Euler equations


 * This page discusses classical compressible fluid flow. For other uses, see Euler function (disambiguation).

In fluid dynamics, the Euler equations govern the compressible, inviscid flow. They correspond to the Navier-Stokes equations with zero viscosity and heat conduction terms. They are usually written in the conservation form shown below to emphasize that they directly represent conservation of mass, momentum, and energy. The equations are named after Leonhard Euler.

This page assumes that classical mechanics applies; see relativistic Euler equations for a discussion of compressible fluid flow when velocities approach the speed of light.

Euler equations in conservation and component form
In differential form, the equations are:



\begin{align} &{\partial\rho\over\partial t}+ \nabla\cdot(\rho\bold u)=0\\[1.2ex] &{\partial\rho{\bold u}\over\partial t}+ \nabla\cdot(\bold u\otimes(\rho \bold \bold u))+\nabla p=0\\[1.2ex] &{\partial E\over\partial t}+ \nabla\cdot(\bold u(E+p))=0, \end{align} $$

where The second equation includes the divergence of a dyadic product, and may be clearer in subscript notation; for each j from 1 to 3 one has:
 * &rho; is the fluid mass density,
 * u is the fluid velocity vector, with components u, v, and w,
 * E = &rho; e + ½ &rho; ( u2 + v2 + w2 ) is the total energy per unit volume, with e is the internal energy per unit mass for the fluid, and
 * p is the pressure.

{\partial(\rho u_j)\over\partial t}+ \sum_{i=1}^3 {\partial(\rho u_i u_j)\over\partial x_i}+ {\partial p\over\partial x_j} =0, $$ where the i and j subscripts label the three Cartesian components: ( x1, x2 , x3 ) = ( x , y , z ) and ( u1 , u2 , u3 ) = ( u , v , w ).

Note that the above equations are expressed in conservation form, as this format emphasizes their physical origins (and is often the most convenient form for computational fluid dynamics simulations). The second equation, which represents momentum conservation, can also be expressed in non-conservation form as:



\rho\left( \frac{\partial}{\partial t}+{\bold u}\cdot\nabla \right){\bold u}+\nabla p=0 $$

but this form obscures the direct connection between the Euler equations and Newton's second law of motion.

Euler equations in conservation and vector form
In vector and conservation form, the Euler equations become:



\frac{\partial \bold m}{\partial t}+ \frac{\partial \bold f_x}{\partial x}+ \frac{\partial \bold f_y}{\partial y}+ \frac{\partial \bold f_z}{\partial z}=0, $$

where



{\bold m}=\begin{pmatrix}\rho \\  \rho u  \\  \rho v  \\ \rho w  \\E\end{pmatrix}\qquad {\bold f_x}=\begin{pmatrix}\rho u\\p+\rho u^2\\ \rho uv \\ \rho uw\\u(E+p)\end{pmatrix}\qquad {\bold f_y}=\begin{pmatrix}\rho v\\ \rho uv \\p+\rho v^2\\ \rho vw \\v(E+p)\end{pmatrix}\qquad {\bold f_z}=\begin{pmatrix}\rho w\\ \rho uw \\  \rho vw \\p+\rho w^2\\w(E+p)\end{pmatrix}. $$

This form makes it clear that fx, fy and fz are fluxes.

The equations above thus represent conservation of mass, three components of momentum, and energy. There are thus five equations and six unknowns. Closing the system requires an equation of state; the most commonly used is the ideal gas law (i.e. p = &rho; (&gamma;-1) e, where ρ is the density, &gamma; is the adiabatic index, and e the internal energy).

Note the odd form for the energy equation; see Rankine-Hugoniot equation. The extra terms involving p may be interpreted as the mechanical work done on a fluid element by its neighbor fluid elements. These terms sum to zero in an incompressible fluid.

The well-known Bernoulli's equation can be derived by integrating Euler's equation along a streamline, under the assumption of constant density and a sufficiently stiff equation of state.

Euler equations in non-conservation form with flux Jacobians
Expanding the fluxes can be an important part of constructing numerical solvers, for example by exploiting (approximate) solutions to the Riemann problem. From the original equations as given above in vector and conservation form, the equations are written in a non-conservation form as:



\frac{\partial \bold m}{\partial t} + \bold A_x \frac{\partial \bold m}{\partial x} + \bold A_y \frac{\partial \bold m}{\partial y} + \bold A_z \frac{\partial \bold m}{\partial z} = 0. $$

where Ax, Ay and Az are called the flux Jacobians, which are matrices equal to:



\bold A_x=\frac{\partial \bold f_x(\bold s)}{\partial \bold s}, \qquad \bold A_y=\frac{\partial \bold f_y(\bold s)}{\partial \bold s} \qquad \text{and} \qquad \bold A_z=\frac{\partial \bold f_z(\bold s)}{\partial \bold s}. $$

Here, the flux Jacobians Ax, Ay and Az are still functions of the state vector m, so this form of the Euler equations is nonlinear, just like the original equations. This non-conservation form is equivalent to the original Euler equations in conservation form, at least in regions where the state vector m varies smoothly.

Flux Jacobians for an ideal gas
The ideal gas law is used as the equation of state, to derive the full Jacobians in matrix form, as given below :


 * {| class="toccolours collapsible collapsed" width="80%" style="text-align:left"

! Flux Jacobians in matrix form for an ideal gas
 * The x-direction flux Jacobian:
 * The x-direction flux Jacobian:



\bold A_x= \left[ \begin{array}{c c c c c} 0 & 1 & 0 & 0 & 0 \\ \hat{\gamma}H-u^2-a^2 & (3-\gamma)u & -\hat{\gamma}v & -\hat{\gamma}w & \hat{\gamma} \\ -uv & v & u & 0 & 0 \\ -uw & w & 0 & u & 0 \\ u[(\gamma-2)H-a^2] & H-\hat{\gamma}u^2 & -\hat{\gamma}uv & -\hat{\gamma}uw & \gamma u \end{array} \right]. $$

The y-direction flux Jacobian:



\bold A_y= \left[ \begin{array}{c c c c c} 0 & 0 & 1 & 0 & 0 \\ -vu & v & u & 0 & 0 \\ \hat{\gamma}H-v^2-a^2 & -\hat{\gamma}u & (3-\gamma)v & -\hat{\gamma}w & \hat{\gamma} \\ -vw & 0 & w & v & 0 \\ v[(\gamma-2)H-a^2] & -\hat{\gamma}uv & H-\hat{\gamma}v^2 & -\hat{\gamma}vw & \gamma v \end{array} \right]. $$

The z-direction flux Jacobian:



\bold A_z= \left[ \begin{array}{c c c c c} 0 & 0 & 0 & 1 & 0 \\ -uw & w & 0 & u & 0 \\ -vw & 0 & w & v & 0 \\ \hat{\gamma}H-w^2-a^2 & -\hat{\gamma}u  & -\hat{\gamma}v & (3-\gamma)w& \hat{\gamma} \\ w[(\gamma-2)H-a^2] & -\hat{\gamma}uw  & -\hat{\gamma}vw & H-\hat{\gamma}w^2 & \gamma w \end{array} \right]. $$ Where $$\hat{\gamma}=\gamma-1$$.
 * }

The total enthalpy H is given by:



H = \frac{E+p}{\rho}, $$

and the speed of sound a is given as:



a=\sqrt{\frac{\gamma p}{\rho}} = \sqrt{(\gamma-1)\left[H-\frac{1}{2}\left(u^2+v^2+w^2\right)\right]}. $$

Linearized form
The linearized Euler equations are obtained by linearization of the Euler equations in non-conservation form with flux Jacobians, around a state m = m0, and are given by:



\frac{\partial \bold m}{\partial t} + \bold A_{x,0} \frac{\partial \bold m}{\partial x} + \bold A_{y,0} \frac{\partial \bold m}{\partial y} + \bold A_{z,0} \frac{\partial \bold m}{\partial z} = 0, $$

where Ax,0, Ay,0 and Az,0 are the values of respectively Ax, Ay and Az at some reference state m = m0.

Transformation to uncoupled wave equations for the one-dimensional case
The Euler equations can be transformed into uncoupled wave equations if they are expressed in characteristic variables instead of conserved variables. As an example, the one-dimensional (1-D) Euler equations in linear flux-Jacobian form is considered:



\frac{\partial \bold m}{\partial t} + \bold A_{x,0} \frac{\partial \bold m}{\partial x} =0. $$

The matrix Ax,0 is diagonalizable, which means it can be decomposed into:



\mathbf{A}_{x,0} = \mathbf{P} \mathbf{\Lambda} \mathbf{P}^{-1}, $$



\mathbf{P}= \left[\bold r_1, \bold r_2, \bold r_3\right] =\left[ \begin{array}{c c c} 1 & 1 & 1 \\ u-a & u & u+a \\ H-u a & \frac{1}{2} u^2 & H+u a \\ \end{array} \right], $$



\mathbf{\Lambda} = \begin{bmatrix} \lambda_1 & 0 & 0 \\ 0 & \lambda_2 & 0 \\ 0 & 0 & \lambda_3 \\ \end{bmatrix} = \begin{bmatrix} u-a & 0 & 0 \\ 0 & u & 0 \\ 0 & 0 & u+a \\ \end{bmatrix}. $$

Here r1, r2, r3 are the right eigenvectors of the matrix Ax,0 corresponding with the eigenvalues &lambda;1, &lambda;2 and &lambda;3.

Defining the characteristic variables as:


 * $$\mathbf{w}= \mathbf{P}^{-1}\mathbf{m},$$

Since Ax,0 is constant, multiplying the original 1-D equation in flux-Jacobian form with P-1 yields:



\frac{\partial \mathbf{w}}{\partial t} + \mathbf{\Lambda} \frac{\partial \mathbf{w}}{\partial x} = 0 $$

The equations have been essentially decoupled and turned into three wave equations, with the eigenvalues being the wave speeds. The variables wi are called Riemann invariants or, for general hyperbolic systems, they are called characteristic variables.

Shock waves
The Euler equations are nonlinear hyperbolic equations and their general solutions are waves. Much like the familiar oceanic waves, waves described by the Euler Equations 'break' and so-called shock waves are formed; this is a nonlinear effect and represents the solution becoming multi-valued. Physically this represents a breakdown of the assumptions that led to the formulation of the differential equations, and to extract further information from the equations we must go back to the more fundamental integral form. Then, weak solutions are formulated by working in 'jumps' (discontinuities) into the flow quantities - density, velocity, pressure, entropy - using the Rankine-Hugoniot shock conditions. Physical quantities are rarely discontinuous; in real flows, these discontinuities are smoothed out by viscosity. (See Navier-Stokes equations)

Shock propagation is studied — among many other fields — in aerodynamics and rocket propulsion, where sufficiently fast flows occur.

The equations in one spatial dimension
For certain problems, especially when used to analyze compressible flow in a duct or in case the flow is cylindrically or spherically symmetric, the one-dimensional Euler equations are a useful first approximation. Generally, the Euler equations are solved by Riemann's method of characteristics. This involves finding curves in plane of independent variables (i.e., x and t) along which partial differential equations (PDE's) degenerate into ordinary differential equations (ODE's). Numerical solutions of the Euler equations rely heavily on the method of characteristics.