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Eigenvalues and eigenvectors of the second derivative
Encyclopedia
Explicit formulas for eigenvalues and eigenvectors of the second derivative
with different boundary conditions are provided both for the continuous and discrete cases. In the discrete case, the standard central difference approximation of the second derivative is used on a uniform grid.
These formulas are used to derive the expressions for eigenfunctions of Laplacian in case of separation of variables
, as well as to find eigenvalues and eigenvectors of multidimensional discrete Laplacian
on a regular grid
, which is presented as a Kronecker sum of discrete Laplacians
in one-dimension.
. Assuming the equation is defined on the domain
, the following are the eigenvalues and normalized eigenvectors. The eigenvalues are ordered in descending order.
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-3.gif)
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-4.gif)
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-5.gif)
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-6.gif)
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-7.gif)
(Note that eigenvalues are repeated except for 0 eigenvalue.)
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-8.gif)
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-9.gif)
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-10.gif)
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-11.gif)
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-12.gif)
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-13.gif)
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-14.gif)
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-15.gif)
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-16.gif)
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-17.gif)
(Note that eigenvalues are repeated except for 0 and the largest one if n is even.)![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-18.gif)
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-19.gif)
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-20.gif)
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-21.gif)
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-22.gif)
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-23.gif)
Rearranging terms, we get
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-24.gif)
Now let
. Also, assuming
, we can scale eigenvectors by any nonzero scalar, so scale
so that
.
Then we find the recurrence
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-29.gif)
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-30.gif)
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-31.gif)
Considering
as an indeterminate,
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-33.gif)
where
is the kth Chebyshev polynomial
of the 2nd kind.
Since
, we get that
.
It is clear that the eigenvalues of our problem will be the zeros of the nth Chebyshev polynomial of the second kind, with the relation
.
These zeros are well known and are:
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-38.gif)
Plugging these into the formula for
,
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-40.gif)
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-41.gif)
And using a trig formula to simplify, we find
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-42.gif)
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-43.gif)
In the standard discretization, we introduce
and
and define
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-46.gif)
The boundary conditions are then equivalent to![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-47.gif)
If we make a change of variables,![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-48.gif)
we can derive the following:![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-49.gif)
with
being the boundary conditions.
This is precisely the Dirichlet formula with
interior grid points and grid spacing
. Similar to what we saw in the above, assuming
, we get
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-54.gif)
This gives us
eigenvalues and there are
. If we drop the assumption that
, we find there is also a solution with
and this corresponds to eigenvalue
.
Relabeling the indices in the formula above and combining with the zero eigenvalue, we obtain,
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-60.gif)
,
where![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-62.gif)
We need to introduce auxiliary variables![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-63.gif)
Consider the recurrence
.
Also, we know
and assuming
, we can scale
so that ![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-68.gif)
We can also write![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-69.gif)
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-70.gif)
Taking the correct combination of these three equations, we can obtain
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-71.gif)
And thus our new recurrence will solve our eigenvalue problem when
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-72.gif)
Solving for
we get
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-74.gif)
Our new recurrence gives
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-75.gif)
where
again is the kth Chebyshev polynomial
of the 2nd kind.
And combining with our Neumann boundary condition, we have
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-77.gif)
A well-known formula relates the Chebyshev polynomials
of the first kind,
, to those of the second kind by
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-79.gif)
Thus our eigenvalues solve
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-80.gif)
The zeros of this polynomial are also known to be
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-81.gif)
And thus
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-82.gif)
Note that there are 2n + 1 of these values, but only the first n + 1 are unique. The (n + 1)th value gives us the zero vector as an eigenvector with eigenvalue 0, which is trivial. This can be seen by returning to the original recurrence. So we consider only the first n of these values to be the n eigenvalues of the Dirichlet - Neumann problem.
Second derivative
In calculus, the second derivative of a function ƒ is the derivative of the derivative of ƒ. Roughly speaking, the second derivative measures how the rate of change of a quantity is itself changing; for example, the second derivative of the position of a vehicle with respect to time is...
with different boundary conditions are provided both for the continuous and discrete cases. In the discrete case, the standard central difference approximation of the second derivative is used on a uniform grid.
These formulas are used to derive the expressions for eigenfunctions of Laplacian in case of separation of variables
Separation of variables
In mathematics, separation of variables is any of several methods for solving ordinary and partial differential equations, in which algebra allows one to rewrite an equation so that each of two variables occurs on a different side of the equation....
, as well as to find eigenvalues and eigenvectors of multidimensional discrete Laplacian
Discrete Laplace operator
In mathematics, the discrete Laplace operator is an analog of the continuous Laplace operator, defined so that it has meaning on a graph or a discrete grid...
on a regular grid
Regular grid
A regular grid is a tessellation of n-dimensional Euclidean space by congruent parallelotopes . Grids of this type appear on graph paper and may be used in finite element analysis as well as finite volume methods and finite difference methods...
, which is presented as a Kronecker sum of discrete Laplacians
Kronecker sum of discrete Laplacians
In mathematics, the Kronecker sum of discrete Laplacians, named after Leopold Kronecker, is a discrete version of the separation of variables for the continuous Laplacian in a rectangular cuboid domain.-General form of the Kronecker sum of discrete Laplacians:...
in one-dimension.
The continuous case
The index j represents the jth eigenvalue or eigenvector and runs from 1 to![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-1.gif)
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-2.gif)
Pure Dirichlet boundary conditions
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-3.gif)
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-4.gif)
Pure Neumann boundary conditions
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-5.gif)
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-6.gif)
Periodic boundary conditions
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-7.gif)
(Note that eigenvalues are repeated except for 0 eigenvalue.)
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-8.gif)
Mixed Dirichlet-Neumann boundary conditions
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-9.gif)
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-10.gif)
Mixed Neumann-Dirichlet boundary conditions
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-11.gif)
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-12.gif)
The discrete case
Notation: The index j represents the jth eigenvalue or eigenvector. The index i represents the ith component of an eigenvector. Both i and j go from 1 to n, where the matrix is size n x n. Eigenvectors are normalized. The eigenvalues are ordered in descending order.Pure Dirichlet boundary conditions
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-13.gif)
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-14.gif)
Pure Neumann boundary conditions
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-15.gif)
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-16.gif)
Periodic boundary conditions
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-17.gif)
(Note that eigenvalues are repeated except for 0 and the largest one if n is even.)
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-18.gif)
Mixed Dirichlet-Neumann boundary conditions
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-19.gif)
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-20.gif)
Mixed Neumann-Dirichlet boundary conditions
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-21.gif)
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-22.gif)
Dirichlet case
In the 1D discrete case with Dirichlet boundary conditions, we are solving![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-23.gif)
Rearranging terms, we get
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-24.gif)
Now let
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-25.gif)
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-26.gif)
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-27.gif)
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-28.gif)
Then we find the recurrence
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-29.gif)
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-30.gif)
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-31.gif)
Considering
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-32.gif)
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-33.gif)
where
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-34.gif)
Chebyshev polynomials
In mathematics the Chebyshev polynomials, named after Pafnuty Chebyshev, are a sequence of orthogonal polynomials which are related to de Moivre's formula and which can be defined recursively. One usually distinguishes between Chebyshev polynomials of the first kind which are denoted Tn and...
of the 2nd kind.
Since
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-35.gif)
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-36.gif)
It is clear that the eigenvalues of our problem will be the zeros of the nth Chebyshev polynomial of the second kind, with the relation
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-37.gif)
These zeros are well known and are:
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-38.gif)
Plugging these into the formula for
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-39.gif)
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-40.gif)
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-41.gif)
And using a trig formula to simplify, we find
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-42.gif)
Neumann case
In the Neumann case, we are solving![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-43.gif)
In the standard discretization, we introduce
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-44.gif)
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-45.gif)
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-46.gif)
The boundary conditions are then equivalent to
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-47.gif)
If we make a change of variables,
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-48.gif)
we can derive the following:
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-49.gif)
with
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-50.gif)
This is precisely the Dirichlet formula with
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-51.gif)
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-52.gif)
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-53.gif)
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-54.gif)
This gives us
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-55.gif)
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-56.gif)
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-57.gif)
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-58.gif)
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-59.gif)
Relabeling the indices in the formula above and combining with the zero eigenvalue, we obtain,
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-60.gif)
Dirichlet-Neumann Case
For the Dirichlet-Neumann case, we are solving![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-61.gif)
where
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-62.gif)
We need to introduce auxiliary variables
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-63.gif)
Consider the recurrence
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-64.gif)
Also, we know
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-65.gif)
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-66.gif)
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-67.gif)
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-68.gif)
We can also write
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-69.gif)
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-70.gif)
Taking the correct combination of these three equations, we can obtain
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-71.gif)
And thus our new recurrence will solve our eigenvalue problem when
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-72.gif)
Solving for
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-73.gif)
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-74.gif)
Our new recurrence gives
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-75.gif)
where
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-76.gif)
Chebyshev polynomials
In mathematics the Chebyshev polynomials, named after Pafnuty Chebyshev, are a sequence of orthogonal polynomials which are related to de Moivre's formula and which can be defined recursively. One usually distinguishes between Chebyshev polynomials of the first kind which are denoted Tn and...
of the 2nd kind.
And combining with our Neumann boundary condition, we have
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-77.gif)
A well-known formula relates the Chebyshev polynomials
Chebyshev polynomials
In mathematics the Chebyshev polynomials, named after Pafnuty Chebyshev, are a sequence of orthogonal polynomials which are related to de Moivre's formula and which can be defined recursively. One usually distinguishes between Chebyshev polynomials of the first kind which are denoted Tn and...
of the first kind,
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-78.gif)
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-79.gif)
Thus our eigenvalues solve
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-80.gif)
The zeros of this polynomial are also known to be
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-81.gif)
And thus
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-82.gif)
Note that there are 2n + 1 of these values, but only the first n + 1 are unique. The (n + 1)th value gives us the zero vector as an eigenvector with eigenvalue 0, which is trivial. This can be seen by returning to the original recurrence. So we consider only the first n of these values to be the n eigenvalues of the Dirichlet - Neumann problem.
![](http://image.absoluteastronomy.com/images/formulas/1/5/5153469-83.gif)