**Perturbation theory** comprises mathematical methods for finding an approximate solution to a problem, by starting from the exact solution of a related, simpler problem. A critical feature of the technique is a middle step that breaks the problem into "solvable" and "perturbation" parts.^{[1]} Perturbation theory is applicable if the problem at hand cannot be solved exactly, but can be formulated by adding a "small" term to the mathematical description of the exactly solvable problem.

Perturbation theory leads to an expression for the desired solution in terms of a formal power series in some "small" parameter – known as a **perturbation series** – that quantifies the deviation from the exactly solvable problem. The leading term in this power series is the solution of the exactly solvable problem, while further terms describe the deviation in the solution, due to the deviation from the initial problem. Formally, we have for the approximation to the full solution A, a series in the small parameter (here called ε), like the following:

In this example, *A*_{0} would be the known solution to the exactly solvable initial problem and *A*_{1}, *A*_{2}, ... represent the **higher-order terms** which may be found iteratively by some systematic procedure. For small ε these higher-order terms in the series become successively smaller.

An approximate "perturbation solution" is obtained by truncating the series, usually by keeping only the first two terms, the initial solution and the "first-order" perturbation correction

Perturbation theory is closely related to methods used in numerical analysis. The earliest use of what would now be called *perturbation theory* was to deal with the otherwise unsolvable mathematical problems of celestial mechanics: for example the orbit of the Moon, which moves noticeably differently from a simple Keplerian ellipse because of the competing gravitation of the Earth and the Sun.

Perturbation methods start with a simplified form of the original problem, which is *simple enough* to be solved exactly. In celestial mechanics, this is usually a Keplerian ellipse. Under non-relativistic gravity, an ellipse is exactly correct when there are only two gravitating bodies (say, the Earth and the Moon) but not quite correct when there are three or more objects (say, the Earth, Moon, Sun, and the rest of the solar system) and not quite correct when the gravitational interaction is stated using formulas from General relativity.

The solved, but simplified problem is then *“perturbed”* to make the conditions that the perturbed solution actually satisfies closer to the real problem, such as including the gravitational attraction of a third body (the Sun). The "conditions" are a formula (or several) that represent reality, often something arising from a physical law like Newton’s second law, the force-acceleration equation,

In the case of the example, the force **F** is calculated based on the number of gravitationally relevant bodies; the acceleration **a** is obtained, using calculus, from the path of the Moon in its orbit. Both of these come in two forms: approximate values for force and acceleration, which result from simplifications, and hypothetical exact values for force and acceleration, which would require the complete answer to calculate.

The slight changes that result from accommodating the perturbation, which themselves may have been simplified yet again, are used as corrections to the approximate solution. Because of simplifications introduced along every step of the way, the corrections are never perfect, and the conditions met by the corrected solution do not perfectly match the equation demanded by reality. However, even only one cycle of corrections often provides an excellent approximate answer to what the real solution should be.

There is no requirement to stop at only one cycle of corrections. A partially corrected solution can be re-used as the new starting point for yet another cycle of perturbations and corrections. In principle, cycles of finding increasingly better corrections could go on indefinitely. In practice, one typically stops at one or two cycles of corrections. The usual difficulty with the method is that the corrections progressively make the new solutions very much more complicated, so each cycle is much more difficult to manage than the previous cycle of corrections. Isaac Newton is reported to have said, regarding the problem of the Moon's orbit, that *"It causeth my head to ache."*^{[2]}

This general procedure is a widely used mathematical tool in advanced sciences and engineering: start with a simplified problem and gradually add corrections that make the formula that the corrected problem matches closer and closer to the formula that represents reality. It is the natural extension to mathematical functions of the "guess, check, and fix" method used by older civilisations to compute certain numbers, such as square roots.

Examples for the "mathematical description" are: an algebraic equation, a differential equation (e.g., the equations of motion in celestial mechanics or a wave equation), a free energy (in statistical mechanics), a Hamiltonian operator (in quantum mechanics).

Examples for the kind of solution to be found perturbatively: the solution of the equation (e.g., the trajectory of a particle), the statistical average of some physical quantity (e.g., average magnetization), the ground state energy of a quantum mechanical problem.

Examples for the exactly solvable problems to start with: linear equations, including linear equations of motion (harmonic oscillator, linear wave equation), statistical or quantum-mechanical systems of non-interacting particles (or in general, Hamiltonians or free energies containing only terms quadratic in all degrees of freedom).

Examples of "perturbations" to deal with: Nonlinear contributions to the equations of motion, interactions between particles, terms of higher powers in the Hamiltonian/Free Energy.

For physical problems involving interactions between particles, the terms of the perturbation series may be displayed (and manipulated) using Feynman diagrams.

Perturbation theory was first devised to solve otherwise intractable problems in the calculation of the motions of planets in the solar system.^{[who?]} The gradually increasing accuracy of astronomical observations led to incremental demands in the accuracy of solutions to Newton's gravitational equations, which led several notable 18th and 19th century mathematicians to extend and generalize the methods of perturbation theory.^{[who?]}^{[citation needed]} These well-developed perturbation methods were adopted and adapted to solve new problems arising during the development of Quantum Mechanics in 20th century atomic and subatomic physics.^{[who?]}^{[citation needed]}

Since the planets are very remote from each other, and since their mass is small as compared to the mass of the Sun, the gravitational forces between the planets can be neglected, and the planetary motion is considered, to a first approximation, as taking place along Kepler's orbits, which are defined by the equations of the two-body problem, the two bodies being the planet and the Sun.^{[3]}

Since astronomic data came to be known with much greater accuracy, it became necessary to consider how the motion of a planet around the Sun is affected by other planets. This was the origin of the three-body problem; thus, in studying the system Moon–Earth–Sun the mass ratio between the Moon and the Earth was chosen as the small parameter. Lagrange and Laplace were the first to advance the view that the constants which describe the motion of a planet around the Sun are "perturbed" , as it were, by the motion of other planets and vary as a function of time; hence the name "perturbation theory" .^{[3]}

Perturbation theory was investigated by the classical scholars — Laplace, Poisson, Gauss — as a result of which the computations could be performed with a very high accuracy. The discovery of the planet Neptune in 1848 by Urbain Le Verrier, based on the deviations in motion of the planet Uranus (he sent the coordinates to Johann Gottfried Galle who successfully observed Neptune through his telescope), represented a triumph of perturbation theory.^{[3]}

The standard exposition of perturbation theory is given in terms of the *order* to which the perturbation is carried out: **first-order perturbation theory** or **second-order perturbation theory**, and whether the perturbed states are degenerate, which requires **singular perturbation**. In the singular case extra care must be taken, and the theory is slightly more elaborate.

This section develops, in simple terms,^{[4]} the general theory for the perturbative solution to a differential equation to the first order. To keep the exposition simple, a crucial assumption is made: that the solutions to the unperturbed system are not *degenerate*, so that the perturbation series can be inverted. There are ways of dealing with the degenerate (or *singular*) case; these require extra care.

Suppose one wants to solve a differential equation of the form

where D is some specific differential operator, and λ is an eigenvalue. Many problems involving ordinary or partial differential equations can be cast in this form.

It is presumed that the differential operator can be written in the form

where ε is presumed to be small, and that, furthermore, the complete set of solutions for *D*^{(0)} are known.

That is, one has a set of solutions , labelled by some arbitrary index n, such that

Furthermore, one assumes that the set of solutions form an orthonormal set,

with *δ _{mn}* the Kronecker delta function.

To zeroth order, one expects that the solutions *g*(*x*) are then somehow "close" to one of the unperturbed solutions . That is,

and

where denotes the relative size, in big-O notation, of the perturbation.

To solve this problem, one assumes that the solution *g*(*x*) can be written as a linear combination of the ,

with all of the constants except for n, where .

Substituting this last expansion into the differential equation, taking the inner product of the result with , and making use of orthogonality, one obtains

This can be trivially rewritten as a simple linear algebra problem of finding the eigenvalue of a matrix, where

where the matrix elements *A _{nm}* are given by

Rather than solving this full matrix equation, one notes that, of all the *c _{m}* in the linear equation, only one, namely

since all of the other terms in the linear equation are of order . The above gives the solution of the eigenvalue to first order in perturbation theory.

The function *g*(*x*) to first order is obtained through similar reasoning. Substituting

so that

gives an equation for .

It may be solved integrating with the partition of unity

to give

which finally gives the exact solution to the perturbed differential equation to first order in the perturbation ε.

Several observations may be made about the form of this solution. First, the sum over functions with differences of eigenvalues in the denominator evokes the resolvent in Fredholm theory. This is no accident; the resolvent acts essentially as a kind of Green's function or propagator, passing the perturbation along. Higher-order perturbations resemble this form, with an additional sum over a resolvent appearing at each order.

The form of this solution also illustrates the idea behind the small-divisor problem. If, for whatever reason, two eigenvalues are close, so that the difference becomes small, the corresponding term in the above sum will become disproportionately large. In particular, if this happens in higher-order terms, the higher-order perturbation may become as large or larger in magnitude than the first-order perturbation. Such a situation calls into question the validity of utilizing a perturbative analysis to begin with, which can be understood to be a fairly catastrophic situation; it is frequently encountered in chaotic dynamical systems, and requires the development of techniques other than perturbation theory to solve the problem.

Curiously, the situation is not at all bad if two or more eigenvalues are *exactly equal*. This case is referred to as singular or degenerate perturbation theory, addressed below. The degeneracy of eigenvalues indicates that the unperturbed system has some sort of symmetry, and that the generators of that symmetry commute with the unperturbed differential operator. Typically, the perturbing term does not possess the symmetry, and so the full solutions do not, either; one says that the perturbation *lifts* or *breaks* the degeneracy. In this case, the perturbation can still be performed, as in following sections; however, care must be taken to work in a basis for the unperturbed states, so that these map one-to-one to the perturbed states, rather than being a mixture.

One may note that a problem occurs in the above first order perturbation theory when two or more eigenfunctions of the unperturbed system correspond to the same eigenvalue, i.e. when the eigenvalue equation becomes

and the index i labels *several states with the same eigenvalue* . The expression for the eigenfunctions which has energy differences in the denominators becomes infinite. In that case, degenerate perturbation theory must be applied.

The degeneracy must first be removed for higher order perturbation theory. First, consider the eigenfunction which is a linear combination of eigenfunctions with the same eigenvalue only,

which, again from the orthogonality of , leads to the following equation,

for each n.

As for the majority of low quantum numbers n, i changes over a *small range of integers*, so often the later equation can be solved analytically as an at most 4 × 4 matrix equation. Once the degeneracy is removed, the first and any order of the above perturbation theory may be further applied relying on the new eigenfunctions.

Consider the following equation for the unknown variable x:

For the initial problem with *ε* = 0, the solution is *x*_{0} = 1. For small ε the lowest-order approximation may be found by inserting the ansatz

into the equation and demanding the equation to be fulfilled up to terms that involve powers of ε higher than the first. This yields *x*_{1} = 1. In the same way, the higher orders may be found. However, even in this simple example it may be observed that for (arbitrarily) small positive ε there are four other solutions to the equation (with very large magnitude). The reason we don't find these solutions in the above perturbation method is because these solutions diverge when *ε* → 0 while the ansatz assumes regular behavior in this limit.

The four additional solutions can be found using the methods of **singular perturbation theory**. In this case this works as follows. Since the four solutions diverge at *ε* = 0, it makes sense to rescale x. We put

such that in terms of y the solutions stay finite. This means that we need to choose the exponent ν to match the rate at which the solutions diverge. In terms of y the equation reads:

The 'right' value for ν is obtained when the exponent of ε in the prefactor of the term proportional to y is equal to the exponent of ε in the prefactor of the term proportional to *y*^{5}, i.e. when *ν* = 1/4. This is called 'significant degeneration'. If we choose ν larger, then the four solutions will collapse to zero in terms of y and they will become degenerate with the solution we found above. If we choose ν smaller, then the four solutions will still diverge to infinity.

Putting *ν* = 1/4 in the above equation yields:

This equation can be solved using ordinary perturbation theory in the same way as regular expansion for x was obtained. Since the expansion parameter is now *ε*^{1/4} we put:

There are five solutions for *y*_{0}: {0, ±1, ±*i*}. We must disregard the solution *y* = 0 since it corresponds to the original regular solution which appears to be at zero for *ε* = 0, because in the limit *ε* → 0 we are rescaling by an infinite amount. The next term is *y*_{1} = − 1/4. In terms of x the four solutions are thus given as:

Many of the ab initio quantum chemistry methods use perturbation theory directly or are closely related methods. Implicit perturbation theory^{[5]} works with the complete Hamiltonian from the very beginning and never specifies a perturbation operator as such. Møller–Plesset perturbation theory uses the difference between the Hartree–Fock Hamiltonian and the exact non-relativistic Hamiltonian as the perturbation. The zero-order energy is the sum of orbital energies. The first-order energy is the Hartree–Fock energy and electron correlation is included at second-order or higher. Calculations to second, third or fourth order are very common and the code is included in most ab initio quantum chemistry programs. A related but more accurate method is the coupled cluster method.

- Cosmological perturbation theory
- Dynamic nuclear polarisation
- Alternative approach to perturbation theory
^{[6]} - Eigenvalue perturbation
- Interval FEM
- Orders of approximation
- Structural stability
- Lyapunov stability
- Homotopy perturbation method

**^**William E. Wiesel (2010).*Modern Astrodynamics*. Ohio: Aphelion Press. p. 107. ISBN 978-145378-1470.**^**Cropper, William H. (2004),*Great Physicists: The Life and Times of Leading Physicists from Galileo to Hawking*, Oxford University Press, p. 34, ISBN 978-0-19-517324-6.- ^
^{a}^{b}^{c}Perturbation theory. N. N. Bogolyubov, jr. (originator), Encyclopedia of Mathematics. URL: http://www.encyclopediaofmath.org/index.php?title=Perturbation_theory&oldid=11676 **^***Sakurai, J.J., and Napolitano, J. (1964,2011).*Modern quantum mechanics*(2nd ed.), Addison Wesley ISBN 978-0-8053-8291-4 . Chapter 5**^**King, Matcha (1976). "Theory of the Chemical Bond".*JACS*.**98**(12): 3415–3420. doi:10.1021/ja00428a004.**^**Martínez-Carranza, J.; Soto-Eguibar, F.; Moya-Cessa, H. (2012). "Alternative analysis to perturbation theory in quantum mechanics".*The European Physical Journal D*.**66**. arXiv:1110.0723. Bibcode:2012EPJD...66...22M. doi:10.1140/epjd/e2011-20654-5.