2\pi \frac{| H_{ba}|^2}{\hbar} \delta (\omega - \omega _{ba}) \end{align}</math>
|num=EQ_ abem7a
}}

{{EqL
|math=<math>\begin{align} \  = 2\pi \frac{| H_{ba}|^2}{\hbar } \delta (E_ b - E_ a - \hbar \omega ) \end{align}</math>
|num=EQ_ abem7b
}}

The <math>\delta </math>-function arises because of the assumption in first order perturbation theory that the amplitude of the initial state is not affected significantly. This will not be the case, for instance, if a monochromatic radiation field couples the two states, in which case the amplitudes oscillate between 0 and 1. However, the assumption of perfectly monochromatic radiation is in itself unrealistic. 

Radiation always has some spectral width. <math>| H_{ba}|^2</math> is proportional to the intensity of the radiation field at resonance. The intensity can be written in terms of a spectral density function 

:<math>\begin{align} S(\omega ^\prime ) = S_0 f(\omega ^\prime ) \end{align}</math>

where <math>S_0</math> is the incident Poynting vector, and f(<math>\omega ^\prime </math>) is a normalized line shape function centered at the frequency <math>\omega ^\prime </math> which obeys <math>\int f (\omega ^\prime ) d\omega ^\prime = 1</math>. We can define a characteristic spectral width of <math>f(\omega ^\prime )</math> by 

{{EqL
|math=<math>\begin{align} \  \Delta \omega = \frac{1}{f(\omega _{ab} )} \end{align}</math>
|num=EQ_ abem8
}}

Integrating Eq. [[{{SUBPAGENAME}}#EQ_abem7b|EQ_abem7b]] over the spectrum of the radiation gives 

{{EqL
|math=<math>\begin{align} \  \Gamma _{ab} = \frac{2\pi | H_{ba}|^2}{\hbar ^2} f(\omega _{ab} ) \end{align}</math>
|num=EQ_ abem9
}}

If we define the effective Rabi frequency by 

{{EqL
|math=<math>\begin{align} \  \Omega _ R = \frac{| H_{ba}| }{\hbar } \end{align}</math>
|num=EQ_ abem10
}}

then 

{{EqL
|math=<math>\begin{align} \  \Gamma _{ab} = {2 \pi } \frac{\Omega _ R^2}{\Delta \omega } \end{align}</math>
|num=EQ_ abem11
}}

Another situation that often occurs is when the radiation is monochromatic, but the final state is actually composed of many states spaced close to each other in energy so as to form a continuum. If such is the case, the density of final states can be described by 

{{EqL
|math=<math>\begin{align} \  dN= \rho (E) dE \end{align}</math>
|num=EQ_ abem12
}}

where <math>dN</math> is the number of states in range <math>dE</math>. Taking <math>\hbar \omega = E_ b - E_ a</math> in Eq. [[{{SUBPAGENAME}}#EQ_abem7b|EQ_abem7b]], and integrating gives 

{{EqL
|math=<math>\begin{align} \  \Gamma _{ab} = 2\pi \frac{| H_{ba}|^2}{\hbar^2 } \rho (E_ b ) \end{align}</math>
|num=EQ_ abem13
}}

This result remains valid in the limit <math>E_ b\rightarrow E_ a</math>, where <math>\omega \rightarrow 0</math>. In this static situation, the result is known as <i>
Fermi's Golden Rule
</i>. 

Note that Eq. [[{{SUBPAGENAME}}#EQ_abem9|EQ_abem9]] and Eq. [[{{SUBPAGENAME}}#EQ_abem13|EQ_abem13]] both describe a uniform rate process in which the population of the initial state decreases exponentially in time. If the population of the initial state is <math>P(0)</math>, then 

{{EqL
|math=<math>\begin{align} \  P(t) = P(0) e^{-\Gamma _{ba} t} \end{align}</math>
|num=EQ_ abem14
}}

Applying this to the dipole transition described in Eq. [[{{SUBPAGENAME}}#EQ_int11|EQ_int11]], we have 

{{EqL
|math=<math>\begin{align} \  \Gamma _{ab} = 2\pi \frac{E^2 d_{ba}^2}{\hbar ^2} f(\omega ) \end{align}</math>
|num=EQ_ abem15
}}

The arguments here do not distinguish whether <math>E_ a < E_ b</math> or <math>E_ a > E_ b</math> (though the sign of <math>\omega = ( E_ b - E_ a )/\hbar </math> obviously does). In the former case the process is absorption, in the latter case it is emission. 

<br style="clear: both" />

== Spontaneous emission rate ==

<span id="SEC_sem"></span> 

The rate of absorption, in CGS units, for the transition <math>a \rightarrow b</math>, where <math>E_ b > E_ a</math>, is, from Eq. [[{{SUBPAGENAME}}#EQ_qrd16|EQ_qrd16]] and Eq. [[{{SUBPAGENAME}}#EQ_abem7b|EQ_abem7b]], 

{{EqL
|math=<math>\begin{align} \  \Gamma _{ab} = \frac{4\pi ^2}{\hbar V} | {\bf \hat{e}} \cdot {\bf d}_{ba} |^2 n\omega \delta (\omega _0 -\omega ) . \end{align}</math>
|num=EQ_ sem1
}}

where <math>\omega _0 = ( E_ b - E_ a ) /\hbar </math>. To evaluate this we need to let <math>n \rightarrow n (\omega )</math>, where <math>n (\omega ) d\omega </math> is the number of photons in the frequency interval <math>d\omega </math>, and integrate over the spectrum. The result is 

{{EqL
|math=<math>\begin{align} \  \Gamma _{ab} = \frac{4\pi ^2}{\hbar V} | {\bf \hat{e}}\cdot {\bf d}_{ba} |^2 \omega _0 n(\omega _0 ) \end{align}</math>
|num=EQ_ sem2
}}

To calculate <math>n (\omega )</math>, we first calculate the mode density in space by applying the usual periodic boundary condition 

{{EqL
|math=<math>\begin{align} \  k_ j L = 2\pi n_ j , ~ ~ ~ j = x,y,z. \end{align}</math>
|num=EQ_ sem3
}}

The number of modes in the range <math>d^3 k = dk_ x dk_ y dk_ z</math> is 

{{EqL
|math=<math>\begin{align}  \  dN = dn_ x dn_ y dn_ z = \frac{V}{{\left(2 \pi \right)^3} } d^3 k=\frac{V}{{\left(2 \pi \right)^3} }k^2 dk \  d\Omega = \frac{V}{{\left(2 \pi \right)^3} } \frac{\omega ^2\,  d\omega \  d\Omega }{c^3} \end{align}</math>
|num=EQ_ sem4
}}

Letting <math>\bar{n} = \bar{n (\omega ) }</math> be the average number of photons per mode, then 

{{EqL
|math=<math>\begin{align} \  n (\omega ) = \bar{n} \frac{dN}{d\omega } = \frac{\bar{n} V\omega ^2 d\Omega }{(2\pi )^3 c^3} \end{align}</math>
|num=EQ_ sem5
}}

Introducing this into Eq. [[{{SUBPAGENAME}}#EQ_sem2|EQ_sem2]] gives 

{{EqL
|math=<math>\begin{align} \  \Gamma _{ab} = \frac{\bar{n}\omega ^3}{2\pi \hbar c^3} | {\bf \hat{e}} \cdot {\bf d}_{ba} |^2 d\Omega \end{align}</math>
|num=EQ_ sem6
}}

We wish to apply this to the case of isotropic radiation in free space, as, for instance, in a thermal radiation field. We can take <math>{\bf d}_{ba}</math> to lie along the <math>z</math> axis and describe '''k''' in spherical coordinates about this axis. Since the wave is transverse, <math>{\bf \hat{e}} \cdot {\bf \hat{D}} = \sin \theta </math> for one polarization, and zero for the other one.  Consequently, 

{{EqL
|math=<math>\begin{align} \  \int | {\bf \hat{e}} \cdot {\bf d}_{ba} |^2 d\Omega = | {\bf d}_{ba} |^2 \int \sin ^2 \theta d\Omega = \frac{8\pi }{3} | {\bf d}_{ba}|^2 \end{align}</math>
|num=EQ_ sem7
}}

Introducing this into Eq. [[{{SUBPAGENAME}}#EQ_sem6|EQ_sem6]] yields the absorption rates 

{{EqL
|math=<math>\begin{align} \  \Gamma _{ab} = \frac{4}{3} \frac{\omega ^3}{\hbar c^3} | {\bf d}_{ba} |^2 \bar{n} \end{align}</math>
|num=EQ_ sem8
}}

It follows that the emission rate for the transition <math>b\rightarrow a</math> is 

{{EqL
|math=<math>\begin{align} \  \Gamma _{ba} = \frac{4}{3} \frac{\omega ^3}{\hbar c^3} | {\bf d}_{ba} |^2 (\bar{n} + 1) \end{align}</math>
|num=EQ_ sem9
}}

If there are no photons present, the emission rate—called the rate of spontaneous emission—is 

{{EqL
|math=<math>\begin{align} \  \Gamma _{ba}^0 = \frac{4}{3} \frac{ \omega ^3}{\hbar c^3} | {\bf d}_{ba}|^2 = \frac{4}{3} \frac{e^2\omega ^3}{\hbar c^3} | \langle b| {\bf r} | a \rangle |^2 \end{align}</math>
|num=EQ_ sem10
}}

In atomic units, in which <math>c = 1 / \alpha </math>, we have 

{{EqL
|math=<math>\begin{align} \  \Gamma _{ba}^0 = \frac{4}{3} \alpha ^3 \omega ^3 | {\bf r}_{ba} |^2 . \end{align}</math>
|num=EQ_ sem11
}}

Taking, typically, <math>\omega = 1</math>, and <math>r_{ba}= 1</math>, we have <math>\Gamma ^0 \approx \alpha ^3</math>. The “<math>Q</math>'' of a radiative transition is <math>Q =\omega /\Gamma \approx \alpha ^{-3}\approx </math> <math>3 \times 10^6</math>. The <math>\alpha ^3</math> dependence of <math>\Gamma </math> indicates that radiation is fundamentally a weak process: hence the high <math>Q</math> and the relatively long radiative lifetime of a state, <math>\tau = 1 /\Gamma </math>. For example, for the <math>2P\rightarrow 1S</math> transition in hydrogen (the <math>L_{\alpha }</math> transition), we have <math>\omega = 3/8</math>, and taking <math>r_{2p,1s} \approx 1</math>, we find <math>\tau = 3.6\times 10^7</math> atomic units, or 0.8 ns. The actual lifetime is 1.6 ns. 

The lifetime for a strong transition in the optical region is typically 10–100 ns. Because of the <math>\omega ^3</math> dependence of <math>\Gamma ^0</math>, the radiative lifetime for a transition in the microwave region—for instance an electric dipole rotational transition in a molecule—is longer by the factor <math> ( \lambda _{\rm microwave} /\lambda _{\rm optical} )^3 \approx 10^{15}</math>, yielding lifetimes on the order of months. Furthermore, if the transition moment is magnetic dipole rather than electric dipole, the lifetime is further increased by a factor of <math>\alpha ^{-2}</math>, giving a time of thousands of years. 

<br style="clear: both" />

== Line Strength ==

<span id="EQ_LINES"></span> 

Because the absorption and stimulated emission rates are proportional to the spontaneous emission rate, we shall focus our attention on the Einstein A coefficient: 

{{EqL
|math=<math>\begin{align} \  A_{ba} = \frac{4}{3} \frac{e^2\omega ^3}{\hbar c^3} | \langle b | {\bf r} | a \rangle |^2 \end{align}</math>
|num=EQ_ lines1
}}

where 

{{EqL
|math=<math>\begin{align} \  | \langle b | {\bf r} | a \rangle |^2 = | \langle b | x | a \rangle |^2 + | \langle b | y | a \rangle |^2 + | \langle b | z | a \rangle |^2 \end{align}</math>
|num=EQ_ lines2
}}

For an isolated atom, the initial and final states will be eigenstates of total angular momentum. (If there is an accidental degeneracy, as in hydrogen, it is still possible to select angular momentum eigenstates.) If the final angular momentum is <math>J_ a</math>, then the atom can decay into each of the <math>2 J_ a + 1</math> final states, characterized by the azimuthal quantum number <math>m_ a = -J_ a , -J_ a + 1,\dots , +J_ a</math>. Consequently, 

{{EqL
|math=<math>\begin{align} \  A_{ba} = \frac{4}{3} \frac{e^2\omega ^3}{\hbar c^3}\sum _{m_ a} | \langle b, J_ b | {\bf r} |a, J_ a, m_ a \rangle |^2 \end{align}</math>
|num=EQ_ lines3
}}

The upper level, however, is also degenerate, with a (<math>2 J_ b + 1</math>)–fold degeneracy. The lifetime cannot depend on which state the atom happens to be in. This follows from the isotropy of space: <math>m_ b</math> depends on the orientation of <math>{\bf J}_ b</math> with respect to some direction in space, but the decay rate for an isolated atom can't depend on how the atom happens to be oriented. Consequently, it is convenient to define the <i>
line strength
</i> <math>S_{ba}</math>, given by 

{{EqL
|math=<math>\begin{align} \  S_{ba} = S_{ab} = \sum _{m_ b} \sum _{m_ a} | \langle b, J_ b, m_ b | {\bf r} | a, J_ a, m_ a \rangle |^2 \end{align}</math>
|num=EQ_ lines4
}}

Then, 

{{EqL
|math=<math>\begin{align} \  A_{ba} = \frac{4}{3} \frac{e^2\omega ^3}{\hbar c^3} \frac{S_{ba}}{g_ b} = \frac{4}{3} \frac{e^2\omega ^3}{\hbar c^3} \frac{S_{ba}}{2J_ b +1} \end{align}</math>
|num=EQ_ lines5
}}

The line strength is closely related to the average oscillator strength <math>\bar{f}_{ab}</math>. <math>\bar{f}_{ab}</math> is obtained by averaging <math>f_{ab}</math> over the initial state <math>|b\rangle </math>, and summing over the values of <math>m</math> in the final state, <math>|a\rangle </math>. For absorption, <math>\omega _{ab} > 0</math>, and 

{{EqL
|math=<math>\begin{align} \  \bar{f}_{ab} = \frac{2m}{3\hbar } \omega _{ab} \frac{1}{2J_ b + 1} \sum _{m_ b} \sum _{m_ a} |\langle b, J_ b, m_ b |{\bf r} | a, J_ a, m_ a \rangle |^2 \end{align}</math>
|num=EQ_ line11
}}

It follows that 

{{EqL
|math=<math>\begin{align} \  \bar{f}_{ba} = - \frac{2J_ b + 1}{2J_ a +1} \bar{f}_{ab} . \end{align}</math>
|num=EQ_ line12
}}

In terms of the oscillator strength, we have 

{{EqL
|math=<math>\begin{align} \  \bar{f}_{ab} = \frac{2m}{3\hbar }\omega _{ab} \frac{1}{2J_ b + 1} {S}_{ab} . \end{align}</math>
|num=EQ_ line13
}}

{{EqL
|math=<math>\begin{align} \  \bar{f}_{ba} = - \frac{2m}{3\hbar } | \omega _{ab} | \frac{1}{2J_ a + 1} {S}_{ab} . \end{align}</math>
|num=EQ_ line14
}}

<br style="clear: both" />

== Excitation by narrow and broad band light sources ==

<span id="SEC_BROAD"></span> 

We have calculated the rate of absorption and emission of an atom in a thermal field, but a more common situation involves interaction with a light beam, either monochromatic or broad band. Here “broad band'' means having a spectral width that is broad compared to the natural line width of the system—the spontaneous decay rate. 

For an electric dipole transition, the radiation interaction is 

{{EqL
|math=<math>\begin{align} \  | H_{ba} | = e | {\bf r}_{ba} |\cdot {\bf \hat{e}} E/2, \end{align}</math>
|num=EQ_ broad1
}}

where <math>E </math> is the amplitude of the field. The transition rate, from Eq. [[{{SUBPAGENAME}}#EQ_sem7|EQ_sem7]], is 

{{EqL
|math=<math>\begin{align} \  W_{ab} = \frac{\pi }{2} \frac{e^2 | {\bf \hat{e}} \cdot {\bf r}_{ba} |^2 E^2}{\hbar ^2} f (\omega _0 ) = \frac{\pi }{2} \frac{e^2 | {\bf \hat{e}} \cdot {\bf r}_{ba} |^2 E^2}{\hbar } f(E_ b - E_ a ) \end{align}</math>
|num=EQ_ broad2
}}

where <math>\omega _0 = ( E_ b - E_ a )/\hbar </math> and <math>f (\omega )</math> is the normalized line shape function, or alternatively, the normalized density of states, expressed in frequency units. The transition rate is proportional to the intensity <math>I_0</math> of a monochromatic radiation source. <math>I_0</math> is given by the Poynting vector, and can be expressed by the electric field as <math>E^2 = 8 \pi I_0 / c</math>. Consequently, 

{{EqL
|math=<math>\begin{align} \  W_{ab} = \frac{4\pi ^2}{c} \frac{e^2 | {\bf \hat{e}} \cdot {\bf r}_{ba} |^2}{\hbar ^2} I_0 f (\omega _0 ) \end{align}</math>
|num=EQ_ broad3
}}

In the case of a Lorentzian line having a FWHM of <math>\Gamma _0</math> centered on frequency <math>\omega _0</math>, 

{{EqL
|math=<math>\begin{align} \  f(\omega ) = \frac{1}{\pi } \frac{(\Gamma _0 /2)}{(\omega - \omega _0 )^2 + (\Gamma _0 /2)^2} \end{align}</math>
|num=EQ_ broad4
}}

In this case, 

{{EqL
|math=<math>\begin{align} \  W_{ab} = \frac{8\pi e^2}{c\hbar ^2 \Gamma _0} | \langle b | {\bf \hat{e}} \cdot {\bf r} | a \rangle |^2 I_0 \end{align}</math>
|num=EQ_ broad5
}}

Note that <math>W_{ab}</math> is the rate of transition between two particular quantum states, not the total rate between energy levels. Naturally, we also have <math> W_{ab} = W_{ba}</math>.\

An alternative way to express Eq. [[{{SUBPAGENAME}}#EQ_broad2|EQ_broad2]] is to introduce the Rabi frequency, 

{{EqL
|math=<math>\begin{align} \  \Omega _ R = \frac{2 H_{ba}}{\hbar } = \frac{e |{\bf \hat{e}}\cdot {\bf r}_{ba} | E}{\hbar } \end{align}</math>
|num=EQ_ broad6
}}

In which case 

{{EqL
|math=<math>\begin{align} \  W_{ab} = \frac{\pi }{2} \Omega _ R^2 f (\omega _0 ) = \Omega _ R^2 \frac{1}{\Gamma _0} \end{align}</math>
|num=EQ_ broad7
}}

If the width of the final state is due soley to spontaneous emission, <math>\Gamma _0 = A = ( 4 e^2 \omega ^3 / 3 \hbar c^3 ) | r_{ba} |^2</math>. Since <math>W_{ab}</math> is proportional to <math> | r_{ba} |^2 /A_0</math>, it is independent of <math> | r_{ba} |^2</math>. It is left as a problem to find the exact relationship, but it can readily be seen that it is of the form 

{{EqL
|math=<math>\begin{align} \  W_{ab} = X\lambda ^2 I_0 /\hbar \omega \end{align}</math>
|num=EQ_ broad8
}}

where X is a numerical factor. <math>I/ \hbar \omega </math> is the photon flux—i.e. the number of photons per second per unit area in the beam. Since <math>W_{ab}</math> is an excitation rate, we interpret <math>X\lambda ^2</math> as the resonance absorption cross section for the atom, <math>\sigma _0</math>. 

At first glance it is puzzling that <math>\sigma _0</math> does not depend on the structure of the atom; one might expect that a transition with a large oscillator strength—i.e. a large value of <math>| r_{ab} |^2</math>—should have a large absorption cross section. However, the absorption rate is inversely proportional to the linewidth, and since that also increases with <math>| r_{ab}|^2</math>, the two factors cancel out. This behavior is not limited to electric dipole transitions, but is quite general. 

There is, however, an important feature of absorption that does depend on the oscillator strength. <math>\sigma _0</math> is the cross section assuming that the radiation is monochromatic compared to the natural line width. As the spontaneous decay rate becomes smaller and smaller, eventually the natural linewidth becomes narrower than the spectral width of the laser, or whatever source is used. In that case, the excitation becomes broad band. 

We now discuss broad band excitation. Using the result of the last section, finding the excitation rate or the absorption cross section for broad band excitation is trivial. From Eq. [[{{SUBPAGENAME}}#EQ_broad2|EQ_broad2]], the absorption rate is proportional to <math>f(\omega _0 )</math>. For monochromatic excitation, <math>f (\omega _0 ) = (2/ \pi ) A^{-1} </math> and <math>W_{\rm mono}= X\lambda ^2 I_0/\hbar \omega </math>. For a spectral source having linewidth <math>\Delta \omega _ s</math>, defined so that the normalized line shape function is <math>f (\omega _0 ) = (2/ \pi ) {\Delta \omega _ s}^{-1} </math>, then the broad band excitation rate is obtained by replacing <math>\Gamma _0</math> with <math>\Delta \omega _ s</math> in Eq. [[{{SUBPAGENAME}}#EQ_broad8|EQ_broad8]]. Thus 

{{EqL
|math=<math>\begin{align} \  W_ B = {\left( X\lambda ^2 \frac{\Gamma _0}{\Delta \omega _ s}\right)} \frac{I_0}{\hbar \omega } \end{align}</math>
|num=EQ_ band1
}}

Similarly, the effective absorption cross section is 

{{EqL
|math=<math>\begin{align} \  \sigma _{\rm eff} = \sigma _0 \frac{\Gamma _0}{\Delta \omega _ s} \end{align}</math>
|num=EQ_ band2
}}

This relation is valid provided <math>\Delta \omega _ s \gg \Gamma _0</math>. If the two widths are comparable, the problem needs to be worked out in detail, though the general behavior would be for <math>\Delta \omega _ s \rightarrow ( \Delta \omega _ s^2 + \Gamma _0^2 )^{1/2}</math>. Note that <math>\Delta \omega _ s</math> represents the actual resonance width. Thus, if Doppler broadening is the major broadening mechanism then 

{{EqL
|math=<math>\begin{align} \  \sigma _{\rm eff} = \sigma _0 \Gamma _0 /\Delta \omega _{\rm Doppler} . \end{align}</math>
|num=EQ_ band3
}}

Except in the case of high resolution laser spectroscopy, it is generally true that <math>\Delta \omega _ s \gg \Gamma _0</math>, so that <math>\sigma _{\rm eff}\ll \sigma _0</math>. 

<br style="clear: both" />
== Higher-order radiation processes ==

Beyond the dipole approximation:
Recall that the interaction Hamiltonian for an atom in an electromagnetic field is given by
:<math>
H_\mathrm{int} = -\frac{e}{mc} p\cdot A+\frac{e^2}{2mc^2}|A|^2+g_s\mu_B S\cdot({\bf\nabla}\times A),
</math>
where the last term we have so far considered only for static magnetic fields.  Neglecting, as before, the <math>|A|^2</math> term, which is appreciable only for very intense fields,  we now consider more fully the dominant term in the atom-field interaction,
:<math>
  H_{ba} = \frac{e}{\rm mc} \langle
  b | p \cdot A (r) | a\rangle.
</math>
For concreteness, we shall take A(r) to be a plane  wave of the form
:<math>
  A (r) = A\hat{z} e^{ikx}.
</math>
Expanding the exponential, we have
:<math>
  H_{ba} = \frac{eA}{\rm mc} \langle b | p_z (1+ikx + (ikx)^2/2 +
  \dots ) | a\rangle.
</math>
Thus far in the course, we have considered only the first term, the dipole term.  If dipole radiation is forbidden, for instance if <math>| a \rangle</math> and <math>| b \rangle</math> have the same parity, then the second term in the parentheses becomes important.  Usually, it is <math>\alpha</math> times smaller.  In particular, since
:<math>
k r \approx \frac{\hbar\omega}{\hbar c}a_0\approx\frac{e^2/a_0}{\hbar c}a_0\approx\frac{e^2}{\hbar c}=\alpha,
</math>
the expansion in \ref{eq:hor3} is effectively an expansion in <math>\alpha</math>.
We can rewrite the second term as follows:
:<math>
  p_z x = (p_z x - zp_x )/2 + (p_z x + zp_x )/2 .
</math>
The first term of Eq. \ref{eq:hor4} is <math>- \hbar L_y/2</math>, and the matrix element becomes
:<math>
  -\frac{ieAk}{2 m} \langle b | \hbar L_y |
  a \rangle  = - iAk \langle b | \mu_B
  L_y | a \rangle,
</math>
where <math>\mu_B = e\hbar /2 m</math> is the Bohr magneton.
The magnetic field is <math>B = - i k A \hat{y}</math>.
Consequently, Eq.\ \ref{eq:hor5} can be written in the more
familiar form <math>-\vec{\mu} \cdot B</math>. (The orbital magnetic moment is <math>\vec{\mu}
  = -\mu_B L</math>: the minus sign arises from our convention that <math>e</math> is
positive.)
We can readily generalize the matrix element to
:<math>
  H_{\rm int}(M1) = B \cdot \mu_B\langle b |L + g_sS| a\rangle,
</math>
where we have added the spin dependent term from Eq. \ref{eq:hor_Hint}.  <math>M1</math> indicates that the matrix element is for a magnetic dipole transition.  The strength of the <math>M1</math> transition is set by
:<math>
\mu_B/c = \frac{1}{2}\frac{e\hbar}{mc}=\frac{1}{2}\frac{e^2}{\hbar c}\frac{\hbar^2}{e m} = \frac{1}{2}\alpha e a_0,
</math>
so it is indeed a factor of <math>\alpha</math> weaker than a dipole transition, as we argued above.

The second term in Eq.\ \ref{eq:hor4} involves <math>( p_z x + z p_x
  )/2</math>.
Making use of the commutator relation <math>[ r, H_0 ] = i\hbar
p / m </math>, we
have
:<math>
  \frac{1}{2} (p_z x + z p_x) = \frac{m}{2i\hbar} ([z, H_0 ] x+ z[x,
  H_0 ]) =
  \frac{m}{2i\hbar} (- H_0 zx +zx H_0 ).
</math>
So, the contribution of this term to <math>H_{ba}</math> is
:<math>
  \frac{ieA}{mc} \frac{km}{2\hbar i} \langle b | - H_0 zx + zx H_0 |
  a \rangle  = - \frac{eAk}{2c} \frac{E_b - E_a}{\hbar} \langle b |
  zx | a \rangle
  = \frac{ieE\omega}{2c} \langle b | zx | a \rangle,
</math>
where we have taken <math>E = i k A</math>.  This is an electric
quadrupole interaction, and we shall denote the matrix element by
:<math>
  H_{\rm int} (E2)^\prime = \frac{ie\omega}{2c} \langle b | zx | a
  \rangle E.
</math>
The prime indicates that we are considering only one component of a
more general expression involving the matrix element <math>\langle b |r:r|a\rangle</math> of a tensor product.  It is straightforward to verify that the electric quadrupole interaction is also of order <math>\alpha</math>.

The total matrix element of the second term in the expansion of Eq.\ \ref{eq:hor3} can be written
:<math>
  H_{\rm int}^{(2)} = H_{\rm int} (M1) + H_{\rm int} (E2).
</math>
Note that <math>H_{\rm int} (M1)</math> is
real, whereas <math>H_{\rm int} (E2)</math> is imaginary.  Consequently,
:<math>| H_{\rm int}^{(2)} |^2 = | H_{\rm int} (M1)|^2 + |
  H_{\rm int}(E2) |^2.
</math>
The magnetic dipole and electric quadrupole terms do not
interfere.

Because transition rates depend on <math>|H_{ba} |^2</math>, the magnetic dipole and electric quadrupole rates
are both smaller than the dipole rate by <math>\alpha^2 \sim 5 \times
10^{-5}</math>.  For this reason they are generally referred to as {\it forbidden}
processes.  However, the term is used somewhat loosely, for there
are transitions which are much more strongly suppressed due to other
selection rules, as for instance triplet to singlet transitions in
helium.
\begin{table} 
<table border=1>

<tr><td>
Transition </td><td> </td><td> Operator </td><td> Parity </td></tr>

<tr><td>
Electric Dipole </td><td> <math>E1</math> </td><td> <math>-er</math> </td><td> - </td></tr>
<tr><td>
Magnetic Dipole </td><td> <math>M1</math> </td><td> <math>-\mu_B(L+g_sS)</math> </td><td> + </td></tr>
<tr><td>
Electric Quadrupole </td><td> <math>E2</math> </td><td> <math>-er:r</math> </td><td>  + </td></tr>

</table>
\caption{Summary of dipole and higher-order radiation processes.}
\end{table}

== Selection rules ==
A forbidden transition, then, is one that is weaker than an electric dipole-allowed transition by <math>\alpha^n</math> and only appears in some higher-order approximation.  Examples of such higher-order effects are the magnetic dipole and electric quadrupole terms described above, multiphoton processes, the relativistic effects which allow singlet to triplet transitions in helium, and hyperfine interactions within the nucleus.
To derive selection rules for the transitions we have discussed above, it is useful to express the matrix elements in terms of spherical tensor operators:
:<math>
H_{int}(T_{l,m}) = \langle n J M | T_{l,m} | n' J' M'\rangle,
</math>
where <math>T_{l,m}</math> is a spherical tensor operator of rank <math>l</math>.  The operators <math>T_{l,m}</math> transform under rotations like the spherical harmonics <math>Y_{l,m}</math>, and any operator can be written as a linear combination of these spherical tensors.  By the Wigner-Eckart Theorem, we can express the matrix element
:<math>
\langle n J M | T_{l,m} | n' J' M'\rangle = \frac{\langle n J \| T_l \| n' J' \rangle}{\sqrt{2J+1}}\langle J' l, M', m| J M\rangle
</math>
in terms of a reduced matrix element <math>\langle n J \| T_l \| n' J' \rangle</math> and a Clebsch-Gordan coefficient \linebreak<math>\langle J' l, M', m| J M\rangle</math>.  In order for the latter to be nonzero, the triangle rule requires that \linebreak<math>|J'-J| \leq l \leq |J'+J|</math>, while conservation of angular momentum requires <math>M = M' + m</math>.
Since the operators <math>er</math> and <math>\mu_B B</math> responsible for <math>E1</math> and <math>M1</math> transitions are both vectors, i.e. tensors of rank <math>l=1</math>, these transitions are both governed by the dipole selection rules
:<math>\begin{align} 
|\Delta J| &= 0, 1;\\
|\Delta m| &= 0, 1.
\end{align}</math>
Since <math>\bf r</math> is a polar vector and <math>\bf L</math> is an axial vector, <math>E1</math> transitions are allowed only between states of opposite parity and <math>M</math> transitions are allowed only between states of the same parity.
The operator responsible for <math>E2</math> transitions is a spherical tensor of rank 2.  For example,
:<math>
xz = (T_{2,-1}-T_{2,1})/4.
</math>

In general, then, we expect that the quadrupole moment can be expressed in terms of <math>T_{2, M} ({\bf r})</math>.  Thus, electric quadrupole transitions are allowed only between states connected by tensors <math>T_{2,m}(r)</math>, requiring:
:<math>\begin{align} 
|\Delta J| & = 0, 1, 2; \\
|\Delta m| &= 0, 1, 2.
\end{align}</math>

and parity unchanged.

In addition, <math>J=0\rightarrow J'=0</math> transitions are forbidden in all of the cases
considered above, since <math>J=J'=0</math> requires <math>\Delta L=0</math> (for any interaction that
does not couple to spin) whereas absorption or emission of a photon implies
<math>|\Delta L|=1</math>.

We now illustrate the use of the spherical tensor for the case of a vector.  
The dipole matrix element for a particular polarization of the field, <math>\hat{\bf {e}}</math>, is 

{{EqL
|math=<math>\begin{align} \  {\bf \hat{e}} \cdot {\bf r}_{ba} = {\bf \hat{e}} \cdot \langle b, J_ b, m_ b | {\bf r} | a, J_ a , m_ a \rangle . \end{align}</math>
|num=EQ_ select1
}}

It is straightforward to calculate <math>x_{ba}, y_{ba}, z_{ba},</math> but a more general approach is to write '''r''' in terms of a spherical tensor. This yields the selection rules directly, and allows the matrix element to be calculated for various geometries using the Wigner-Eckart theorem as discussed above.

The orbital angular momentum operator of a system with total angular momentum <math>L</math> can be written in terms of a spherical harmonic <math>Y_{L,M}</math>. Consequently, the spherical harmonics constitute spherical tensor operators. A vector can be written in terms of spherical harmonics of rank 1. This permits the vector operator '''r''' to be expressed in terms of the spherical tensor <math>T_{1,M}({\bf r}).</math> 

The spherical harmonics of rank 1 are 

{{EqL
|math=<math>\begin{align} \  Y_{1,0} = \sqrt {\frac{3}{4\pi }} \cos \theta ; \qquad Y_{1, +1} = - \sqrt {\frac{3}{8\pi }} \sin \theta e^{+i\phi }\qquad Y_{1,-1} = \sqrt {\frac{3}{8\pi }} \sin \theta e^{-i\phi } \end{align}</math>
|num=EQ_ select2
}}

These are normalized so that 

{{EqL
|math=<math>\begin{align} \  \int Y_{1,m^\prime }^* Y_{1,m} \sin \theta d\theta d\phi = \delta _{m^\prime , m} \end{align}</math>
|num=EQ_ select3
}}

We can write the vector '''r''' in terms of components <math>r_ m ,\  m = +1, 0, -1</math>, 

{{EqL
|math=<math>\begin{align} \  r_0 = r\sqrt {\frac{4\pi }{3}} Y_{1,0} ,\qquad r_{\pm } = r\sqrt {\frac{4\pi }{3}} Y_{1,\pm 1} , \end{align}</math>
|num=EQ_ select4
}}

or, more generally 

{{EqL
|math=<math>\begin{align} \  r_ M = rT_{1,M} (\theta , \phi ) \end{align}</math>
|num=EQ_ select5
}}

Consequently, 

{{EqL
|math=<math>\begin{align} \  \langle b, J_ b, m_ b | r_ M | a, J_ a, m_ a \rangle = \langle b, J_ b, m_ b | rT_{1,M} | a, J_ a, m_ a \rangle \end{align}</math>
|num=EQ_ select6
}}

{{EqL
|math=<math>\begin{align} \  = \langle b, J_ b | r | a, J_ a \rangle \langle J_ b, m_ b |  T_{1,M} | J_ a, m_ a \rangle \end{align}</math>
|num=EQ_ select7
}}

The first factor is independent of <math>m</math>. It is 

{{EqL
|math=<math>\begin{align} \  r_{ba} = \int _0^{\infty } R_{b,J_ b}^* (r) r R_{a,J_ a} (r) r^2 dr \end{align}</math>
|num=EQ_ select8
}}

where <math>r_{ba}</math> contains the radial part of the matrix element. It vanishes unless <math>| b \rangle </math> and <math>| a \rangle </math> have opposite parity. The second factor in Eq. [[{{SUBPAGENAME}}#EQ_select7|EQ_select7]] yields the selection rule 

{{EqL
|math=<math>\begin{align} \  | J_ b - J_ a | = 0, 1; ~ ~ ~ m_ b = m_ a \pm M = m_ a, m_ a \pm 1 \end{align}</math>
|num=EQ_ select9
}}

Similarly, for magnetic dipole transition, Eq. [[{{SUBPAGENAME}}#EQ_hor6|EQ_hor6]], we have 

{{EqL
|math=<math>\begin{align} \  H_{ba} (M1) = \mu _ B B \langle b, J_ b, m_ b , | T_{LM} (L) | a, J_ a , m_ a \rangle \end{align}</math>
|num=EQ_ select10
}}

It immediately follows that parity is unchanged, and that 

{{EqL
|math=<math>\begin{align} \  | \Delta J | = 0,1 ~ ~ ~ (J=0\rightarrow J= 0~ \mbox{forbidden}); ~ ~ | \Delta m | = 0,1 \end{align}</math>
|num=EQ_ select11
}}

This discussion of matrix elements, selection rules, and radiative processes barely skims the subject. For an authoritative treatment, the books by Shore and Manzel, and Sobelman are recommended.

== References ==

<thebibliography>
<attributes>
<widelabel>99</widelabel>
</attributes>
<bibitem>
<attributes>
<key>JAC63</key>
<label>None</label>
</attributes>
E.T. Jaynes and F.W. Cummings, Proc. IEEE, '''51''', 89 (1963). 


</bibitem><bibitem>
<attributes>
<key>EIN17</key>
<label>None</label>
</attributes>
A. Einstein, Z. Phys. '''18''', 121 (1917), reprinted in English by D. ter Haar, <it>
The Old Quantum Theory
</it>, Pergammon, Oxford. 


</bibitem>
</thebibliography>

<bibitem>

</bibitem>[EIN17a] A. Einstein, Z. Phys. '''18''', 121 (1917), translated in ''Sources of Quantum Mechanics'', B. L. Van der Waerden, Cover Publication, Inc., New York, 1967. This book is a gold mine for anyone interested in the development of quantum mechanics. 




\begin{thebibliography}{99}

\bibitem{JAC63} E.T. Jaynes and F.W. Cummings, Proc.
IEEE, 51, 89 (1963).

\bibitem{EIN17} A. Einstein, Z. Phys. 18, 121 (1917), reprinted
in English by D.\ ter Haar, {\it The Old Quantum Theory}, Pergammon, Oxford.

\end{thebibliography}

[[Category:8.421]]