Introduction to Inverse Theory

GEO 5210 โ€“ Seismology I L14-1
Lecture 14 โ€“ Seismic Inversion Part I
1. A brief introduction to Inverse Theory
Inverse theory in seismology has many applications. Some of the most important are:
1) Earthquake location
2) Determining 1D velocity and density structure of the Earth
3) Seismic tomography โ€“ i.e., 3D velocity variations.
Many problems in the physical sciences can be written in the form of a linear equation:
Where we define:
A = model/data kernel. This provides the relationship between model parameters and data.
m = model vector. Contains the unknown model parameters.
d = data vector. Contains our observations.
Example: Straight line fitting
A simple example would be temperature measurements (Ti) made as a function of depth (zi) in the Earth.
Looking at these data we see what looks to be a linear increase of temperature with depth. So, letโ€™s try and describe our ith temperature measurement as follows:
That is, we want to find the equation of a straight line that best fits our observations. We can write this in matrix form:
GEO 5210 โ€“ Seismology I L14-2
Where our data vector (d) contains our temperature measurements (T1, T2, โ€ฆ, T5), our model vector (m) contains the unknowns (our slope โ€“ b and intercept โ€“ a), and the model kernel (A) shows the relationship we are assuming between our data and unknowns.
Just multiplying out the first term of our matrix above we can see that this represents the relationship we are looking for:
If the system above was evenly determined (i.e., we had the same number of equations and unknowns) then we could easily find the solution of ๐€๐€๐€๐€=๐๐ by just solving for m. That is:
๐ฆ =๐€๐€โˆ’1๐๐
We can see why this is called inverse theory, because to find our solutions (our model parameters) we have to find the inverse of the model kernel.
But, our example problem had 2 unknowns and 5 observations. This is often the case that we encounter, i.e., we usually have more observations than unknowns โ€“ this is referred to as an overdetermined system.
Overdetermined Systems
Recall that a matrix A is invertible if there exists a matrix B such that: AB = BA = I. Non-square matrices are not invertible. Hence, in our example above we have a 5 ร— 2 matrix, which is not square and not directly invertible.
Traditionally, what is done is to look for the solution that provides the best fit in the least squares sense. Consider the next image:
GEO 5210 โ€“ Seismology I L14-3
Here we show our observed temperature readings (red circles) and a possible line fit to these observations. The black cross shows the predicted (model) value for this line at each depth. What we calculate is the residual. Where we define the residual = observed value โ€“ model value.
The least-squares solution provides the best-fit where we define the best-fit as the line for which the sum of the squared residuals has its least value. That is, we seek to minimize:
Where ri is the ith residual.
We set up our equations as:
The solution by least squares can be determined from multiplying each side of the above equation by the transpose of A: ๐€๐€๐‘ก๐‘ก (see your linear algebra text for proof).
Now we solve for m:
โ‡’๐ฆ =(๐€๐€๐‘ก๐‘ก๐€๐€)โˆ’๐Ÿ๐Ÿ๐€๐€๐‘ก๐‘ก๐๐
Note that in our example A is a 5 ร— 2 matrix. So, At is a 2 ร— 5 matrix. So, multiplying ๐€๐€๐‘ก๐‘ก๐€๐€ we get a 2 ร— 2 matrix, which is square, and possibly invertible.
Underdetermined Systems
Underdetermined systems are also possible. That is, we have more unknowns than equations. If we try the least squares solution we find that ๐€๐€๐‘ก๐‘ก๐€๐€ is singular (i.e., it has no inverse). There are an infinite number of solutions. That is, if we try to fit a straight line to a single data point, any line will fit through that data point:
GEO 5210 โ€“ Seismology I L14-4
This is unfortunate because sometimes parts of problems we are trying to solve may be underdetermined.
The traditional approach to handling this is to look for the simplest solution. That is, we search for the model values that have the shortest length in the least squares sense. Specifically we seek to minimize:
In this case, the solution is:
๐ฆ =๐€๐€๐‘ก๐‘ก(๐€๐€๐€๐€๐‘ก๐‘ก)โˆ’1๐๐
To make this clear, letโ€™s take a look at an example. Suppose we have just one measurement:
T1 = 5ยฐ at z1 = 10 m.
So, we set up our matrix equation as:
Solving ๐ฆ =๐€๐€๐‘ก๐‘ก(๐€๐€๐€๐€๐‘ก๐‘ก)โˆ’1๐๐ we get:
GEO 5210 โ€“ Seismology I L14-5
โ‡’๐‘Ž๐‘Ž=5101=0.0495 (the intercept)
โ‡’๐‘๐‘=50101=0.495 (the slope)
And our solution length is:
So, we get a straight line passing through our point that looks like:
But is this solution really of any interest to us?
The problem in geophysics is that we often encounter cases where parts of our problem are over-determined and other parts are under-determined. So, typically we try to seek a compromise between minimizing the prediction error (the residuals) and the solution length.
Damped Least Squares
The damped least squares solution is:
๐ฆ =(๐€๐€๐‘ก๐‘ก๐€๐€+ฮป2๐ˆ๐ˆ)โˆ’1๐€๐€๐‘ก๐‘ก๐๐
Where ฮป is a damping factor.
We try to choose a value of ฮป that minimizes both the prediction error and solution length.
โ€ข If ฮป2 is large ๏ƒ  the emphasis is on minimizing the solution length.
GEO 5210 โ€“ Seismology I L14-6
The effect of a large damping factor is to produce a smooth model (i.e., we have a small model length) but not necessarily a great fit to the data.
โ€ข If ฮป2 is small ๏ƒ  the emphasis is on minimizing the residuals (prediction error).
The effect of a small damping factor is have very small residuals but a very rough model (and a very large solution length).
We typically try to find a balance between these two end-member cases. For example, we can try a range of values for ฮป and produce a trade-off curve as shown below. Here we try to find the optimal solution as a balance between model roughness and model misfit. Calculating model roughness can be done in a variety of ways, for example by looking at the 2nd derivative of the model values.
GEO 5210 โ€“ Seismology I L14-7
But, one must always be cautious of these solutions. The optimal model doesnโ€™t necessarily imply it is really the Earth we are looking at.
The figure below is an example of the effect of damping in a seismic tomography model. This is from the S-wave tomography model S20RTS by Jeroen Ritsema. It shows a cross-section through the Earth (cutting through the central Pacific LLSVP). Here we can see the effect that choosing a different damping parameter can have on the resulting model. On the left we have a heavily damped model which gives us a very smooth model. Whereas on the right we have less damping that results in a much rougher model and stronger perturbations in velocity.
2. Tau-P Inversion
Previously we noted that travel-time vs. distance or ray parameter vs. distance plots do not produce singularly valued functions. To get around this limitation we generate a new function called a Tau-p or ฯ„(p) curve.
GEO 5210 โ€“ Seismology I L14-8
Setting up the inverse problem:
Recall from a previous lecture that we defined Tau(p) as follows:
๐œ๐œ(๐‘๐‘)=2๔€ถฑ(๐‘ข๐‘ข2โˆ’๐‘๐‘2)12 ๐‘‘๐‘‘๐‘‘ ๐‘ง๐‘ง๐‘๐‘0
We can write this instead for a stack of discrete layers:
๐œ๐œ๔€ตซ๐‘๐‘๐‘—๐‘—๔€ตฏ=2๔€ท๔€ตซ๐‘ข๐‘ข๐‘–๐‘–2โˆ’๐‘๐‘๐‘—๐‘—2๔€ตฏ12๐‘›๐‘›๐‘–๐‘–=1โ„Ž๐‘–๐‘–; ๐‘ข๐‘ข๐‘–๐‘–>๐‘๐‘๐‘—๐‘—
That is, we have measured ฯ„ at a number of discrete ray parameters (p1, p2, p3, โ€ฆ, pm). And we decide to parameterize our Earth model as a series of n-layers, each with thickness h:
Letโ€™s think about this problem in the sense of straight-line fitting segments of our travel-time vs. distance curve:
GEO 5210 โ€“ Seismology I L14-9
That is, what if we approximate the real travel-time curve (blue), by a series of straight line segments (red segments). Each one of these segments has a ray parameter p, and letโ€™s assume that the slowness is u. This is strictly only true if we are looking at refracted arrivals (headwaves โ€“ see the aside at the end of this lecture), but is a good first approximation in any case, and is true in the limit that our straight line segment lengths go to zero.
Letโ€™s consider a few values of this equation.
๐œ๐œ๔€ตซ๐‘๐‘๐‘—๐‘—๔€ตฏ=2๔€ท๔€ตซ๐‘ข๐‘ข๐‘–๐‘–2โˆ’๐‘๐‘๐‘—๐‘—2๔€ตฏ12๐‘›๐‘›๐‘–๐‘–=1โ„Ž๐‘–๐‘–; ๐‘ข๐‘ข๐‘–๐‘–>๐‘๐‘๐‘—๐‘—
j = 1
Recall that in our setup we assume that u1 = p1, u2 = p2, etc. Hence our first term (๐‘ข๐‘ข12โˆ’๐‘๐‘12)=0. Since we have increasing velocity with depth, that means that u2 < u1. And u1 = p1, so that u2 < p1. Thus, our second term (๐‘ข๐‘ข22โˆ’๐‘๐‘12)12 is undefined (hence, the condition that ๐‘ข๐‘ข๐‘–๐‘–>๐‘๐‘๐‘—๐‘—).
So, ๐œ๐œ(๐‘๐‘1)=0. This makes sense since our first straight-line segment passes through the origin.
j = 2
The second term is zero here, so:
j = 3
Just considering the non-zero terms:
All terms
So, it should be obvious by now that we can write this in the form of a matrix:
GEO 5210 โ€“ Seismology I L14-10
Which is a matrix equation of the form:
Which can be inverted for the layer thicknesses (h).
3. 1D Seismic Velocity Models
The first 1-D models of Earthโ€™s seismic velocity structure were set up by Jeffreys and Bullen. Their 1940 JB model consisted of 7 layers labeled A through G as follows:
Deepest Depth (km)
Upper Mantle
Mantle Transition
Lower Mantle
Outer Core
Core Transition
Inner Core
The layer names A through G are no longer used. But, it is interesting to note that early on the lowermost part of the D layer was observed to be different, hence the D layer was split into the D’ and Dสบ layers. Dสบ is still used for the lowermost part of the mantle. Another interesting feature was the F-layer, or the Core transition zone. This was dropped in future models, but now researchers are putting forth further evidence that there is a transition region from the outer- to inner- core, and hence the F-layer is making a comeback.
More recent developments are:
1981 โ€“ PREM (Preliminary Reference Earth Model) โ€“ by Dziewonski and Anderson.
Note that these models typically invert for seismic velocities as polynomial functions in different bands of the Earth as opposed to a stack of layers as we discussed above.
GEO 5210 โ€“ Seismology I L14-11
PREM model.
1991 โ€“ IASP91 (International Association of Seismology and the Physics of the Earthโ€™s Interior) โ€“ by Kennett and Engdahl.
This model primarily improves the seismic velocities at the mantle transition zone.
1995 โ€“ AK135 โ€“ by Kennett, Engdahl, and Buland.
The main difference in model AK135 from IASP91 is in the velocities near the boundary of the inner core.
The next figure shows the difference between the JB40 model and the IASP91 model. As can be seen the variations arenโ€™t that dramatic.
GEO 5210 โ€“ Seismology I L14-12
From Stein & Wysession.
The Moon
The only other planetary body for which we have 1D seismic velocity profiles is the moon. Recall that we installed seismometers on the moon during the Apollo missions:
Apollo 12 Alsep (Apollo Lunar Surface Experiments Package)
GEO 5210 โ€“ Seismology I L14-13
Several competing models currently exist. But, one of the best models is by Nakamura 1983. Note that these models do not resolve structure down to the lunar core.
Model Nakamura 1983. Plot by Yao Yao (green โ€“ S-wave velocity; red โ€“ P-wave velocity)
4. Density Structure
Models like PREM also include density as a function of depth. How is this determined? The answer can be seen by looking at the Adams-Williamson equation.
Assume that the Earth is made of infinitesimally thin spherical shells with uniform properties.
We know at depth that pressure (P) is given by:
g = gravitational acceleration.
ฯ = density
h = depth
If we consider a change in pressure ฮ”P with increasing depth ฮ”h:
GEO 5210 โ€“ Seismology I L14-14
And, in the limit ฮ”โ„ŽโŸถ0
That is the change in pressure with increasing depth is +ฯg. Going the other way, with increasing radius:
โ‡’๐‘‘๐‘‘๐‘‘ ๐‘‘๐‘‘๐‘‘ =โˆ’๐‘” (๐‘Ÿ๐‘Ÿ)๐œŒ๐œŒ(๐‘Ÿ๐‘Ÿ)
That is, the pressure decreases with increasing radius.
We also know that the acceleration of gravity at radius r is (just equate Newtonโ€™s second law with Newtonโ€™s law of universal gravitation):
๐‘” (๐‘Ÿ๐‘Ÿ)=๐บ๐บ๐‘€๐‘€๐‘Ÿ๐‘Ÿ๐‘Ÿ๐‘Ÿ2
Mr = Mass within radius r.
โ‡’๐‘‘๐‘‘๐‘‘ ๐‘‘๐‘‘๐‘‘ =โˆ’๐บ๐บ๐‘€๐‘€๐‘Ÿ๐‘Ÿ๐‘Ÿ๐‘Ÿ2๐œŒ๐œŒ(๐‘Ÿ๐‘Ÿ)
From the chain rule:
๐‘‘๐‘‘๐‘‘ ๐‘‘๐‘‘๐‘‘ =๐‘‘๐‘‘๐‘‘ ๐‘‘๐‘‘๐‘‘ ๐‘‘๐‘‘๐‘‘ ๐‘‘๐‘‘๐‘‘
โ‡’๐‘‘๐‘‘๐‘‘ ๐‘‘๐‘‘๐‘‘ =โˆ’๐บ๐บ๐‘€๐‘€๐‘Ÿ๐‘Ÿ๐œŒ๐œŒ(๐‘Ÿ๐‘Ÿ)๐‘Ÿ๐‘Ÿ2๐‘‘๐‘‘๐‘‘ ๐‘‘๐‘‘๐‘‘ (Eqn 1)
Recall that bulk modulus (k) (or Incompressibility) is a materials ability to resist being compressed under a pressure equal in all directions.
Bulk modulus = k VVPโˆ’ฮ”ฮ”=,
Where P is the Pressure (Force/Area) applied to a volume of material given by V. Graphically, if we apply an equal Pressure (P) on all sidesโ€ฆ
GEO 5210 โ€“ Seismology I L14-15
Then the box deforms as followsโ€ฆ
Where the dashed lines show the volume of the original, uncompressed, box.
For small volumes:
๐‘˜๐‘˜=๐‘‘๐‘‘๐‘‘ ๐‘‘๐‘‘๐‘‘๐‘‘โˆ’๐‘‰ ๔€ต—; (๐ธ๐ธ๐ธ๐ธ๐ธ๐ธ 2)
Noting that we have a minus sign so that with increasing pressure we get a smaller volume.
Since we know that ๐œŒ๐œŒ=๐‘š๐‘š/๐‘‰ we can write:
๐‘‘๐‘‘๐‘‘ ๐‘‘๐‘‘๐‘‘๐‘‘=๐‘‘๐‘‘๐‘‘๐‘‘๐‘‘๐‘‘๔‰€๐‘š๐‘š๐‘‰ ๔‰
Carrying out the derivative:
โ‡’๐‘‘๐‘‘๐‘‘ ๐‘‘๐‘‘๐‘‘๐‘‘=โˆ’๐‘š๐‘š๐‘‰ 2
And substituting back in ๐œŒ๐œŒ=๐‘š๐‘š/๐‘‰ :
โ‡’๐‘‘๐‘‘๐‘‘ ๐‘‘๐‘‘๐‘‘๐‘‘=โˆ’๐œŒ๐œŒ๐‘‰
GEO 5210 โ€“ Seismology I L14-16
โ‡’๐‘‘๐‘‘๐‘‘๐‘‘๐‘‰ =โˆ’๐‘‘๐‘‘๐‘‘ ๐œŒ๐œŒ
Now, if we substitute this into Eqn 2:
โ‡’๐‘˜๐‘˜=๐‘‘๐‘‘๐‘‘ ๐‘‘๐‘‘๐‘‘๐‘‘โˆ’๐‘‰ ๔€ต—=๐‘‘๐‘‘๐‘‘ ๐‘‘๐‘‘๐‘‘ ๐œŒ๐œŒ=๐œŒ๐œŒ๐‘‘๐‘‘๐‘‘ ๐‘‘๐‘‘๐‘‘
โ‡’๐‘‘๐‘‘๐‘‘ ๐‘‘๐‘‘๐‘‘ =๐œŒ๐œŒ๐‘˜๐‘˜
And substituting this back into Eqn 1:
โ‡’๐‘‘๐‘‘๐‘‘ ๐‘‘๐‘‘๐‘‘ =โˆ’๐บ๐บ๐‘€๐‘€๐‘Ÿ๐‘Ÿ๐œŒ๐œŒ(๐‘Ÿ๐‘Ÿ)๐‘Ÿ๐‘Ÿ2๐‘‘๐‘‘๐‘‘ ๐‘‘๐‘‘๐‘‘ =โˆ’๐บ๐บ๐‘€๐‘€๐‘Ÿ๐‘Ÿ๐œŒ๐œŒ(๐‘Ÿ๐‘Ÿ)๐‘Ÿ๐‘Ÿ2 ๐œŒ๐œŒ(๐‘Ÿ๐‘Ÿ)๐‘˜๐‘˜
Now, if we recall our seismic wave speeds:
P-wave velocity = ๐›ผ๐›ผ=๔€ถจ๐‘˜๐‘˜+43๐œ‡๐œ‡๐œŒ๐œŒ
S-wave velocity = ๐›ฝ๐›ฝ=๔€ถง๐œ‡๐œ‡๐œŒ๐œŒ
And substituting back into our previous equation for the rate of change of density with respect to radius:
GEO 5210 โ€“ Seismology I L14-17
โ‡’๐‘‘๐‘‘๐‘‘ ๐‘‘๐‘‘๐‘‘ = โˆ’๐บ๐บ๐‘€๐‘€๐‘Ÿ๐‘Ÿ๐œŒ๐œŒ(๐‘Ÿ๐‘Ÿ)๐‘Ÿ๐‘Ÿ2 ๐œŒ๐œŒ(๐‘Ÿ๐‘Ÿ)๐‘˜๐‘˜=โˆ’๐บ๐บ๐‘€๐‘€๐‘Ÿ๐‘Ÿ๐œŒ๐œŒ(๐‘Ÿ๐‘Ÿ)๐‘Ÿ๐‘Ÿ21๐›ผ๐›ผ2โˆ’43๐›ฝ๐›ฝ2
If we let ๐œ‘๐œ‘=๐›ผ๐›ผ2โˆ’43๐›ฝ๐›ฝ2, then we arrive at the Adams-Williamson equation:
๐‘‘๐‘‘๐‘‘ ๐‘‘๐‘‘๐‘‘ = โˆ’๐บ๐บ๐‘€๐‘€๐‘Ÿ๐‘Ÿ๐œŒ๐œŒ(๐‘Ÿ๐‘Ÿ)๐‘Ÿ๐‘Ÿ2๐œ‘๐œ‘
This equation gives us the density gradient with respect to radius. Unfortunately, density is also on the RHS of this equation, which is what we are interested in solving for. We already know the seismic velocities however in great detail (see previous lecture!). So, how do we solve this problem?
What we do is an iterative approach. That is, we start at the Earthโ€™s surface at a known density:
๐œŒ๐œŒ(6371 ๐‘˜๐‘˜๐‘˜ )=3300๐‘˜๐‘˜๐‘˜ ๐‘š๐‘š3โ„
We know the Mass of the Earth (Mr) and the seismic wave speeds, so we can now calculate the gradient ๐‘‘๐‘‘๐‘‘ ๐‘‘๐‘‘๐‘‘ . Hence, with this gradient we can linearly extrapolate the density to a new smaller radius:
Now, with this new density, we can calculate a new Mr at the new radius, and repeat. Hence, it is an iterative process. Remember, we also have important constraints that must be satisfied:
โ€ข Total Mass of the Earth: ME = 5.974ร—1024 kg.
โ€ข Mass at each successive level: ๐‘€๐‘€๐‘Ÿ๐‘Ÿ=๐‘€๐‘€๐ธ๐ธโˆ’4๐œ‹๐œ‹โˆซ๐œŒ๐œŒ(๐‘Ÿ๐‘Ÿ)๐‘Ÿ๐‘Ÿ2๐‘‘๐‘‘๐‘‘ ๐‘…๐‘…๐ธ๐ธ๐‘Ÿ๐‘Ÿ
โ€ข Moment of inertia constant: ๐ผ๐ผ๐‘š๐‘š๐‘Ž๐‘Ž2=0.3307
There are a couple problems with direct implementation of this approach that also need to be accounted for.
GEO 5210 โ€“ Seismology I L14-18
โ€ข This assumes adiabatic compression. But, convection is happening in the mantle so an extra term accounting for convection must be included.
โ€ข This approach also assumes that the composition is constant throughout the Earth. This is readily accounted for by introducing density jumps at compositional boundaries.

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