Boltzmann equation

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File:StairsOfReduction.svg

The place of the Boltzmann kinetic equation on the stairs of model reduction from microscopic dynamics to macroscopic continuum dynamics (illustration to the content of the book<ref> Template:Cite bookTemplate:Pn</ref>)

The Boltzmann equation or Boltzmann transport equation (BTE) describes the statistical behaviour of a thermodynamic system not in a state of equilibrium; it was devised by Ludwig Boltzmann in 1872.<ref name="Encyclopaediaof">Encyclopaedia of Physics (2nd Edition), R. G. Lerner, G. L. Trigg, VHC publishers, 1991, ISBN (Verlagsgesellschaft) 3-527-26954-1, ISBN (VHC Inc.) 0-89573-752-3.</ref> The classic example of such a system is a fluid with temperature gradients in space causing heat to flow from hotter regions to colder ones, by the random but biased transport of the particles making up that fluid. In the modern literature the term Boltzmann equation is often used in a more general sense, referring to any kinetic equation that describes the change of a macroscopic quantity in a thermodynamic system, such as energy, charge or particle number.

The equation arises not by analyzing the individual positions and momenta of each particle in the fluid but rather by considering a probability distribution for the position and momentum of a typical particle—that is, the probability that the particle occupies a given very small region of space (mathematically the volume element <math>d^3 \mathbf{r}</math>) centered at the position <math>\mathbf{r}</math>, and has momentum nearly equal to a given momentum vector <math> \mathbf{p}</math> (thus occupying a very small region of momentum space <math>d^3 \mathbf{p}</math>), at an instant of time.

The Boltzmann equation can be used to determine how physical quantities change, such as heat energy and momentum, when a fluid is in transport. One may also derive other properties characteristic to fluids such as viscosity, thermal conductivity, and electrical conductivity (by treating the charge carriers in a material as a gas).<ref name="Encyclopaediaof" /> See also convection–diffusion equation.

The equation is a nonlinear integro-differential equation, and the unknown function in the equation is a probability density function in six-dimensional space of a particle position and momentum. The problem of existence and uniqueness of solutions is still not fully resolved, but some recent results are quite promising.<ref>Template:Cite journal</ref><ref>Template:Cite journal</ref>

Overview

The phase space and density function

The set of all possible positions r and momenta p is called the phase space of the system; in other words a set of three coordinates for each position coordinate x, y, z, and three more for each momentum component Template:Math, Template:Math, Template:Math. The entire space is 6-dimensional: a point in this space is Template:Math, and each coordinate is parameterized by time t. A relevant differential element is written <math display="block"> d^3\mathbf{r} \, d^3\mathbf{p} = dx \, dy \, dz \, dp_x \, dp_y \, dp_z. </math>

Since the probability of Template:Mvar molecules, which all have Template:Math and Template:Math within <math> d^3\mathbf{r} \, d^3\mathbf{p}</math>, is in question, at the heart of the equation is a quantity Template:Math which gives this probability per unit phase-space volume, or probability per unit length cubed per unit momentum cubed, at an instant of time Template:Mvar. This is a probability density function: Template:Math, defined so that, <math display="block">dN = f (\mathbf{r},\mathbf{p},t) \, d^3\mathbf{r} \, d^3\mathbf{p}</math> is the number of molecules which all have positions lying within a volume element <math> d^3\mathbf{r}</math> about Template:Math and momenta lying within a momentum space element <math> d^3\mathbf{p}</math> about Template:Math, at time Template:Mvar.<ref>Template:Cite book</ref> Integrating over a region of position space and momentum space gives the total number of particles which have positions and momenta in that region:

<math display="block">\begin{align} N & = \int\limits_\mathrm{momenta} d^3\mathbf{p} \int\limits_\mathrm{positions} d^3\mathbf{r}\,f (\mathbf{r},\mathbf{p},t) \\[5pt] & = \iiint\limits_\mathrm{momenta} \quad \iiint\limits_\mathrm{positions} f(x,y,z, p_x,p_y,p_z, t) \, dx \, dy \, dz \, dp_x \, dp_y \, dp_z \end{align}</math>

which is a 6-fold integral. While Template:Math is associated with a number of particles, the phase space is for one-particle (not all of them, which is usually the case with deterministic many-body systems), since only one Template:Math and Template:Math is in question. It is not part of the analysis to use Template:Math, Template:Math for particle 1, Template:Math, Template:Math for particle 2, etc. up to Template:Math, Template:Math for particle N.

It is assumed the particles in the system are identical (so each has an identical mass Template:Mvar). For a mixture of more than one chemical species, one distribution is needed for each, see below.

Principal statement

The general equation can then be written as<ref name="McGrawHill">McGraw Hill Encyclopaedia of Physics (2nd Edition), S. P. Parker, 1993, Template:ISBN.</ref> <math display="block">

\frac{df}{dt} =
\left(\frac{\partial f}{\partial t}\right)_\text{force} +
\left(\frac{\partial f}{\partial t}\right)_\text{diff} +
\left(\frac{\partial f}{\partial t}\right)_\text{coll},

</math>

where the "force" term corresponds to the forces exerted on the particles by an external influence (not by the particles themselves), the "diff" term represents the diffusion of particles, and "coll" is the collision term – accounting for the forces acting between particles in collisions. Expressions for each term on the right side are provided below.<ref name="McGrawHill" />

Note that some authors use the particle velocity Template:Math instead of momentum Template:Math; they are related in the definition of momentum by Template:Math.

The force and diffusion terms

Consider particles described by Template:Math, each experiencing an external force Template:Math not due to other particles (see the collision term for the latter treatment).

Suppose at time Template:Mvar some number of particles all have position Template:Math within element <math> d^3\mathbf{r}</math> and momentum Template:Math within <math> d^3\mathbf{p}</math>. If a force Template:Math instantly acts on each particle, then at time Template:Math their position will be <math> \mathbf{r} + \Delta \mathbf{r} = \mathbf{r} +\frac{\mathbf{p}}{m} \, \Delta t </math> and momentum Template:Math. Then, in the absence of collisions, Template:Math must satisfy

<math display="block"> f \left (\mathbf{r}+\frac{\mathbf{p}}{m} \, \Delta t,\mathbf{p}+\mathbf{F} \, \Delta t, t+\Delta t \right )\,d^3\mathbf{r}\,d^3\mathbf{p} = f(\mathbf{r}, \mathbf{p},t) \, d^3\mathbf{r} \, d^3\mathbf{p} </math>

Note that we have used the fact that the phase space volume element <math> d^3\mathbf{r} \, d^3\mathbf{p}</math> is constant, which can be shown using Hamilton's equations (see the discussion under Liouville's theorem). However, since collisions do occur, the particle density in the phase-space volume <math> d^3\mathbf{r} \, d^3\mathbf{p}</math> changes, so Template:NumBlk

where Template:Math is the total change in Template:Math. Dividing (Template:EquationNote) by <math> d^3\mathbf{r} \, d^3\mathbf{p} \, \Delta t</math> and taking the limits Template:Math and Template:Math, we have Template:NumBlk

The total differential of Template:Math is: Template:NumBlk\cdot d\mathbf{p} \\[5pt] & = \frac{\partial f}{\partial t}dt +\nabla f \cdot \frac{\mathbf{p}}{m}dt + \frac{\partial f}{\partial \mathbf{p}}\cdot \mathbf{F} \, dt \end{align}</math> |Template:EquationRef}} where Template:Math is the gradient operator, Template:Math is the dot product, <math display="block"> \frac{\partial f}{\partial \mathbf{p}} = \mathbf{\hat{e}}_x\frac{\partial f}{\partial p_x} + \mathbf{\hat{e}}_y\frac{\partial f}{\partial p_y} + \mathbf{\hat{e}}_z \frac{\partial f}{\partial p_z}= \nabla_\mathbf{p}f </math> is a shorthand for the momentum analogue of Template:Math, and Template:Math, Template:Math, Template:Math are Cartesian unit vectors.

Final statement

Dividing (Template:EquationNote) by Template:Math and substituting into (Template:EquationNote) gives:

<math display="block">\frac{\partial f}{\partial t} + \frac{\mathbf{p}}{m}\cdot\nabla f + \mathbf{F} \cdot \frac{\partial f}{\partial \mathbf{p}} = \left(\frac{\partial f}{\partial t} \right)_\mathrm{coll}</math>

In this context, Template:Math is the force field acting on the particles in the fluid, and Template:Mvar is the mass of the particles. The term on the right hand side is added to describe the effect of collisions between particles; if it is zero then the particles do not collide. The collisionless Boltzmann equation, where individual collisions are replaced with long-range aggregated interactions, e.g. Coulomb interactions, is often called the Vlasov equation.

This equation is more useful than the principal one above, yet still incomplete, since Template:Math cannot be solved unless the collision term in Template:Math is known. This term cannot be found as easily or generally as the others – it is a statistical term representing the particle collisions, and requires knowledge of the statistics the particles obey, like the Maxwell–Boltzmann, Fermi–Dirac or Bose–Einstein distributions.

The collision term (Stosszahlansatz) and molecular chaos

Two-body collision term

A key insight applied by Boltzmann was to determine the collision term resulting solely from two-body collisions between particles that are assumed to be uncorrelated prior to the collision. This assumption was referred to by Boltzmann as the "{{#invoke:Lang|lang}}" and is also known as the "molecular chaos assumption". Under this assumption the collision term can be written as a momentum-space integral over the product of one-particle distribution functions:<ref name="Encyclopaediaof" /> <math display="block">

\left(\frac{\partial f}{\partial t}\right)_\text{coll} =
\iint g I(g, \Omega)[f(\mathbf{r},\mathbf{p'}_A, t) f(\mathbf{r},\mathbf{p'}_B,t) - f(\mathbf{r},\mathbf{p}_A,t) f(\mathbf{r},\mathbf{p}_B,t)] \,d\Omega \,d^3\mathbf{p}_B,

</math> where Template:Math and Template:Math are the momenta of any two particles (labeled as A and B for convenience) before a collision, Template:Math and Template:Math are the momenta after the collision, <math display="block">

g = |\mathbf{p}_B - \mathbf{p}_A| = |\mathbf{p'}_B - \mathbf{p'}_A|

</math> is the magnitude of the relative momenta (see relative velocity for more on this concept), and Template:Math is the differential cross section of the collision, in which the relative momenta of the colliding particles turns through an angle Template:Mvar into the element of the solid angle Template:Math, due to the collision.

Simplifications to the collision term

Since much of the challenge in solving the Boltzmann equation originates with the complex collision term, attempts have been made to "model" and simplify the collision term. The best known model equation is due to Bhatnagar, Gross and Krook.<ref>Template:Cite journal</ref> The assumption in the BGK approximation is that the effect of molecular collisions is to force a non-equilibrium distribution function at a point in physical space back to a Maxwellian equilibrium distribution function and that the rate at which this occurs is proportional to the molecular collision frequency. The Boltzmann equation is therefore modified to the BGK form:

<math display="block">\frac{\partial f}{\partial t} + \frac{\mathbf{p}}{m}\cdot\nabla f + \mathbf{F} \cdot \frac{\partial f}{\partial \mathbf{p}} = \nu (f_0 - f),</math>

where <math>\nu</math> is the molecular collision frequency, and <math>f_0</math> is the local Maxwellian distribution function given the gas temperature at this point in space. This is also called "relaxation time approximation".

General equation (for a mixture)

For a mixture of chemical species labelled by indices Template:Math the equation for species Template:Mvar is<ref name="Encyclopaediaof" />

<math display="block">\frac{\partial f_i}{\partial t} + \frac{\mathbf{p}_i}{m_i} \cdot \nabla f_i + \mathbf{F} \cdot \frac{\partial f_i}{\partial \mathbf{p}_i} = \left(\frac{\partial f_i}{\partial t} \right)_\text{coll},</math>

where Template:Math, and the collision term is

<math display="block"> \left(\frac{\partial f_i}{\partial t} \right)_{\mathrm{coll}} = \sum_{j=1}^n \iint g_{ij} I_{ij}(g_{ij}, \Omega)[f'_i f'_j - f_i f_j] \,d\Omega\,d^3\mathbf{p'},</math>

where Template:Math, the magnitude of the relative momenta is

<math display="block">g_{ij} = |\mathbf{p}_i - \mathbf{p}_j| = |\mathbf{p}'_i - \mathbf{p}'_j|,</math>

and Template:Math is the differential cross-section, as before, between particles i and j. The integration is over the momentum components in the integrand (which are labelled i and j). The sum of integrals describes the entry and exit of particles of species i in or out of the phase-space element.

Applications and extensions

Conservation equations

The Boltzmann equation can be used to derive the fluid dynamic conservation laws for mass, charge, momentum, and energy.<ref name="dG1984">Template:Cite book</ref>Template:Rp For a fluid consisting of only one kind of particle, the number density Template:Mvar is given by <math display="block">n = \int f \,d^3\mathbf{p}.</math>

The average value of any function Template:Math is <math display="block">\langle A \rangle = \frac 1 n \int A f \,d^3\mathbf{p}.</math>

Since the conservation equations involve tensors, the Einstein summation convention will be used where repeated indices in a product indicate summation over those indices. Thus <math>\mathbf{x} \mapsto x_i</math> and <math>\mathbf{p} \mapsto p_i = m v_i</math>, where <math>v_i</math> is the particle velocity vector. Define <math>A(p_i)</math> as some function of momentum <math>p_i</math> only, whose total value is conserved in a collision. Assume also that the force <math>F_i</math> is a function of position only, and that f is zero for <math>p_i \to \pm\infty</math>. Multiplying the Boltzmann equation by A and integrating over momentum yields four terms, which, using integration by parts, can be expressed as

<math display="block">\int A \frac{\partial f}{\partial t} \,d^3\mathbf{p} = \frac{\partial }{\partial t} (n \langle A \rangle),</math>

<math display="block">\int \frac{p_j A}{m}\frac{\partial f}{\partial x_j} \,d^3\mathbf{p} = \frac{1}{m}\frac{\partial}{\partial x_j}(n\langle A p_j \rangle),</math>

<math display="block">\int A F_j \frac{\partial f}{\partial p_j} \,d^3\mathbf{p} = -n F_j\left\langle \frac{\partial A}{\partial p_j}\right\rangle,</math>

<math display="block">\int A \left(\frac{\partial f}{\partial t}\right)_\text{coll} \,d^3\mathbf{p} = \frac{\partial }{\partial t}_\text{coll} (n \langle A \rangle) = 0,</math>

where the last term is zero, since Template:Math is conserved in a collision. The values of Template:Math correspond to moments of velocity <math>v_i</math> (and momentum <math>p_i</math>, as they are linearly dependent).

Zeroth moment

Letting <math>A = m(v_i)^0 = m</math>, the mass of the particle, the integrated Boltzmann equation becomes the conservation of mass equation:<ref name="dG1984" />Template:Rp <math display="block">\frac{\partial}{\partial t}\rho + \frac{\partial}{\partial x_j}(\rho V_j) = 0,</math> where <math>\rho = mn</math> is the mass density, and <math>V_i = \langle v_i\rangle</math> is the average fluid velocity.

First moment

Letting <math>A = m(v_i)^1 = p_i</math>, the momentum of the particle, the integrated Boltzmann equation becomes the conservation of momentum equation:<ref name="dG1984" />Template:Rp

<math display="block">\frac{\partial}{\partial t}(\rho V_i) + \frac{\partial}{\partial x_j}(\rho V_i V_j+P_{ij}) - n F_i = 0,</math>

where <math>P_{ij} = \rho \langle (v_i-V_i) (v_j-V_j) \rangle</math> is the pressure tensor (the viscous stress tensor plus the hydrostatic pressure).

Second moment

Letting <math>A = \frac{m(v_i)^2}{2} = \frac{p_i p_i}{2m}</math>, the kinetic energy of the particle, the integrated Boltzmann equation becomes the conservation of energy equation:<ref name="dG1984" />Template:Rp

<math display="block">\frac{\partial}{\partial t} \left(u + \tfrac{1}{2} \rho V_i V_i\right) + \frac{\partial}{\partial x_j} \left(u V_j + \tfrac{1}{2} \rho V_i V_i V_j + J_{qj} + P_{ij} V_i\right) - n F_i V_i = 0,</math>

where <math display="inline">u = \tfrac{1}{2} \rho \langle (v_i-V_i) (v_i-V_i) \rangle</math> is the kinetic thermal energy density, and <math display="inline">J_{qi} = \tfrac{1}{2} \rho \langle(v_i - V_i)(v_k - V_k)(v_k - V_k)\rangle</math> is the heat flux vector.

Hamiltonian mechanics

In Hamiltonian mechanics, the Boltzmann equation is often written more generally as <math display="block">\hat{\mathbf{L}}[f]=\mathbf{C}[f], </math> where Template:Math is the Liouville operator (there is an inconsistent definition between the Liouville operator as defined here and the one in the article linked) describing the evolution of a phase space volume and Template:Math is the collision operator. The non-relativistic form of Template:Math is <math display="block">\hat{\mathbf{L}}_\mathrm{NR} = \frac{\partial}{\partial t} + \frac{\mathbf{p}}{m} \cdot \nabla + \mathbf{F}\cdot\frac{\partial}{\partial \mathbf{p}}\,.</math>

Quantum theory and violation of particle number conservation

It is possible to write down relativistic quantum Boltzmann equations for relativistic quantum systems in which the number of particles is not conserved in collisions. This has several applications in physical cosmology,<ref name=KolbTurner>Template:Cite bookTemplate:Pn</ref> including the formation of the light elements in Big Bang nucleosynthesis, the production of dark matter and baryogenesis. It is not a priori clear that the state of a quantum system can be characterized by a classical phase space density f. However, for a wide class of applications a well-defined generalization of f exists which is the solution of an effective Boltzmann equation that can be derived from first principles of quantum field theory.<ref name=BEfromQFT>Template:Cite journal</ref>

General relativity and astronomy

The Boltzmann equation is of use in galactic dynamics. A galaxy, under certain assumptions, may be approximated as a continuous fluid; its mass distribution is then represented by f; in galaxies, physical collisions between the stars are very rare, and the effect of gravitational collisions can be neglected for times far longer than the age of the universe.

Its generalization in general relativity is<ref>Template:Cite book</ref><ref>R K Sachs (Academic Press NY)Template:Full</ref><ref>Template:Cite journal</ref><ref>Template:Cite journal</ref> <math display="block">\hat{\mathbf{L}}_\mathrm{GR}[f] = p^\alpha\frac{\partial f}{\partial x^\alpha} - \Gamma^\alpha{}_{\beta\gamma} p^\beta p^\gamma \frac{\partial f}{\partial p^\alpha} = C[f],</math> where Template:Math is the Christoffel symbol of the second kind (this assumes there are no external forces, so that particles move along geodesics in the absence of collisions), with the important subtlety that the density is a function in mixed contravariant-covariant Template:Math phase space as opposed to fully contravariant Template:Math phase space.<ref>Template:Cite journal</ref><ref>Template:Cite journal</ref>

In physical cosmology the fully covariant approach has been used to study the cosmic microwave background radiation.<ref>Template:Cite journal</ref> More generically the study of processes in the early universe often attempt to take into account the effects of quantum mechanics and general relativity.<ref name=KolbTurner /> In the very dense medium formed by the primordial plasma after the Big Bang, particles are continuously created and annihilated. In such an environment quantum coherence and the spatial extension of the wavefunction can affect the dynamics, making it questionable whether the classical phase space distribution f that appears in the Boltzmann equation is suitable to describe the system. In many cases it is, however, possible to derive an effective Boltzmann equation for a generalized distribution function from first principles of quantum field theory.<ref name=BEfromQFT /> This includes the formation of the light elements in Big Bang nucleosynthesis, the production of dark matter and baryogenesis.

Solving the equation

Exact solutions to the Boltzmann equations have been proven to exist in some cases;<ref>Template:Cite journal</ref> this analytical approach provides insight, but is not generally usable in practical problems.

Instead, numerical methods (including finite elements and lattice Boltzmann methods) are generally used to find approximate solutions to the various forms of the Boltzmann equation. Example applications range from hypersonic aerodynamics in rarefied gas flows<ref>Template:Cite journal</ref><ref>Template:Cite journal</ref> to plasma flows.<ref>Template:Cite journal</ref> An application of the Boltzmann equation in electrodynamics is the calculation of the electrical conductivity - the result is in leading order identical with the semiclassical result.<ref>Template:Cite book</ref>

Close to local equilibrium, solution of the Boltzmann equation can be represented by an asymptotic expansion in powers of Knudsen number (the Chapman–Enskog expansion<ref>Template:Cite bookTemplate:Pn</ref>). The first two terms of this expansion give the Euler equations and the Navier–Stokes equations. The higher terms have singularities. The problem of developing mathematically the limiting processes, which lead from the atomistic view (represented by Boltzmann's equation) to the laws of motion of continua, is an important part of Hilbert's sixth problem.<ref>Template:Cite journal</ref>

Limitations and further uses of the Boltzmann equation

The Boltzmann equation is valid only under several assumptions. For instance, the particles are assumed to be pointlike, i.e. without having a finite size. There exists a generalization of the Boltzmann equation that is called the Enskog equation.<ref name="Cercignani Microscopic Foundations">Template:Cite book</ref> The collision term is modified in Enskog equations such that particles have a finite size, for example they can be modelled as spheres having a fixed radius.

No further degrees of freedom besides translational motion are assumed for the particles. If there are internal degrees of freedom, the Boltzmann equation has to be generalized and might possess inelastic collisions.<ref name="Cercignani Microscopic Foundations"/>

Many real fluids like liquids or dense gases have besides the features mentioned above more complex forms of collisions, there will be not only binary, but also ternary and higher order collisions.<ref>Template:Cite arXiv</ref> These must be derived by using the BBGKY hierarchy.

Boltzmann-like equations are also used for the movement of cells.<ref>Template:Cite journal</ref><ref>Template:Cite journal</ref> Since cells are composite particles that carry internal degrees of freedom, the corresponding generalized Boltzmann equations must have inelastic collision integrals. Such equations can describe invasions of cancer cells in tissue, morphogenesis, and chemotaxis-related effects.

See also

• Vlasov equation
• The Vlasov–Poisson equation
• Landau kinetic equation
• Fokker–Planck equation
• Williams–Boltzmann equation
• Derivation of Navier–Stokes equation from LBE
• Derivation of Jeans equation from BE
• Jeans's theorem
• H-theorem

References

• Template:Cite book. Very inexpensive introduction to the modern framework (starting from a formal deduction from Liouville and the Bogoliubov–Born–Green–Kirkwood–Yvon hierarchy (BBGKY) in which the Boltzmann equation is placed). Most statistical mechanics textbooks like Huang still treat the topic using Boltzmann's original arguments. To derive the equation, these books use a heuristic explanation that does not bring out the range of validity and the characteristic assumptions that distinguish Boltzmann's from other transport equations like Fokker–Planck or Landau equations.

• Template:Cite journal
• Template:Cite journal
• Template:Cite journal

External links

• The Boltzmann Transport Equation by Franz Vesely
• Boltzmann gaseous behaviors solved