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We present results of simulations of the spectrum of the accretion flow on to the supermassive black hole in our Galactic Centre, Sagittarius A*, generated with a coupling of Monte Carlo (MC) radiation and general relativistic magnetohydrodynamic codes. In our modelling, we use the two‐dimensional  harm grmhd  code to first model the physical parameters of the disc, then feed its results into our two‐dimensional MC photon transport code. We will discuss results obtained which fit radio, infrared and  Chandra ‐obtained flaring or quiescent X‐ray data points, as well as the validity of the amount of scaling of input parameters (density, temperature and magnetic field) required to fit these points.  harm  output will be used to suggest whether the scaling is within reasonable limits.

Monte Carlo simulations of the broad‐band spectra of Sagittarius A* through the use of general relativistic magnetohydrodynamics