equation

Navier-Stokes equations

The Navier-Stokes equations are partial differential equations that describe the motion of viscous fluid substances in various flow conditions.
51 related articles · 4 formulas · 3 who worked here

Description

French engineer Claude-Louis Navier (1821) and British physicist George Stokes (1845) combined into a system equations expressing the conservation of mass and momentum in a viscous fluid. The momentum equation: ρ (∂v/∂t + v·∇v) = -∇p + μ ∇²v + f. The left side is mass times acceleration (including convective transport), the right side includes pressure forces, viscous friction, and external influences. The incompressibility condition ∇·v = 0 is added. Their genius was accounting for internal friction (the term with viscosity μ).

History

Claude-Louis Navier derived the equations in 1821, introducing a molecular hypothesis about forces between particles. In 1845, George Gabriel Stokes refined the derivation, abandoning molecular notions and formulating the commonly accepted form with a continuum approach. Later, Leonhard Euler derived equations for an ideal (inviscid) fluid, and Navier and Stokes added viscosity.

How it works

The equations are the foundation of hydro- and aerodynamics, meteorology, oceanography, astrophysics (accretion disks, interstellar medium). Depending on the Reynolds number, they describe laminar or turbulent flow. Numerical methods of computational fluid dynamics (CFD) allow modeling everything from blood flow to aircraft aerodynamics, but high turbulence requires supercomputers.

In practice

Weather forecasts, wing aerodynamics calculations, climate modeling, and ocean current simulations — all are built on these equations.

Fun fact

The Clay Mathematics Institute has announced a $1 million prize for proving that solutions to the equations always exist and do not 'blow up' (remain smooth) in the three-dimensional case — it is one of the Millennium Prize problems.

Concept graph →

Formulas

$$\frac{d}{dy} \left( \eta \frac{dV}{dy} \right) = -\frac{F}{\rho}$$
Shear stress gradient balances body force in fluid flow.
What is in the formula
yvariablespatial coordinate perpendicular to flow — position metre
Vvariablefluid velocity in the flow direction — velocity metre per second
Fvariablebody force per unit volume acting on the fluid — force density newton per cubic metre
ρvariablefluid mass density — mass density kilogram per cubic metre
ηconstantdynamic viscosity of the fluid — dynamic viscosity = material-dependent pascal second
d/dyoperatorderivative with respect to y — ordinary derivative
\frac{d}{dy}(\eta_{xx}^{{nl}}\frac{dv}{dy})=-\frac{ee}{m} · 2606.27788
$$\frac{dP}{dr} = -\frac{G m(r) \rho(r)}{r^2} \left[1+\frac{P(r)}{\rho(r)c^2}\right] \left[1+\frac{4\pi r^3 P(r)}{m(r)c^2}\right] \left[1-\frac{2Gm(r)}{rc^2}\right]^{-1}$$
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
$$\frac{dP_r}{dr} = -\frac{G(\epsilon + P_r)(m + 4\pi r^3 P_r/c^2)}{c^2 r^2 (1 - 2Gm/(c^2 r))} + \frac{2(P_t - P_r)}{r}$$
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
$$\frac{dP}{dr} = -\frac{(P+\varepsilon)(m+4\pi r^3 P)}{r(r-2m)}$$
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

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