Fluid description of relativistic, magnetized plasma

Many astrophysical plasmas and some laboratory plasmas are relativistic: either the thermal speed or the local ow speed (in a convenient frame) approaches the speed of light. Many such plasmas are also magnetized, in the sense that the thermal Larmor radius is smaller than gradient scale lengths. Relativistic MHD, conventionally used to describe such systems, requires the collision time to be shorter than any other time{scale in the system. On this assumption it uses the thermodynamic equilibrium form of the plasma pressure tensor, neglecting stress anisotropy as well as heat ow along the magnetic eld. Beginning with exact moments of the kinetic equation, we derive a closed set of Lorentz{covariant uid equations that allows for anisotropy and heat ow, as would pertain to a collisionless plasma, far from thermodynamic equilibrium. The heart of the derivation is the construction of the plasma stress tensor as the fully general solution to the energy{momentum conservation law in the case of dominant electromagnetic force. Subject headings: stars: atmospheres, galaxies: jets, methods: analytical, physical data and processes, relativistic plasmas