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PROFESSOR: Are we ready?
So good afternoon.
Just a reminder, this week we see each other three times--
today on Wednesday and Friday in this other lecture
hall for our mid-term exam.
Today we will finish the big chapter
on light-atom interaction.
But we're not getting rid of it, because we
will be transitioning to an important aspect
of light-atom interaction.
And these are line shifts and line broadening.
So today we start the next big chapter-- line shifts and line
broadening.
But before I do that, we have to finish light-atom interaction.
And I want to come back to the rotating wave
approximation revisited.
So I'll revisit the revisit of the rotating wave
approximation.
And sometimes when I have discussions
with students after class, I realize
that something which I sort of casually mentioned
is either confusing or interesting for you.
And there are two aspects I actually
want to come back here.
So several people reacted to that,
but some felt it was maybe a little bit too complicated.
Or others asked me about some details.
So let me come back to two aspects.
And I hope you find them interesting.
One is when we sorted out all those terms,
those [? need two ?] angular momentum selection rules.
But I made sort of the innocent comment-- well,
if you have omega minus omega in a time-dependent Hamiltonian,
one term is responsible for absorption,
one is for emission.
And when more than one person asked me about it,
I think many more than one person in class
would like to know more about it.
So therefore, let me spend the first few minutes in explaining
why is a time-dependent term in the Hamiltonian
with plus or minus omega, why is one of them
responsible for absorption, and one
is responsible for emission?
Well, we have Schrodinger's equation,
which says that the change of the amplitude in state one
has a term.
And if it started out with population in state two--
let's say perturbation theory, we start in state two--
then it is the only term where the differential equation,
through an off-diagonal matrix element
puts amplitude from state two into state one.
So what I'm writing down here is just Schrodinger's equation.
And the operator V is the drive field
connecting state two to state one.
And so if I just integrate this equation
for a short time between time t and t plus delta t,
and I'm asking, did we change the population
of state one, which is now our final state?
Well, then you integrate over that for time interval delta t.
But now comes the point that the initial state has,
in its time-dependent wave function,
a vector which is e to the minus i omega 2 t.
The final state, which I called one,
has-- because it's a complex conjugate-- plus omega 1 t.
And let's just assume we have here
the proportionality to e to the i omega t.
And let me just say omega can now be positive and negative.
It will be part of the answer whether it
should be positive or negative.
Well, this integral here becomes an integral of e to the i,
omega 1 minus omega 2 plus omega t integrated with time.
And this is an oscillating function,
where if you integrated with over time,
it will average to zero unless omega
is equal or at least close to the frequency
difference between initial and excited state.
So actually, what you encounter here
is-- well, what I've derived for you here is actually,
you can say energy conservation.
I didn't assume it.
It is built into the time evolution of the Schrodinger
equation, that you can only go from state one
to state two or state two to one if the drive term has a Fourier
component omega, which makes up for the difference.
Or I'm using different language now.
If, through the drive term, you provide photons,
you provide quanta of energy, where omega fulfills
the equation for energy conservation.
And you also see from this result, when omega 1 is higher
than omega 2, omega has to be negative.
When the reverse is true, omega has to be positive.
So that's why I said, the e to the plus
i omega t term is responsible for absorption.
The e to the minus i omega t term
is responsible for stimulated emission.
You also see, of course-- but I stop here,
because I think you've heard it often enough.
If you integrate over short time delta t,
this equation has to be fulfilled
only to within 1 over delta t.
This is sort of the energy-time uncertainty.
For short times, the photon energy
does not need to match exactly the energy difference.
And you also realize when we think
about omega is close to resonance,
then e to the i omega t does absorption.
But if you're in the ground state,
e to the minus i omega t, leads now
to a very rapid oscillation here,
which is close to [? 2 ?] omega oscillation.
And we've discussed that in the context of the AC stark shift,
that this gives rise to the [? proxy ?] shift.
We've also discussed that this term is rapidly oscillating
and it's nothing else than the counter-rotating term which
we usually neglect when we do the rotating wave
approximation.
So everything we've discussed in this context--
counter-rotating term, energy conservation, Heisenberg's
uncertainty, time-energy uncertainty
actually comes from this kind of formalism.
Any question?
Of course, if you quantize the electromagnetic field,
then you don't have a drive term with e to the i omega t.
You just have a and a [? degas ?] for the photons.
And the question, which term absorbs a photon
or creates a photon, does not exist.
Because you know it whether it's a or a [? dega. ?] But
you have the two choices, whether you
want to use a fully quantized field with photon operators
or whether you want to use the time-dependent formalism,
using a semi-classical or classical field
in the Schrodinger equation.
The second comment I wanted to do
is using the semi-classical picture,
I was sort of going with you through some examples when
the rotating wave approximation is necessary, when not.
When do you have counter-rotating terms.
And yes, everything I told you is, I think,
is the best possible way how you can-- I assume,
because I haven't found a better one-- the best possible way
to present it and explain it to using
the time-dependent electromagnetic field.
But I realized after class that it
may be useful to quickly state what
I have said in using the photon picture.
If we have circular polarization,
we have, for given frequency, annihilation and creation
operator.
But let's assume that the mode we are considering
is right-handed circularly polarized,
so the operator creates a photon at frequency omega
with this right-handed circular polarization.
So that means now if we start from a level m
and we have now light-atom interaction,
the operator which annihilates a photon
with circular polarization because of angular momentum
conservation can only take us to a level
where the magnetic quantum number is n plus 1.
Well, the operator A [? dega ?] creates a photon
through stimulated emission.
And so this is now our two-level system.
And now we should ask the question, in terms of rotating
wave approximation, is necessary or not,
are there counter-rotating terms?
Well, the counter-rotating terms are the non-intuitive terms,
where you start out in the lowest state.
But now instead of absorbing a photon, you emit a photon.
And the operator for emission is this one.
So I can now ask, is there another term?
Why don't we stick to the blue color for the photons?
That there is a term which is driven by the operator
A [? dega ?] circularly polarized.
Well, the answer is, there may be such a term,
but the state we need has now a magnetic quantum
number of m minus 1 because of angular momentum selection
rules.
So this here is the counter-rotating term,
which you may or may not neglect, depending whether you
want to make the rotating wave approximation or not.
So therefore, if you got a little bit confused
about the different cases I considered
at the end of the last lecture, then
you may just summarize the many examples I gave you
in the lecture just as a note which
you should keep in the back of your head,
namely-- let me first phrase it in words
and then write it down.
If you have circular polarization and angular
momentum selection rules, then the counter-rotating term
may require a third level and is not part of two-level physics.
So if you have a situation where the third level does not exist,
you do not have a counter-rotating term.
However, in all situations I've encountered in the lab,
this third level does exist.
OK.
So let me just write that down-- counter-rotating term
for circularly polarized radiation
requires a third level which may not exist.
And then you don't have this term.
But it does exist in most cases.
Anyway, just an additional clarification for the topics
we had on Wednesday.
Any questions about that?
Yes.
STUDENT: Are there cases other than a spin-1/2 system where it
doesn't exist?
PROFESSOR: Well, I mentioned the example last class--
if you do spectroscopy of an S2P transition
in the magnetic field of a neutron star.
Then the same one splitting is so huge
that, well, you can assume that this has been shifted so far
away that it has been completely suppressed.
Other than that, well, we have the trivial situation
which we discussed in NMR.
If you simply have spin one half,
then the total number of levels is only two,
because we're talking about spin up and spin down.
Or I constructed, in the last class,
the forbidden transition, a doublet S to doublet S state.
So that's two pairs of S equals one half.
And then we are missing this state
to couple any counter-rotating term into the system.
OK.
The next subject is saturation.
Now, in this chapter, I want to talk
about saturation in general.
I want to discuss monochromatic light but also broadband light.
And I want to introduce concepts of saturation intensity
of absorption cross section, certain things which
I find extremely useful if I want to understand what happens
when light interacts with a system.
Just sort of to whet your appetite,
I will sort of show you that the absorption cross
section of a two-level system is independent
whether you have a strong or weak transition.
Some people think the cross section should be--
but there is a difference which is
important between monochromatic and broadband light.
But in the end, the concepts are very simple.
I should say, sometimes I feel it's almost too
simple to present it in class.
On the other hand, if I don't present it,
I can't make a few comments and guide you through.
So my conclusion now is, at least
for now, I show you some prepared slides,
and I sort of step you through, and make a few annotations,
and point out certain things.
We have already partially transitioned
to teach you this material through homework assignment.
This week's homework assignment, which is due on Wednesday,
is almost completely on saturation.
And I will make a few comments where what I present you today
is an extension or different from what you're learning
in the homework and vice versa.
Yes.
If I wanted to present you saturation,
power broadening, and all that in the purest form,
I would just preset you with the Optical Bloch equations.
We can solve them.
And then we have everything we want-- a result which
explains saturation and a result which
explains power broadening.
And you do some of it in your homework.
However, what I want to show here
is that saturation is actually a general feature
of a two-level system if you have sort of three rates, which
I will explain to you in a moment-- very similar
to Einstein's A and B coefficient--
that all such systems have saturation.
And then you may immediately solve the Optical Bloch
creation for monochromatic radiation.
But for broadband radiation, we usually
don't use the Optical Bloch equations,
because for infinitely broad light,
there is no coherence for which we
need Optical Bloch equations.
If you only have the Optical Bloch equations,
you have solved for saturation in one limiting case,
and you don't see that the concept of saturation
is much broader.
So therefore, let us assume that we have a two-level system.
And we have the couple two levels
with a rate-- which you can think
of the rate of absorption, the rate of stimulated emission.
And I call the rate the unsaturated rate.
In addition, there is some dissipation,
some spontaneous decay described by gamma.
So Ru is the unsaturated rate for absorption
and for stimulated emission.
Of course, you know even before you solve those equations
that there must be some saturation built in.
If you would look at the fraction of atoms
in the excited state and you change the laser power,
which means changing the unsaturated rate,
things cannot shoot up forever, because you cannot put more
than 100% of the population into the excited state.
However, the effect that when we increase the laser power,
we do upwards absorption and downward stimulation--
means you won't even get 100%.
The maximum you can get is 50%.
And what I'm just drawing for you is
this is a phenomenon of saturation,
and now we want to understand the details.
So using this rate equation, we are
defining-- this is now a definition-- the saturated rate
is the net transfer from A to B.
Because we have an absorption and stimulated emission,
the net transfer is the [? unsaturated ?] rate
times the population difference.
And this is our saturated rate.
But of course, we normalize everything for atom.
So therefore, our saturated rate has a rate coefficient S
times the total number of atoms, or the total population
in both states.
Eventually, we are interested in steady state.
We can immediately solve the rate equation
in terms of steady state, which is done there.
And we find that for those, we can now
eliminate one of the states from the equation,
because we have the steady state ratio.
And then we find that the saturated rate
is gamma over 2 times an expression which
involves a saturation parameter.
So in other words, it's just almost trivial solutions
of very simple equations, which describe the saturation
phenomenon I outlined for you at the beginning.
This solution has the two limiting cases
which we want to see-- that at a very low unsaturated rate,
the saturated rate is the unsaturated rate because there
is no saturation.
And secondly, if we would go to infinite power,
the saturated rate becomes gamma over 2,
because we have equalized the population between ground
and excited state.
One half of the atoms are in the excited state,
and they dissipate or scatter light with the rate gamma.
All right.
Any questions?
We now want to specialize it to a situation which we often
encounter, namely monochromatic radiation.
And for monochromatic radiation, the unsaturated rate
follows-- well, I factored out something here.
But it follows the normalized line shape,
which is a Lorentzian.
And therefore, our unsaturated rate
is proportion to the laser power.
But I usually like to express the laser power through a Rabi
frequency or the Rabi frequency squared.
So our unsaturated rate follows this Lorentzian.
And on resonance, this part is one.
Our rate is omega Rabi squared over comma.
And the definition for the saturation parameter of one,
or for the saturation intensity is that the unsaturated rate
has to be gamma over 2.
So therefore, by omega Rabi squared
over gamma is the unsaturated rate,
it should be gamma over 2 for saturation,
for saturation parameter of one.
So therefore, our saturation pentameter resonance
is given by this expression.
And if you use the previous result
and apply it to this unsaturated rate,
we find a saturated rate which shows now
the new phenomenon of power broadening.
Let me illustrate it in two ways.
The saturated rate involves a saturation parameter,
and the unsaturated rate is a Lorentzian.
But this Lorentzian appears now in the numerator
and the denominator.
So it appears twice.
But with a one-step manipulation,
you can transform it into a single Lorentzian.
But this single Lorentzian is now power-broadened.
It no longer has [? width ?] of gamma
over-- of the natural line with gamma.
It has an additional term, and this is power broadening.
STUDENT: [INAUDIBLE]?
PROFESSOR: No.
It's still-- the resonance is at [? 0 ?] [INAUDIBLE].
The equations are trivial.
It's really just substituting one
and getting from an expression, simplifying it
to simple Lorentzian.
I just want to emphasize the result.
If you drive a transition, we have
now-- the [? width ?] of the Lorentzian is now gamma over 2
if we have no saturation.
But then if we crank up the saturation parameter,
the [? width ?] increases with a square root of the power.
That's an important result.
The square root of the power leads to broadening.
Now let me give you a pictorial description
of what we have done here.
If we start with the Lorentzian and we increase the power,
you sort of want to drive the system with the stronger
Lorentzian.
But we know we have a ceiling, which is saturation.
And of course, when you drive it stronger,
you reach the ceiling on resonance
earlier than you reach the ceiling when you transfer it
away from resonance.
So therefore, if you start with the red curve,
crank up the power, you will get more
of a factor, more of a result in the wings
because you are not yet saturated there.
And this graphical construction, which I have just sort of
indicated to you, lead now to a curve which is broadened,
broader than the original Lorentzian.
And this is the reason behind power broadening.
I want to mention one thing here.
For the classroom discussion, I have
assumed that the light-atom interaction can be described
by Fermi's golden rule, which we know is a limitation.
When the system is, in effect, incoherent
or no longer coherent, we had a long discussion
about Rabi oscillation, Fermi's golden rule
in the last two weeks.
But what I'm doing is mathematically correct.
The Optical Bloch equation, which
you'll use in your homework assignment,
will include the transition from Rabi oscillation
towards Fermi's golden rule.
And I'm just considering this [? fundamental ?] case.
OK.
I've talked about saturation of a transition.
I've mentioned that we have defined the saturation
parameter such that when we have saturation parameter of one,
we sort of get into the non-linear regime
where saturation happens.
And of course, for an experimentalist,
the next question is, at what intensity does that happen?
This is summarized in those equations.
It's as simple as possible algebra.
You just combine two equations.
I don't want to do it here.
And we have a result for the saturation intensity, which
has two features, which I want to point out.
One is [? its case ?] with omega cube.
So the higher the frequency of your transition is,
the harder it is to saturate.
Of course, it has something to do with that in saturation,
you have an unsaturated rate, which
is one half of the spontaneous emission rate.
And you remember that the spontaneous emission rate
was proportional to omega cube.
So that's why we have, again, the omega cube factor.
And in addition, the larger-- actually, it depends.
Sorry.
I made a mistake.
Well, you can write the results in several ways.
If you have an intensity and you go back to photons,
you get factors of omega.
So when I said omega cubed comes from the natural line widths,
yes, it does, but it's not the only omega factor.
You can write the result actually
that you have a gamma squared dependence,
because one gamma comes from the matrix element squared
and one comes because you need to compete in your excitation
with spontaneous emission.
So anyway, this is sort of the result.
And you can calculate it for your favorite atom.
And for alkaline atoms, we usually find
that the saturation intensity is a few milliwatt
per square centimeter
Well, we can now repeat some of this exercise
for the broadband case.
In the broadband case, the unsaturated rate,
which is the rate for absorption in stimulated emission,
following Einstein's treatment of the AB coefficient
is used by using Einstein's B coefficient
times the spectral intensity.
And now we want the same situation as before.
We want to reach saturation.
And saturation happens when this is comparable with gamma.
And it's purely a definition that we
say it should be gamma over 2.
But we are consistent with what we did before.
And if you just take this equation
and calculate what the saturation intensity is,
well, gamma is nothing else than the Einstein A coefficient.
Here we have the Einstein B coefficient.
And if we take the ratio between the Einstein A and B
coefficient, the matrix element, everything
which is specific to the atom, cancels out.
And the saturation intensity, or the spectral density--
it's the spectral density now for broadband--
only depends on speed of light and the transition frequency
cube.
And it doesn't make a difference whether you
have a two-level system which has a strong matrix element
or weak matrix element.
I could explain it to you now at this point,
but we want to hold the idea that there
is a difference between single mode
monochromatic and broadband excitation
until I have discussed one more concept.
And this is the cross section.
Just to check, are there any questions?
Yes, Nancy.
AUDIENCE: So in the broadband case,
the line shift doesn't matter at all?
Because in the monochromatic case,
we had a line shift [INAUDIBLE].
Well, hold your question.
The line shape matters.
I will now discuss what is the line shape of the atom.
And the quick answer is, if the atom has a line shape,
we have to take the atomic line shape
and do a convolution with the line of the radiation.
And we have the two situations where in one case,
the monochromatic light is narrower
than the line shape of the atoms.
In the other case, it's broader.
And this difference, in the end, will
be responsible for the effect that the line widths
of the atom, which is the natural line widths,
will cancel out in one case and not in the other.
But that's actually the result of the next five minutes.
Other questions?
I know this topic can get confusing,
because we go from one definition to the next.
So let me just summarize.
What I've said so far is we [? derive ?] an atom.
We have absorption, we have stimulated emission.
And we want to understand the phenomenon of saturation.
And based on the effect how we define saturation, namely
that the unsaturated rate is gamma over 2,
we got some nice results for the saturation intensity
and for power broadening of a Lorentzian.
So it's pretty much having a definition and running with it.
And now we want to express the same physics
by using the concept of a cross section
for the following reason.
You can do physics, you can do atomic physics
without ever thinking about a cross section.
You can just say, I have a laser beam of a certain intensity,
and I scatter light.
But often, when we scatter something--
and you may be familiar, from atomic collisions--
you often want to write the scattering rate
as a density times cross section times relative velocity.
And this sort of has this intuitive feeling.
If you have a stream of particles in your accelerator
or a stream of photons in your laser beam,
you can now hold onto the picture
that each atom in your target is a little disk.
If the particle of photons hits the disk, something happens.
If it misses the disk, nothing happens.
And the area of the disk is this cross section.
So in other words, we want to now understand
how big is the disk of the atom which will, so to speak,
cast the shadow, which is synonymous with absorption,
when we illuminate those atoms with laser light.
So for me, a very intuitive quantity.
Anyway, so all we do is we have already
discussed the rate of excitation,
which is now the unsaturated rate.
But now we express the unsaturated rate
by the density of photons times the cross section.
And the relative velocity is the speed of light.
And from this equation, we find-- because everything
is known, we have talked about that on the last few pages--
we find that the cross section is-- and this is the result.
6 pi lambda bar square.
Lambda bar is the wavelengths of light divided by 2 pi.
So we find that for monochromatic radiation,
the cross sectional of a two-level system
is independent of the strength of the transition,
independent of the matrix element.
It just depends on the resonant wavelengths.
Now you would say, well, but what is now
the difference between a strong and a weak transition?
And this is shown here.
If you take your monochromatic laser and you scan it,
you scan it through the cross section.
When you are on resonance, you have 6 pi lambda bar square.
And the difference between a narrow transition
with a small Einstein A coefficient
and a strong transition with a large Einstein A coefficient
simply means that in one case, it's narrower.
In the other case, it's wider.
We talked about the phenomenon of saturation.
6 pi lambda bar squared is the cross section
in the perturbative limit, or the unsaturated cross section.
Of course, if you increase the laser power,
you saturation the transition.
The atom will have a smaller and smaller cross section.
Actually, that's something important you should consider.
When you have an atom and you increase the laser power,
you scatter light.
And the scattered light, or the absorbed light, saturates.
But with the cross section, we want
to know what fraction of the laser light is scattered.
And the fraction of the laser light scattered
goes to zero, because you make your laser
light stronger and stronger.
And the total amount of laser light which is scattered
saturates.
So in other words, you have a saturation
of the scattered light.
You have a saturation of the net transfer of atoms
through the excited state in the limit of infinite laser power.
But since the cross section is sort of normalized by the laser
power, the cross section has this dependence, 1 over 1
plus saturation parameter, and goes to 0.
And that means-- and this is sort
of the language we use-- that the transition bleaches out.
If you saturation the transition,
the cross section becomes smaller.
So when you saturation the transition in an absorption
imaging experiment, which many of you do,
the shadow is less and less black
exactly because the cross section is bleaching out.
But the amount of light you would scatter
you would observe in fluorescence
is not getting less, it saturates.
This is sort of just the two flip sides of the coin.
If anybody is confused, please ask a question.
OK.
So now in this picture, we can immediately
understand why we have differences
between monochromatic radiation and broadband radiation.
If you want to saturation a transition
with monochromatic radiation, we have our narrow laser.
We absorb with a cross section 6 pi lambda bar square.
And we have to increase the intensity of the laser
until the excitation rate equals gamma over 2.
That's our definition for saturation.
So therefore, the laser intensity
is proportional to gamma, because we
have the cross section is constant,
but the product of cross section and laser intensity
has to be equal to gamma over 2.
However, now consider the case that you
use broadband radiation.
The spectrum is completely broad.
Now, if an atom has a stronger transition,
its cross section is wider, and the atom
can sort of absorb a wider part of the incident spectrum.
So therefore, if the atom has a stronger transition,
it automatically takes, absorbs more of your spectral profile.
And therefore, the result for the saturation
and for the spectral saturation intensity
is independent of the matrix element
and the strengths of the transition.
In general, if you're not in either
of the extreme cases of monochromatic light
or broadband light, what you have to do
is you have to use this cross section
as a function of frequency, and convolve it
to a convolution with a spectrum of the incident light.
And this is exactly done here.
You take your frequency-dependent cross
section.
You do the convolution with the spectrum of the incident light.
And if you assume the incident light is spectrally very broad,
you simply integrate over the Lorentzian line shape
of the cross section.
And then you find exactly the same result
as we had two slides ago, that the saturation intensity
is independent of the strengths of the transition.
OK.
Can you think of a very intuitive argument
why for spectrally broad radiation,
all the properties of the atoms cancel out?
If you think about one physical example for, let's say,
black body radiation-- this is spectrally broad.
So you have an atom in a black body cavity.
And the atom experiences a very broad spectrum.
For what number of photons, black body photons per mode
would we find saturation?
Think about it.
It's a simple criterion you can formulate for black body
radiation to saturation your transition in terms
of the number of photons per mode.
You crank up the temperature in your cavity.
How high do you have to go with the temperature
in order to saturate an atom which is inside your black body
cavity?
AUDIENCE: One photon.
PROFESSOR: Pretty close.
AUDIENCE: 1 over [? degenerates. ?]
PROFESSOR: [? Degenerates. ?] OK.
No [? degenerates. ?] I hate [? degenerates. ?]
That's your private homework to put in [? degenerates ?]
afterwards.
The answer I came was n equals 1/2, I think.
I run the risk that I'm off by a factor of 2 now.
But the argument was that--
AUDIENCE: The rate equals [? degeneracy ?] by n by gamma.
So if the rate equals gamma over 1/2,
that mean that [? degenerates ?] by n equals 1/2.
And if [? degenerates ?] equals 1, n equals 1/2.
PROFESSOR: Yes.
OK.
So spontaneous emission, we know that spontaneous emission--
from our derivation of spontaneous emission--
corresponds to one photon per mode.
And our criterion now is that we want to have an absorption rate
or stimulated rate which is gamma over 2.
So we get sort of 1/2 the effect of spontaneous emission when
we have 1/2 a photon per mode.
So therefore, spontaneous emission absorption
is proportional to n.
And I think if n equals 1/2, then
we have the unsaturated rates equal to gamma over 2.
So this is a very physical argument.
When we put an atom into a black body cavity,
and we have 1/2 a photon per mode occupation number,
then we saturate any atom we put in.
Because using Einstein's argument, we have now the rate
coefficient for absorption emission
for stimulated emission and absorption is just 1/2
of the rate coefficient for spontaneous emission.
And that explains that all atomic properties
have to cancel out.
So now question for you.
We talked about the fact that if you have hyperfine transitions,
that it would take-- what was the value?
1,000 years for spontaneous emission?
So that we can completely neglect spontaneous emission.
On the other hand, we've just learned that saturation only
comes from spontaneous emission.
Without spontaneous emission, we wouldn't have saturation.
But now I'm telling you that any atom should really
be saturated if we put it in a black body cavity
where n bar is 1/2.
So what is the story now if we put an atom into a black body
cavity, and we are asking about, will we saturate?
The hyperfine transition.
Will we eventually have-- saturation
means we have [BLOWS AIR], 1/4 of the atoms in the excited
state, 3/4 in the ground state.
So the delta n has been reduced from 1, which it was initially,
to 3/4 minus 1/4, which is 1/2.
What will happen?
I mean, this was almost like a thermodynamic argument.
Will we equilibrate and saturate hyperfine transitions
in a black body cavity based on this argument
that for n bar equals 1/2, we should really
saturate everything?
AUDIENCE: Yes, but it's going to take a long time?
PROFESSOR: Yeah.
So for those conditions, if your black body cavity
was n bar equals 1/2, you should saturate any two-level system
completely independent what gamma is.
And if the gamma is 10 nanoseconds or 10,000 years,
you will saturate it.
The value of gamma has completely
dropped out of the argument.
But of course, if you want to reach any kind of equilibrium,
it will take a time scale, which is 1 over gamma.
And then we are back to 1,000 years.
Questions?
All right.
Then let's conclude this chapter and start our discussion
about line shifts and line broadening.
I have a problem with the tablet computer.
I draw a line, but the computer draws a line somewhere else.
So maybe I should just go back to this one and then copy
things over.
OK.
Our next big chapter is line shifts and broadening.
So the first question is motivational.
Why should we be interested in line broadening?
Well, the answer is almost trivial.
No resonance is infinitely narrow.
Whenever we want to interpret any result we obtain
spectroscopically, we are not observing a delta function,
we are not observing a resonance,
we are observing a line shape.
And unless we understand the line shape,
we may not accurately find the resonance frequency.
You could, of course, assume that your line shape is
symmetric, which may be the case but is not always the case.
So without understanding line broadening,
you cannot interpret spectroscopic information.
And eventually, as I mentioned in the first chapter
of this course, the art of analyzing line shapes
and finding the line center is very well advanced.
When we have caesium fountain clocks,
the accuracy how you operate the clock as a frequency standard
is on the order of one microhertz.
But those fountain clocks with you toss up
the atoms for one second in the atomic fountain,
they fall up and down, well, like a rock,
which takes about a second for a rock to go up and down a meter.
So therefore, the line width is on the order of one Hertz.
So therefore, people have to understand any single aspect
of the line shape at the level of 10 to the minus 5,
or 10 to the minus 6 to have this kind of accuracy.
OK.
So I thought I want to start this unit by collecting form
you examples for phenomena which cause broadening and shifting
of lines.
And well, my list has about 10 of them.
Let's see how many you get.
So what phenomena can lead to line shifts and line
broadening?
AUDIENCE: Phonons.
PROFESSOR: Phonons?
In terms of-- OK, AC stark effect.
Pardon?
AUDIENCE: Magnetic field noise.
PROFESSOR: Magnetic field noise.
OK.
I tried to-- yes, very good.
OK, yes.
Let me just try to group it a little bit
further, because I want to discuss it.
So we have external fields.
And external fields can have AC stark shifts.
If an external field is noisy, we have noise fluctuations.
All right.
Anything else?
AUDIENCE: Doppler shift.
PROFESSOR: Doppler shift.
Yes.
So we have the velocity of the atoms.
Doppler shift.
AUDIENCE: Collisions.
PROFESSOR: Collisions.
Very good.
Well, we just talked about one thing.
AUDIENCE: [INAUDIBLE].
PROFESSOR: Exactly.
When we have external fields, we can
have external fields like magnetic fields
or electric fields which cause shift and broadening.
And if there's noise, additional shifts.
But when we regard those fields as drive fields,
they can do power broadening.
Maybe by collisions, I should add the keyboard "pressure
broadening."
The higher the pressure in your gas cell is,
the more collisions you have and the more you have broadening.
Other suggestion?
If you don't have any of those effects,
do you measure delta function?
What's the line width?
Will?
STUDENT: [INAUDIBLE].
STUDENT: Spontaneous emission.
PROFESSOR: Spontaneous emission.
Yes.
And if you don't have spontaneous emission,
do we then measure delta function?
STUDENT: There's a Fourier limit.
PROFESSOR: The Fourier limit.
You can call it observation time,
or time of light broadening.
If an atom flies through your laser beam
and you can interrogate it only for a finite time,
you have a broadening due to the Fourier theorem.
And this can be called time of flight broadening and time of--
or interaction time broadening.
STUDENT: Rotations and vibrations?
PROFESSOR: Rotations and vibrations.
Not really.
These are more-- then the system has more energy levels,
and that's what you want to find out.
So maybe I'm more asking, how are those energy levels--
how do they appear spectroscopically?
Well, I think that's pretty complete.
Two external fields.
If you want, you can add gravity.
There is a gravitational red shift,
which is general relativity.
But anyway, let me look over that and try to categorize it.
What we had here actually all comes from a finite observation
time.
Either we do not have the atom long enough in our laser beam,
and that sets a limit.
Or if you are interested in an excited state and the excited
state decays, then the atoms themselves
have terminated our interrogation time.
The second class here, velocity, I
would summarize that we have motion of the atom.
It's a form of motional broadening.
We will actually discuss, when we discuss motion, also
the possibility of having atoms in a harmonic oscillator
potential, ions in an ion trap.
So these are now trapped particles.
This will actually often give rise to a splitting of the line
into side bends.
So we want to discuss that.
I've already mentioned external fields, conditional [INAUDIBLE]
interrogation, power broadening.
Some power broadening will actually
result into a splitting of line into [INAUDIBLE] triplet.
So power will not only broaden the line,
it can also split the line.
And we want to discuss that.
And finally, we have the effect of atomic interactions.
So for interactions, I think we should add something
like mean field shifts, which also goes sometimes
by the name of clock shift.
If you're not at zero density, your transition
can be shifted by the presence of other atoms.
Will?
STUDENT: Isn't collisional broadening or pressure
broadening sort of just an ensemble
average of a stark effect?
So that's sort of an external field?
PROFESSOR: That depends now.
Collisions is one of the richest phenomena on the list here.
You're ahead of me.
But in the next few minutes, I wanted to actually
see, well, maybe we should-- those categories are not
mutually exclusive, because one part of collisions is.
An atom is in the excited state, it collides,
it gets de-excited.
So then collisions have no other effect
than sort of give us a finite observation time,
where there is an effective lifetime, which is just
the time between two collisions.
So it can be this.
There's another aspect of collisions,
that every time there is a collision,
an atom feels the electric field of another atom.
And then we have some form of collisional broadening,
because we do some statistical averaging over stark effects,
over level shifts.
Now, there is a third aspect of collisions,
which is maybe surprising to many of you.
And this is actually-- I put it here under motion.
It is collisional narrowing, or [? diche ?] narrowing.
There's one limiting case when you have collisions,
that collisions lead to a narrower line and not only
to a broader line.
the reason is a little bit-- if you put an atom in a buffer gas
and it collides with all the buffer gas atom,
it cannot fly away.
So buffer gas and collisions can sort of
help to increase your observation time.
But only if the other effects of collisions are absent.
So anyway, I thought this is a number
of really interesting effects.
And you already see from my presentation and discussion
that it makes perfect sense to discuss them not one by one,
as they appear in other chapters,
but try to have comprehensive discussions of those.
Let me talk about one classification of those shifts
and broadening.
And one is the distinction between homogeneous
and inhomogeneous broadening.
So the picture here is that if you
have-- let me just give you the cartoon picture.
If you have different atoms, atom 1, atom 2, atom 3.
A homogeneous broadening situation
is if the line has been broadened
for each atom in the same way.
An inhomogeneous broadening situation
is that atom 1 has a line here, atom 2 has a line here,
atom 3 has a line there.
And if you look at the statistical ensemble,
you may find the same line widths
as on the left-hand side, but the situation and the mechanism
is a very different one.
So the different characteristics are that here, we
have a mechanism which broadens or widens
the line for each atom.
Whereas here, there is maybe not even any line
broadening for the atom.
It's more a random shift to individual atoms.
And the widening happens for the ensemble.
Another very important distinction
is in the left case, if you have one powerful laser,
it can talk to all the atoms.
Whereas in the right-hand side, you
may have a laser with a certain frequency,
and it may only excite one group of atoms in your ensemble.
So this is the opposite here.
In many situations do we have a physical picture where,
in homogeneous broadening, we can understand it
as random interruptions of the phase's evolution of the atom.
For instance, through spontaneous emission,
or you can see certain collisions-- just mean
the phase of the excited state is suddenly perturbed.
And therefore, the phase is randomized.
So if the physical picture is a random interruption
of the phase evolution, well, a random interruption
of a phase evolution means that there
is an exponential decay of coherence.
And the line shape, the Fourier transform
of an exponential decay is a Lorentzian.
Whereas the physical picture behind inhomogeneous broadening
is that you have random perturbations.
And if you have many random or small perturbations,
they often follow a normal distribution,
which is a Gaussian.
There's one other aspect of an inhomogeneous broadening.
If it's an inhomogeneous broadening,
it is as if the individual atom is not broadened,
the individual atom is actually sharp,
it has a longer coherence.
And you can-- there are techniques to make
that visible.
And one famous technique, for those of you
who have heard about it, are an echo technique.
So having explained to you in a general way
the difference between inhomogeneous and homogeneous
broadening, how would you classify the line broadening
mechanisms we have collected before?
Which one are inhomogeneous broadening?
STUDENT: Doppler broadening.
PROFESSOR: Doppler broadening.
We exploit that when we do saturation spectroscopy
in the lab, when we just talk to one component of the velocity
distribution.
What else?
STUDENT: [INAUDIBLE].
STUDENT: Collisions.
PROFESSOR: Collisions.
That's actually a good one.
Usually, collisions are classified
as homogeneous broadening, because the simplest
model for collisions is collisions
are sort of just hard-core collisions which just de-excite
the atom, completely change the coherent phase evolution.
And therefore, collisions would broaden the transition
for all atoms to a line widths which
is 1 over the collision rates.
However-- and this shows that the distinction cannot always
be made-- you can actually have collision rate which depends
on the velocity.
The faster atoms may have a smaller collision cross
section than the slower atoms.
And now you have an inhomogeneous aspect
of the collision rate.
And therefore, collision rate becomes inhomogeneous.
I mean, the standard example for inhomogeneous fields
would-- if you have an inhomogeneous magnetic field,
you have stationary atoms-- well, not in an atomic gas,
but maybe in [INAUDIBLE] or in a solid.
And you have an inhomogeneous magnetic field.
This is actually the standard case
of nuclear magnetic resonance, that each atom
possesses at its local magnetic field.
And the line shape is inhomogeneously broadened.
Colin?
STUDENT: [INAUDIBLE] clock shift sometimes,
in some circumstances.
PROFESSOR: If the density is constant,
you would actually say the mean field is
the same for all atoms in the ensemble.
But if you have a trapped atom sample
where the density drops at the edge,
you may actually have a sharper line,
and less broadening, or less shift at the edge of the cloud.
Anyway, so I think you have all the tools to classify it.
And you see from the discussion that sometimes it's
not so obvious.
Or you may have a mechanism which
has [? both ?] inhomogeneous that it does something
to all atoms.
So for instance, collisions broaden all the atoms,
but then different atoms are more broadened than others.
So there may be also an inhomogeneous aspect.
But finally, let me ask you the following.
It seems the first items on our list
had sort of a very natural explanation
in terms of the Fourier theorem, that, well, we only talk
to the atoms for a finite time.
Or the atoms decide not to talk to us for longer,
because they spontaneously decay.
Now, maybe you want to give me some arguments why
some of the other mechanisms are actually
also due to some form of finite time of interrogation.
Well, if I would say, can we regard collisions
as an effect of finite observation time?
Well, if I rephrase "observation time" to "finite coherence
time," that something interrupts the coherent evolution
of the wave function, I think we would
say the collision time sets a time limit to the coherence
time and therefore, should also be regarded
as due to the finite time, we can
drive the atom in a coherent fashion.
If I take power broadening, we just
discussed power broadening.
Well, what is the rate-- or 1 over the rate
of power broadening?
We just discussed that that's maybe
nice to take it out of the context.
We discussed before that power-broadened line widths
is gamma over 2 times S plus 1 square root of it--
the saturation parameter.
But when does power broadening happening?
And what is the real time scale for what is the physical--
STUDENT: Spontaneous emission.
PROFESSOR: Spontaneous-- so we had a criterion
that the unsaturated rate has to be comparable to gamma.
Let's forget about factors of 2 now.
But that means that the Rabi frequency
has to be comparable to gamma.
The Rabi frequency tells us a time of Rabi flopping.
So actually, power broadening can
be understood as a finite observation time broadening,
but the atom is leaving the excited state
not by spontaneous emission, but by stimulated emission.
So in other words, stimulated emission
interrupts our ability to observe the atoms
in the excited state.
And so again, we see that there is a process coming
in which interrupts our observation
time of the unperturbed atomic levels.
Well, let me go one step further.
Let me ask you, do you have any idea
how we could discuss the Doppler shift as
due to some finite time scale?
You would say, well, yeah, that's dimensional analysis.
If you have a broadening, a broadening is a frequency,
1 over the frequency is the time,
and there is a time scale associated
with Doppler broadening.
Sure.
But now my question is, what is the physical time
scale with Doppler broadening?
Yes?
STUDENT: [? Collisions. ?]
PROFESSOR: No.
We have an ideal gas without any collisions-- just
a [INAUDIBLE] distribution.
You're right.
In practice, yes.
But I try to create an idealized situation.
So what is the time scale of Doppler broadening?
You may have never heard the question.
But this is for me, what I want to really teach you
when I teach all these different line shifts
and line broadening.
There is a common denominator.
STUDENT: You could think of the atom [INAUDIBLE] emission.
And then you would have velocity [INAUDIBLE] emission.
PROFESSOR: You're talking about recoil shifts,
and the atom is changing its velocity due to recoil.
This would something in addition,
but it's not necessarily the case here.
I give you a physical argument.
If I make the atom heavier and heavier and heavier,
the effect of the recoil vanish.
But then I can heat up the heavier atom,
that it moves with the same velocity as the slow atom.
So there is an effect which you can associate just
to the velocity and to the velocity distribution.
And that's what I want to discuss now.
But there is another effect with the recoil.
But I can say the recoil is a finite mass
effect, for that purpose.
The mass is sort of my handle, whether the recoil
of a singular photon is important or not.
Yes?
STUDENT: [INAUDIBLE]?
PROFESSOR: Yes, but this is really
a more trivial finite observation time.
When you heat the wall of the chamber,
it's a collision with the chamber.
It means we have only a finite interaction size.
Now, let me sort of guide you to that.
The secret here is when we say, you
have a finite lifetime, a finite observation time,
what matters when we do spectroscopy
is the time we can observe the atoms coherently.
If the atoms de-phase, if the atoms get out
of coherence-- for instance, if you have collisions--
if collision de-excite the atom-- we'll
talk about it later-- it's like spontaneous emission.
But then there are collisions which
just create a phase hiccup, that the excited
state gets a random phase.
So an interruption of the phase, an interruption
of the coherent evolution is, in effect,
an interruption of us probing the atoms in a coherent way.
And then the Fourier transform just tells us, this time, or 1
over this time, is the line which we observe.
And you would say, but how does it
come into play with atoms with a velocity distribution?
In the following way.
If you line up several atoms and they interact with a laser
beam, some atoms are faster, some atoms are slower.
If some of the atoms have moved compared to the slower
atoms, one additional wavelength,
then your ensemble of atoms is no longer
interacting with the laser beam in a phase-coherent way.
Because of the different velocities,
they are now talking to random phases of the laser.
So therefore, Doppler broadening is
nothing else as a loss of the atoms
to coherently interact with a laser, because some of them
have moved an additional wavelength in the laser beam.
Well, if that is true-- but what happens if the laser beam is
like this, with the wavelengths, and the atoms go perpendicular?
What happens then?
STUDENT: There's no Doppler.
PROFESSOR: Then there is no Doppler effect.
So what I'm saying is fully consistent
with every single thing you know about the Doppler effect.
OK.
So I think there's not much more we can do today.
But let me give you the summary of this discussion.
To the best of my knowledge, all line broadening mechanisms
can be described by using the concept of coherence time.
And it's a coherence time of a correlation function.
It's pretty much the correlation function
of the phase which the atom experiences.
At t equals 0, it experiences one phase of your drive field.
And a later time, how long does it stay coherent
with the coherent evolution of the phase of your drive
field of a correlation function?
However, in the case of inhomogeneous
broadening-- and this is what I just
discussed with the different atoms
starting together and having different velocities.
In the case of inhomogeneous broadening,
I have to include in the description of the correlation
function ensemble averaging.
So this is our agenda.
On Wednesday, I will start to discuss with you
very simple cases.
I sort of like, before I introduce correlation function,
we have the generalized discussion
to summarize for you the phenomenological description
of just Rabi resonance, Ramsey resonance, exponential decay,
simple Doppler broadening, the recoil effect,
that you have a clear physical picture of what
the different phenomena are.
And then we describe them with a common language,
with a common formalism, which is
a formalism of correlation functions.
Any questions?
One obvious question-- the chapter
on line shifts and broadening will not be on the mid-term.
OK.
See you on Wednesday.