# Spherical harmonics

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In mathematics, **spherical harmonics** are the angular portion of a set of solutions to Laplace's equation. Represented in a system of spherical coordinates, Laplace's spherical harmonics are a specific set of spherical harmonics that forms an orthogonal system, first introduced by Pierre Simon de Laplace in 1782.^{[1]} Spherical harmonics are important in many theoretical and practical applications, particularly in the computation of atomic orbital electron configurations, representation of gravitational fields, geoids, and the magnetic fields of planetary bodies and stars, and characterization of the cosmic microwave background radiation. In 3D computer graphics, spherical harmonics play a special role in a wide variety of topics including indirect lighting (ambient occlusion, global illumination, precomputed radiance transfer, etc.) and modelling of 3D shapes.

## History

Spherical harmonics were first investigated in connection with the Newtonian potential of Newton's law of universal gravitation in three dimensions. In 1782, Pierre-Simon de Laplace had, in his *Mécanique Céleste*, determined that the gravitational potential at a point **x** associated to a set of point masses *m*_{i} located at points **x**_{i} was given by

Each term in the above summation is an individual Newtonian potential for a point mass. Just prior to that time, Adrien-Marie Legendre had investigated the expansion of the Newtonian potential in powers of *r* = |**x**| and *r*_{1} = |**x**_{1}|. He discovered that if *r* ≤ *r*_{1} then

where γ is the angle between the vectors **x** and **x**_{1}. The functions *P*_{i} are the Legendre polynomials, and they are a special case of spherical harmonics. Subsequently, in his 1782 memoire, Laplace investigated these coefficients using spherical coordinates to represent the angle γ between **x**_{1} and **x**. (See Applications of Legendre polynomials in physics for a more detailed analysis.)

In 1867, William Thomson (Lord Kelvin) and Peter Guthrie Tait introduced the solid spherical harmonics in their *Treatise on Natural Philosophy*, and also first introduced the name of "spherical harmonics" for these functions. The solid harmonics were homogeneous solutions of Laplace's equation

By examining Laplace's equation in spherical coordinates, Thomson and Tait recovered Laplace's spherical harmonics. The term "Laplace's coefficients" was employed by William Whewell to describe the particular system of solutions introduced along these lines, whereas others reserved this designation for the zonal spherical harmonics that had properly been introduced by Laplace and Legendre.

The 19th century development of Fourier series made possible the solution of a wide variety of physical problems in rectangular domains, such as the solution of the heat equation and wave equation. This could be achieved by expansion of functions in series of trigonometric functions. Whereas the trigonometric functions in a Fourier series represent the fundamental modes of vibration in a string, the spherical harmonics represent the fundamental modes of vibration of a sphere in much the same way. Many aspects of the theory of Fourier series could be generalized by taking expansions in spherical harmonics rather than trigonometric functions. This was a boon for problems possessing spherical symmetry, such as those of celestial mechanics originally studied by Laplace and Legendre.

The prevalence of spherical harmonics already in physics set the stage for their later importance in the 20th century birth of quantum mechanics. The spherical harmonics are eigenfunctions of the square of the orbital angular momentum operator

and therefore they represent the different quantized configurations of atomic orbitals.

## Laplace's spherical harmonics

Laplace's equation imposes that the divergence of the gradient of a scalar field *f* is zero. In spherical coordinates this is:^{[2]}

Consider the problem of finding solutions of the form *f*(*r*,θ,φ) = *R*(*r*)*Y*(θ,φ). By separation of variables, two differential equations result by imposing Laplace's equation:

The second equation can be simplified under the assumption that *Y* has the form *Y*(θ,φ) = Θ(θ)Φ(φ). Applying separation of variables again to the second equation gives way to the pair of differential equations

for some number *m*. A priori, *m* is a complex constant, but because Φ must be a periodic function whose period evenly divides 2π, *m* is necessarily an integer and Φ is a linear combination of the complex exponentials *e*^{±imφ}. The solution function *Y*(θ,φ) is regular at the poles of the sphere, where θ=0,π. Imposing this regularity in the solution Θ of the second equation at the boundary points of the domain is a Sturm–Liouville problem that forces the parameter λ to be of the form λ = ℓ(ℓ+1) for some non-negative integer with ℓ ≥ |*m*|; this is also explained below in terms of the orbital angular momentum. Furthermore, a change of variables *t* = cosθ transforms this equation into the Legendre equation, whose solution is a multiple of the associated Legendre polynomial . Finally, the equation for *R* has solutions of the form *R*(*r*) = *Ar*^{ℓ} + *Br*^{−ℓ−1}; requiring the solution to be regular throughout **R**^{3} forces *B* = 0.^{[3]}

Here the solution was assumed to have the special form *Y*(θ,φ) = Θ(θ)Φ(φ). For a given value of ℓ, there are 2ℓ+1 independent solutions of this form, one for each integer *m* with −ℓ ≤ *m* ≤ ℓ. These angular solutions are a product of trigonometric functions, here represented as a complex exponential, and associated Legendre polynomials:

which fulfill

Here is called a spherical harmonic function of degree ℓ and order *m*, is an associated Legendre polynomial, *N* is a normalization constant, and θ and φ represent colatitude and longitude, respectively. In particular, the colatitude θ, or polar angle, ranges from 0 at the North Pole to π at the South Pole, assuming the value of π/2 at the Equator, and the longitude φ, or azimuth, may assume all values with 0 ≤ φ < 2π. For a fixed integer ℓ, every solution *Y*(θ,φ) of the eigenvalue problem

is a linear combination of . In fact, for any such solution, *r*^{ℓ}*Y*(θ,φ) is the expression in spherical coordinates of a homogeneous polynomial that is harmonic (see below), and so counting dimensions shows that there are 2ℓ+1 linearly independent such polynomials.

The general solution to Laplace's equation in a ball centered at the origin is a linear combination of the spherical harmonic functions multiplied by the appropriate scale factor *r*^{ℓ},

where the are constants and the factors are known as solid harmonics. Such an expansion is valid in the ball

### Orbital angular momentum

In quantum mechanics, Laplace's spherical harmonics are understood in terms of the orbital angular momentum^{[4]}

The is conventional in quantum mechanics; it is convenient to work in units in which . The spherical harmonics are eigenfunctions of the square of the orbital angular momentum

Laplace's spherical harmonics are the joint eigenfunctions of the square of the orbital angular momentum and the generator of rotations about the azimuthal axis:

These operators commute, and are densely defined self-adjoint operators on the Hilbert space of functions *f* square-integrable with respect to the normal distribution on **R**^{3}:

Furthermore, **L**^{2} is a positive operator.

If *Y* is a joint eigenfunction of **L**^{2} and *L*_{z}, then by definition

for some real numbers *m* and λ. Here *m* must in fact be an integer, for *Y* must be periodic in the coordinate φ with period a number that evenly divides 2π. Furthermore, since

and each of *L*_{x}, *L*_{y}, *L*_{z} are self-adjoint, it follows that λ ≥ *m*^{2}.

Denote this joint eigenspace by *E*_{λ,m}, and define the raising and lowering operators by

Then *L*_{+} and *L*_{−} commute with **L**^{2}, and the Lie algebra generated by *L*_{+}, *L*_{−}, *L*_{z} is the special linear Lie algebra, with commutation relations

Thus *L*_{+} : *E*_{λ,m} → *E*_{λ,m+1} (it is a "raising operator") and *L*_{−} : *E*_{λ,m} → *E*_{λ,m−1} (it is a "lowering operator"). In particular, *L*Template:Su : *E*_{λ,m} → *E*_{λ,m+k} must be zero for *k* sufficiently large, because the inequality λ ≥ *m*^{2} must hold in each of the nontrivial joint eigenspaces. Let *Y* ∈ *E*_{λ,m} be a nonzero joint eigenfunction, and let *k* be the least integer such that

Then, since

it follows that

Thus λ = ℓ(ℓ+1) for the positive integer ℓ = *m*+*k*.

## Conventions

### Orthogonality and normalization

Several different normalizations are in common use for the Laplace spherical harmonic functions. Throughout the section, we use the standard convention that (see associated Legendre polynomials)

which is the natural normalization given by Rodrigues' formula.

In seismology, the Laplace spherical harmonics are generally defined as (this is the convention used in this article)

while in quantum mechanics:^{[5]}^{[6]}

which are orthonormal

where δ_{ij} is the Kronecker delta and *d*Ω = sinθ *d*φ *d*θ. This normalization is used in quantum mechanics because it ensures that probability is normalized, i.e.

The disciplines of geodesy and spectral analysis use

which possess unit power

The magnetics community, in contrast, uses Schmidt semi-normalized harmonics

which have the normalization

In quantum mechanics this normalization is sometimes used as well, and is named Racah's normalization after Giulio Racah.

It can be shown that all of the above normalized spherical harmonic functions satisfy

where the superscript * denotes complex conjugation. Alternatively, this equation follows from the relation of the spherical harmonic functions with the Wigner D-matrix.

### Condon–Shortley phase

One source of confusion with the definition of the spherical harmonic functions concerns a phase factor of (−1)^{m} for *m* > 0, 1 otherwise, commonly referred to as the Condon–Shortley phase in the quantum mechanical literature. In the quantum mechanics community, it is common practice to either include this phase factor in the definition of the associated Legendre polynomials, or to append it to the definition of the spherical harmonic functions. There is no requirement to use the Condon–Shortley phase in the definition of the spherical harmonic functions, but including it can simplify some quantum mechanical operations, especially the application of raising and lowering operators. The geodesy^{[7]} and magnetics communities never include the Condon–Shortley phase factor in their definitions of the spherical harmonic functions nor in the ones of the associated Legendre polynomials.{{ safesubst:#invoke:Unsubst||date=__DATE__ |$B=
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### Real form

A real basis of spherical harmonics can be defined in terms of their complex analogues by setting

The Condon-Shortley phase convention is used here for consistency. The corresponding inverse equations are

The real spherical harmonics are sometimes known as *tesseral spherical harmonics*.^{[8]} These functions have the same orthonormality properties as the complex ones above.
The harmonics with *m* > 0 are said to be of cosine type, and those with *m* < 0 of sine type. The reason for this can be seen by writing the functions in terms of the Legendre polynomials as

The same sine and cosine factors can be also seen in the following subsection that deals with the cartesian representation.

See here for a list of real spherical harmonics up to and including , which can be seen to be consistent with the output of the equations above.

#### Use in quantum chemistry

As is known from the analytic solutions for the hydrogen atom, the eigenfunctions of the angular part of the wave function are spherical harmonics. However, the solutions of the non-relativistic Schrödinger equation without magnetic terms can be made real. This is why the real forms are extensively used in basis functions for quantum chemistry, as the programs don't then need to use complex algebra. Here, it is important to note that the real functions span the same space as the complex ones would.

For example, as can be seen from the table of spherical harmonics, the usual *p* functions () are complex and mix axis directions, but the real versions are essentially just *x*, *y* and *z*.

## Spherical harmonics in Cartesian form

The following expresses normalized spherical harmonics in Cartesian coordinates (Condon-Shortley phase):

and for *m* = 0:

Here

and

### Examples

Using the expressions for , , and listed explicitly above we obtain:

It may be verified that this agrees with the function listed here and here.

### Real form

Using the equations above to form the real spherical harmonics, it is seen that for only the terms (cosines) are included, and for only the terms (sines) are included:

and for *m* = 0:

## Spherical harmonics expansion

The Laplace spherical harmonics form a complete set of orthonormal functions and thus form an orthonormal basis of the Hilbert space of square-integrable functions. On the unit sphere, any square-integrable function can thus be expanded as a linear combination of these:

This expansion holds in the sense of mean-square convergence — convergence in L^{2} of the sphere — which is to say that

The expansion coefficients are the analogs of Fourier coefficients, and can be obtained by multiplying the above equation by the complex conjugate of a spherical harmonic, integrating over the solid angle Ω, and utilizing the above orthogonality relationships. This is justified rigorously by basic Hilbert space theory. For the case of orthonormalized harmonics, this gives:

If the coefficients decay in ℓ sufficiently rapidly — for instance, exponentially — then the series also converges uniformly to *f*.

A square-integrable function *f* can also be expanded in terms of the real harmonics *Y*_{ℓm} above as a sum

The convergence of the series holds again in the same sense, but the benefit of the real expansion is that for real functions *f* the expansion coefficients become real.

## Spectrum analysis

### Power spectrum in signal processing

The total power of a function *f* is defined in the signal processing literature as the integral of the function squared, divided by the area of its domain. Using the orthonormality properties of the real unit-power spherical harmonic functions, it is straightforward to verify that the total power of a function defined on the unit sphere is related to its spectral coefficients by a generalization of Parseval's theorem:

where

is defined as the angular power spectrum. In a similar manner, one can define the cross-power of two functions as

where

is defined as the cross-power spectrum. If the functions *f* and *g* have a zero mean (i.e., the spectral coefficients *f*_{00} and *g*_{00} are zero), then *S*_{ff}(ℓ) and *S*_{fg}(ℓ) represent the contributions to the function's variance and covariance for degree ℓ, respectively. It is common that the (cross-)power spectrum is well approximated by a power law of the form

When β = 0, the spectrum is "white" as each degree possesses equal power. When β < 0, the spectrum is termed "red" as there is more power at the low degrees with long wavelengths than higher degrees. Finally, when β > 0, the spectrum is termed "blue". The condition on the order of growth of *S*_{ff}(ℓ) is related to the order of differentiability of *f* in the next section.

### Differentiability properties

One can also understand the differentiability properties of the original function *f* in terms of the asymptotics of *S*_{ff}(ℓ). In particular, if *S*_{ff}(ℓ) decays faster than any rational function of ℓ as ℓ → ∞, then *f* is infinitely differentiable. If, furthermore, *S*_{ff}(ℓ) decays exponentially, then *f* is actually real analytic on the sphere.

The general technique is to use the theory of Sobolev spaces. Statements relating the growth of the *S*_{ff}(ℓ) to differentiability are then similar to analogous results on the growth of the coefficients of Fourier series. Specifically, if

then *f* is in the Sobolev space *H*^{s}(*S*^{2}). In particular, the Sobolev embedding theorem implies that *f* is infinitely differentiable provided that

for all *s*.

## Algebraic properties

### Addition theorem

A mathematical result of considerable interest and use is called the *addition theorem* for spherical harmonics. This is a generalization of the trigonometric identity

in which the role of the trigonometric functions appearing on the right-hand side is played by the spherical harmonics and that of the left-hand side is played by the Legendre polynomials.

Consider two unit vectors **x** and **y**, having spherical coordinates (θ,φ) and (θ′,φ′), respectively. The addition theorem states

where *P*_{ℓ} is the Legendre polynomial of degree ℓ. This expression is valid for both real and complex harmonics.^{[9]} The result can be proven analytically, using the properties of the Poisson kernel in the unit ball, or geometrically by applying a rotation to the vector **y** so that it points along the *z*-axis, and then directly calculating the right-hand side.^{[10]}

In particular, when **x** = **y**, this gives Unsöld's theorem^{[11]}

which generalizes the identity cos^{2}θ + sin^{2}θ = 1 to two dimensions.

In the expansion (Template:EquationNote), the left-hand side *P*_{ℓ}(**x**·**y**) is a constant multiple of the degree ℓ zonal spherical harmonic. From this perspective, one has the following generalization to higher dimensions. Let *Y*_{j} be an arbitrary orthonormal basis of the space **H**_{ℓ} of degree ℓ spherical harmonics on the *n*-sphere. Then , the degree ℓ zonal harmonic corresponding to the unit vector *x*, decomposes as^{[12]}

Furthermore, the zonal harmonic is given as a constant multiple of the appropriate Gegenbauer polynomial:
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Combining (Template:EquationNote) and (Template:EquationNote) gives (Template:EquationNote) in dimension *n* = 2 when **x** and **y** are represented in spherical coordinates. Finally, evaluating at **x** = **y** gives the functional identity

where ω_{n−1} is the volume of the (*n*−1)-sphere.

### Clebsch–Gordan coefficients

{{#invoke:main|main}} The Clebsch–Gordan coefficients are the coefficients appearing in the expansion of the product of two spherical harmonics in terms of spherical harmonics itself. A variety of techniques are available for doing essentially the same calculation, including the Wigner 3-jm symbol, the Racah coefficients, and the Slater integrals. Abstractly, the Clebsch–Gordan coefficients express the tensor product of two irreducible representations of the rotation group as a sum of irreducible representations: suitably normalized, the coefficients are then the multiplicities.

### Parity

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The spherical harmonics have well defined parity in the sense that they are either even or odd with respect to reflection about the origin. Reflection about the origin is represented by the operator . For the spherical angles, this corresponds to the replacement . The associated Legendre polynomials gives (−1)^{ℓ+m} and from the exponential function we have (−1)^{m}, giving together for the spherical harmonics a parity of (−1)^{ℓ}:

This remains true for spherical harmonics in higher dimensions: applying a point reflection to a spherical harmonic of degree ℓ changes the sign by a factor of (−1)^{ℓ}.

## Visualization of the spherical harmonics

The Laplace spherical harmonics can be visualized by considering their "nodal lines", that is, the set of points on the sphere where , or alternatively where . Nodal lines of are composed of circles: some are latitudes and others are longitudes. One can determine the number of nodal lines of each type by counting the number of zeros of in the latitudinal and longitudinal directions independently. For the latitudinal direction, the real and imaginary components of the associated Legendre polynomials each possess ℓ−|*m*| zeros, whereas for the longitudinal direction, the trigonometric sin and cos functions possess 2|*m*| zeros.

When the spherical harmonic order *m* is zero (upper-left in the figure), the spherical harmonic functions do not depend upon longitude, and are referred to as **zonal**. Such spherical harmonics are a special case of zonal spherical functions. When ℓ = |*m*| (bottom-right in the figure), there are no zero crossings in latitude, and the functions are referred to as **sectoral**. For the other cases, the functions checker the sphere, and they are referred to as **tesseral**.

More general spherical harmonics of degree ℓ are not necessarily those of the Laplace basis , and their nodal sets can be of a fairly general kind.^{[13]}

## List of spherical harmonics

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Analytic expressions for the first few orthonormalized Laplace spherical harmonics that use the Condon-Shortley phase convention: