equation

Boltzmann equation

The Boltzmann equation governs the statistical behavior of a thermodynamic system not in equilibrium, describing the time evolution of particle distribution functions.
39 related articles · 5 formulas · 1 who worked here

Description

In 1872, Ludwig Boltzmann, an Austrian physicist, posed a bold question: how does the smooth flow of a gas arise from the chaotic jostling of molecules? Imagine a swarm of bees: each darts about on its own, but the whole swarm moves like a single cloud. The Boltzmann equation is the mathematical pattern of this cloud. It connects the random jumps of individual particles to the slow changes in density and temperature. The left side of the equation is like a movement schedule, the right side the result of collision accidents. Thanks to this bridge between the micro and macro worlds, we understand why a kettle boils and why a shock wave from an explosion propagates at a certain speed. The swarm remains a swarm, despite the chaos within.

History

Ludwig Boltzmann formulated the equation in 1872 in his work 'Further Studies on the Thermal Equilibrium of Gas Molecules', building on Maxwell's ideas. He introduced the H-theorem, proving entropy increase over time. Later, mathematicians Hilbert, Chapman, and Enskog developed solution methods. In the 20th century, the equation became the foundation of plasma physics and rarefied gas dynamics.

How it works

Used to calculate non-equilibrium flows: from satellite aerodynamics in the upper atmosphere to electron dynamics in semiconductors. Limitation: only for dilute media, where triple collisions are negligible; at high densities, kinetic theory of dense gases is needed. For quantum systems (fermions, bosons), the equation is modified into the Uehling–Uhlenbeck equation.

In practice

Used in engine design, aerodynamics, and plasma modeling in fusion reactors.

Fun fact

Boltzmann was persecuted for his ideas — many physicists of his era did not believe in atoms. He took his own life in 1906, but on his grave is engraved the formula S = k log W — the relationship between entropy and probability, which became an icon of statistical physics.

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Formulas

$$ rac{ ext{d} ext{concentration}}{ ext{d}t} = ext{divergence of flux}$$
Describes how concentration changes over time due to diffusion.
What is in the formula
concentrationvariablelocal concentration of the diffusing species — concentration mole per cubic metre
tvariabletime — time second
fluxvariablediffusive flux vector — diffusive flux mole per square metre per second
d/dtoperatorrate of change with respect to time — time derivative
divergenceoperatormeasures the net outflow of a vector field per unit volume — divergence operator
\partial_tφ\simeq\nabla*[\frac{(1-φ)^2φ}{n_0\zeta_0μ(φ)}\nabla\pi] · 2606.31786
$$\frac{dP}{dr} = -\frac{(P+\varepsilon)(m+4\pi r^3 P)}{r(r-2m)}$$
Describes hydrostatic equilibrium in general relativistic stars.
What is in the formula
PvariablePressure at radius r — pressure pascal
rvariableRadial coordinate — radius metre
εvariableEnergy density — energy density joule per cubic metre
mvariableMass enclosed within radius r — mass kilogram
d/droperatorDerivative with respect to radial coordinate — ordinary derivative
\frac{dp_i}{dr}=-\frac{(p_i+\varepsilon_i)(m+4πr^3(p_{{nm}}+p_{{dm}}))}{r(r-2m)} · 2607.03840v1
$$\frac{dP_r}{dr} = -\frac{G(\epsilon + P_r)(m + 4\pi r^3 P_r/c^2)}{c^2 r^2 (1 - 2Gm/(c^2 r))} + \frac{2(P_t - P_r)}{r}$$
Describes hydrostatic equilibrium in general relativity with anisotropic pressure.
What is in the formula
P_rvariableRadial pressure — pressure pascal
rvariableRadial coordinate — radius metre
εvariableEnergy density — energy density joule per cubic metre
mvariableMass enclosed within radius r — mass kilogram
P_tvariableTangential pressure — pressure pascal
GconstantFundamental constant governing gravitational strength — gravitational constant = 6.67430e-11 cubic metre per kilogram per second squared
cconstantUniversal speed limit for massless particles — speed of light = 299792458 metre per second
d/droperatorDifferentiates a function with respect to r — ordinary derivative
\frac{dp_r}{dr}=-\frac{g(ε+p_r)(m+4πr^3p_r/c^2)}{c^2r^2(1-2gm/(c^2r))}+\frac{2(p_t-p_r)}{r} · 2607.25055v1
$$\frac{N_i}{N} = \frac{g_i e^{-E_i/kT}}{Q}$$
Probability of a state in thermal equilibrium.
What is in the formula
N_ivariableNumber of particles in state i — particle number
NvariableTotal number of particles — particle number
g_ivariableDegeneracy of state i — degeneracy
E_ivariableEnergy of state i — energy joule
TvariableAbsolute temperature — temperature kelvin
kconstantRelates energy to temperature at the particle level — boltzmann constant = 1.380649e-23 joule per kelvin
e^{-E_i/kT}operatorExponential of the negative energy over kT — exponential function
\frac{n_u}{n_{{tot}}}=\frac{g_u}{q}e^{-e_u/kt} · 2606.03313v1
p(s)=\frac{1}{z(β)}\exp(-βe) · 2607.10285
$$\frac{dP}{dr} = -\frac{G m(r) \rho(r)}{r^2} \left[1+\frac{P(r)}{\rho(r)c^2}\right] \left[1+\frac{4\pi r^3 P(r)}{m(r)c^2}\right] \left[1-\frac{2Gm(r)}{rc^2}\right]^{-1}$$
General relativistic equation for hydrostatic equilibrium in spherical symmetry.
What is in the formula
PvariablePressure — pressure pascal
rvariableRadial coordinate — radius metre
mvariableEnclosed mass — mass kilogram
ρvariableMass density — mass density kilogram per metre cubed
GconstantUniversal gravitational constant — gravitational constant = 6.67430e-11 metre cubed per kilogram per second squared
cconstantSpeed of light in vacuum — speed of light = 299792458 metre per second
d/droperatorDerivative with respect to radial coordinate — derivative with respect to radius
\frac{dp}{dr}=-\frac{gm(r)ρ(r)}{r^2}[1+\frac{p(r)}{ρ(r)c^2}][1+\frac{4πr^3p(r)}{m(r)c^2}][1-\frac{2gm(r)}{rc^2}]^{-1} · 2607.12722
\frac{dp}{dr}=-\frac{gm(r)\varepsilon}{r^2}(1+\frac{p}{\varepsilon})(1+\frac{4πr^3p}{m(r)})(1-\frac{2gm(r)}{r})^{-1} · 2607.13930

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