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'''1.1. \htmladdnormallink{Classical mechanics''' {http://planetphysics.us/encyclopedia/NewtonianMechanics.html}.} In classical mechanics, we study the [[../CosmologicalConstant/|motion]] of a [[../Particle/|particle]]. This motion is described by a ([[../Vectors/|vector]]) [[../Bijective/|function]] of one variable, <math>q=q(t)</math>, representing the [[../Position/|position]] of the particle as a function of time. This function must satisfy the Newton equation of motion,
<math>
\ddot{q}=-U^{\prime}(q),
</math>
where <math>U</math> the potential [[../CosmologicalConstant/|energy]], and the [[../CosmologicalConstant/|mass]] of the particle is 1. Another way to express this law of motion is to say that <math>q(t)</math> must be a solution of a certain variational problem. Namely, one introduces {\it the [[../Lagrangian/|Lagrangian]]}
<math>
\mathcal{L}(q)=\frac{\dot{q}^{2}}{2}-U(q)
</math>
(the difference of kinetic and potential energy), and {\it the action functional}
<math>
S(q)=\int_{a}^{b}\mathcal{L}({\it q}){\it dt}
</math>
(for some fixed <math>a<b</math>). Then the law of motion can be expressed as {\it the least action principle}: <math>q(t)</math> must be a critical point of <math>S</math> on the space of all functions with given <math>q(a)</math> and <math>q(b)</math>. In other words, the Newton equation is the Euler-Lagrange equation for the solution of the variational problem defined by <math>S</math>.

'''Remark 1.'''  The name "least action principle" comes from the fact that in some cases (for example when <math>U^{\prime \prime}\leq 0</math>) the action is not only extremized but also minimized at the solution <math>q(t)</math>. In general, however, it is not the case, and the trajectory of the particle may not be a minimum, but only a saddle point of the action. Therefore, the law of motion is better formulated as the "extremal (or stationary) action principle" ; this is the way we will think of it in the future.

'''Remark 2.'''  Physicists often consider solutions of Newton's equation on the whole line rather than on a fixed interval <math>[a,\ b]</math>. In this case, the naive definition of an extremal does not make sense, since the action integral <math>S(q)= \int_{\mathbb{R}}\mathcal{L}(q)dt</math> is improper and in general diverges. Instead, one makes the following "correct" definition: a function <math>q(t)</math> on <math>\mathbb{R}</math> is an extremal of <math>S</math> if the expression
<math>
\frac{d}{ds}|_{s=0}\int_{\mathbb{R}}\mathcal{L}(q+s\epsilon)dt:=\int_{\mathbb{R}}(\frac{\partial L}{\partial q}\dot{\epsilon}+\frac{\partial L}{\partial\dot{q}}\ddot{\epsilon}+\cdots),
</math>
where <math>\epsilon(t)</math> is any compactly supported perturbation, is identically zero. With this definition, the extremals are exactly the solutions of Newton's equation.

\noindent
'''1.2. Classical \htmladdnormallink{field''' {http://planetphysics.us/encyclopedia/CosmologicalConstant2.html} theory.} In classical field theory, the situation is similar. In this case, we should think not of a single particle, but of a "continuum of particles" (e.g. a string, a membrane, a jet of fluid); so the motion is described by a classical field-a (vector) function <math>\phi(x,\ t)</math> depending on both space and time coordinates <math>(x\in \mathbb{R}^{d},\ t\in \mathbb{R})</math>. Consequently, the equation of motion is a [[../DifferentialEquations/|partial differential equation]]. For example, for a string or a membrane the equation of motion is the [[../TransversalWave/|wave equation]] <math>\square \phi=0</math>, where <math>\square </math> is the [[../DAlembertian/|D'Alembertian]] <math>\partial_{t}^{2}-v^{2}\triangle</math> (here <math>\triangle</math> is the [[../LaplaceOperator/|Laplacian]] with respect to the space coordinates, and <math>v</math> the [[../VelocityOfWave/|velocity of wave]] propagation).

As in [[../Mechanics/|mechanics]], in classical field theory there is a Lagrangian <math>\mathcal{L}(\phi)</math> (a differential polynomial in <math>\phi</math>), whose integral <math>S( \phi)=\int_{D}\mathcal{L}(\phi)dxdt</math> over a region <math>D</math> in space and time is called the action. The law of motion can be expressed as the condition that the action must be extremized over any closed region <math>D</math> and fixed [[../PiecewiseLinear/|boundary]] conditions; so the equations of motion (also called the field equations) are the Euler-Lagrange equations for this variational problem. For example, in the case of string or membrane, the Lagrangian is
<math>
\mathcal{L}(u)=\frac{1}{2}(\phi_{t}^{2}-v^{2}(\nabla\phi)^{2}).
</math>
'''Remark.'''  Like in mechanics, solutions of the field equations on the whole space (rather than a closed region <math>D</math>) are extremals of the action in the sense that
<math>
\frac{d}{ds}|_{s=0}\int_{\mathbb{R}^{d+1}}\mathcal{L}(u+s\epsilon)dxdt=0,
</math>
where <math>\epsilon</math> is a compactly supported perturbation.

\noindent
'''1.3. Brownian motion.'''  One of the main differences between classical and [[../QuantumParadox/|quantum mechanics]] is, roughly speaking, that [[../QuantumParticle/|quantum particles]] do not have to obey the classical equations of motion, but can randomly deviate from their classical trajectories. Therefore, given the position and [[../Velocity/|velocity]] of the particle at a given time, we cannot determine its position at a later time, but can only determine the density of probability that at this later time the particle will be found at a given point. In this sense quantum particles are similar to random (Brownian) particles. Brownian particles are a bit easier to understand conceptually, so let us begin with them.

The motion of a Brownian particle in <math>\mathbb{R}^{d}</math> in a potential field <math>U:\mathbb{R}^{d}\rightarrow \mathbb{R}</math> is described by astochastic process <math>q=q(t),\ q=(q_{1},\ \ldots,\ q_{d})\in \mathbb{R}^{d}</math>. That is, for each real <math>t</math> we have a [[../LebesgueMeasure/|random variable]] <math>q(t)</math> (position of the particle at a time <math>t</math>), such that the dependence of <math>t</math> is [[../CoIntersections/|regular]] in some sense. The random [[../NewtonianMechanics/|dynamics]] of the particle is "defined" as follows: 1 if <math>y</math> : <math>[a,\ b]\rightarrow \mathbb{R}^{d}</math> is a continuously differentiable function, then the density of probability that <math>q(t)=y(t)</math> for <math>t\in[a,\ b]</math> is proportional to <math>e^{-S(y)/\kappa}</math>, where <math>S(y) := \int_{a}^{b}(\frac{1}{2}y^{\prime 2}-U(y))dt</math> is the action for the corresponding classical mechanical [[../SimilarityAndAnalogousSystemsDynamicAdjointnessAndTopologicalEquivalence/|system]], and <math>\kappa</math> is the diffusion coefficient. Thus, for given <math>q(a)</math> and <math>q(b)</math>, the likeliest <math>q(t)</math> is the one that minimizes <math>S</math> (in particular, solves the classical equations of motion <math>\ddot{q}=-U^{\prime}(q))</math>, while the likelihood of the other paths decays exponentially with the deviation of the action of these paths from the minimal possible.

'''Remark.'''  This discussion assumes that the extremum of <math>S</math> at <math>q</math> is actually a minimum, which we know is not always the case.

All the information we can hope to get about such a process is contained in the correlation functions <math><q_{i_{1}}(t_{1})\ldots q_{i_{n}}(t_{n})></math>, which by definition are the expectation values of the products of random variables <math> q_{i_{1}}(t_{1})\ldots q_{i_{n}}(t_{n})</math> (more specifically, by Kolmogorov's [[../Formula/|theorem]] the stochastic process <math>q(t)</math> is completely determined by these functions). So such functions should be regarded as the output, or answer, of the theory of the Brownian particle.

So the main question is how to compute the correlation functions. The definition above obviously gives the following answer: given <math>t_{1},\ \ldots,\ t_{n}\in[a,\ b]</math>, we have
<math>
(1)= = \quad <q_{j_{1}}(t_{1})\ldots= =  q_{j_{n}}(t_{n})>=\int q_{j_{1}}(t_{1})\ldots= = q_{j_{n}}(t_{n})e^{-S(q)/\kappa}Dq,
</math>
where integration is carried out over the space of paths <math>[a,\ b]\rightarrow \mathbb{R}^{n}</math>, and <math>Dq</math> is a [[../LebesgueMeasure/|Lebesgue measure]] on the space of paths such that <math> \int e^{-S(q)/\kappa}Dq=1</math>. Such an integral is called a path integral, since it is an integral over the space of paths.

It is clear, however, that such definition and answer are a priori not satisfactory from the mathematical viewpoint, since the infinite dimensional integration that we used requires justification. In this particular case, such justification is possible within the framework of Lebesgue measure theory, and the corresponding integration theory is called the theory of Wiener integrals. (To be more precise, one cannot define the measure <math>Dq</math>, but one can define the measure <math>e^{-S(q)/\kappa}Dq</math> for sufficiently nice potentials <math>U(q))</math>.

\noindent
'''1.4. Quantum mechanics.'''  Now let us turn to a quantum particle. Quantum mechanics is notoriously difficult to visualize, and the randomness of the behavior of a quantum particle is less intuitive and more subtle than that of a Brownian particle; nevertheless, it was pointed out by Feynman that the behavior of a quantum particle in a potential field <math>U(q)</math> is correctly described by the same model, with the real positive [[../Parameter/|parameter]] <math>\kappa</math> replaced by the imaginary number <math> i\hslash</math>, where <math>\hslash>0</math> is the Planck constant. In other words, the dynamics of a quantum particle can be expressed via the {\it correlation functions}
<math>
(2)= = \quad <q_{j_{1}}(t_{1})\ldots= =  q_{j_{n}}(t_{n})>=\int q_{j_{1}}(t_{1})\ldots= = q_{j_{n}}(t_{n})e^{iS(q)/\hslash}Dq,
</math>
where <math>Dq</math> is normalized so that <math> \int e^{iS(q)/\hslash}Dq=1</math>.

\noindent
'''1.5. \htmladdnormallink{Quantum field theory''' {http://planetphysics.us/encyclopedia/SpaceTimeQuantizationInQuantumGravityTheories.html}.} The situation is the same in field theory. Namely, a useful theory of [[../CosmologicalConstant/|quantum fields]] (used in the study of interactions of elementary particles) is obtained when one considers correlation functions
<math>
(3)= = \quad <\phi_{j_{1}}(x_{1},\ t_{1})\ldots= = \phi_{j_{n}}(x_{n},\ t_{n})>=\int\phi_{j_{1}}(x_{1},\ t_{1})\ldots= = \phi_{j_{n}}(x_{n},\ t_{n})e^{iS(\phi)/\hslash}D\phi,
</math>
where <math> D\phi</math> is normalized so that <math> \int e^{iS(\phi)/\hslash}D\phi=1</math>.

Of course, from the mathematical point of view, this setting is a priori even less satisfactory than the one for the Brownian particle, since it involves integration with respect to the complex valued measure <math>e^{iS(q)/\hslash}Dq</math>, which nobody knows how to define. Nevertheless, physicists imagine that certain integrals of this [[../Bijective/|type]] exist and come to correct and interesting conclusions (both physical and mathematical). Therefore, making sense of such integrals is an interesting problem for mathematicians.

'''References'''

This is a derivative [[../Work/|work]] from [1] a [http://creativecommons.org/licenses/by-nc-sa/3.0/us/ Creative Commons Attribution-Noncommercial-Share Alike 3.0 work]

[1] MIT OpenCourseWare, 18.238 [http://ocw.mit.edu/OcwWeb/Mathematics/18-238Fall2002/LectureNotes/ Geometry and Quantum Field Theory], Fall 2002

{{CourseCat}}

[[Category:Quantum field theory]]