In fluid mechanics and astrophysics, the relativistic Euler equations are a generalization of the Euler equations that account for the effects of general relativity.
They have applications in high-energy astrophysics and numerical relativity, where they are commonly used for describing phenomena such as gamma-ray bursts, accretion phenomena, and neutron stars, often with the addition of a magnetic field.
[1] Note: for consistency with the literature, this article makes use of natural units, namely the speed of light
and the Einstein summation convention.
For most fluids observable on Earth, traditional fluid mechanics based on Newtonian mechanics is sufficient.
However, as the fluid velocity approaches the speed of light or moves through strong gravitational fields, or the pressure approaches the energy density (
), these equations are no longer valid.
[2] Such situations occur frequently in astrophysical applications.
For example, gamma-ray bursts often feature speeds only
less than the speed of light,[3] and neutron stars feature gravitational fields that are more than
times stronger than the Earth's.
[4] Under these extreme circumstances, only a relativistic treatment of fluids will suffice.
The equations of motion are contained in the continuity equation of the stress–energy tensor
is the total mass-energy density (including both rest mass and internal energy density) of the fluid,
is the fluid pressure,
[2] To the above equations, a statement of conservation is usually added, usually conservation of baryon number.
is the number density of baryons this may be stated
These equations reduce to the classical Euler equations if the fluid three-velocity is much less than the speed of light, the pressure is much less than the energy density, and the latter is dominated by the rest mass density.
To close this system, an equation of state, such as an ideal gas or a Fermi gas, is also added.
[1] In the case of flat space, that is
is the energy density of the system, with
Expanding out the sums and equations, we have, (using
to observe the behavior of the velocity itself, we see that the equations of motion become
Note that taking the non-relativistic limit, we have
This says that the energy of the fluid is dominated by its rest energy.
, and can see that we return the Euler Equation of
In order to determine the equations of motion, we take advantage of the following spatial projection tensor condition:
shows that the two completely cancel.
This cancellation is the expected result of contracting a temporal tensor with a spatial tensor.
This relativity-related article is a stub.