Relativistic Euler equations

Summary

The relativistic Euler equations describe a perfect fluid, without viscosity or heat conduction, in special or general relativity. They state that the energy–momentum tensor of the fluid and the number of its particles are conserved. They reduce to the classical Euler equations when speeds are small compared with the speed of light and pressure is small compared with energy density. They model fluids in astrophysics, such as neutron stars, accretion flows and the early universe, and the quark–gluon plasma of heavy-ion collisions.