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We develop a numerical scheme for solving a fully special relativisticresistive radiation magnetohydrodynamics. Our code guarantees conservations oftotal mass, momentum and energy. Radiation energy density and radiation fluxare consistently updated using the M-1 closure method, which can resolve ananisotropic radiation fields in contrast to the Eddington approximation as wellas the flux-limited diffusion approximation. For the resistive part, we adopt asimple form of the Ohm's law. The advection terms are explicitly solved with anapproximate Riemann solver, mainly HLL scheme, and HLLC and HLLD schemes forsome tests. The source terms, which describe the gas-radiation interaction andthe magnetic energy dissipation, are implicitly integrated, relaxing theCourant-Friedrichs-Lewy condition even in optically thick regime or a largemagnetic Reynolds number regime. Although we need to invert $4\times 4$ (forgas-radiation interaction) and $3\times 3$ (for magnetic energy dissipation)matrices at each grid point for implicit integration, they are obtainedanalytically without preventing massive parallel computing. We show that ourcode gives reasonable outcomes in numerical tests for idealmagnetohydrodynamics, propagating radiation, and radiation hydrodynamics. Wealso applied our resistive code to the relativistic Petschek type magneticreconnection, revealing the reduction of the reconnection rate via theradiation drag.

Numerical Treatment of Anisotropic Radiation Field Coupling with the Relativistic Resistive Magnetofluids