Speaker
Description
Simulations of black hole X-ray binary systems (BHXRBs) can help us understand physical changes in these systems as an outburst occurs. Here, we present the first three-dimensional GRMHD simulations of created using the H-AMR code of a low mass X-ray binary undergoing a spectral state transition, both in the MAD (magnetically arrested disk) and SANE (standard and normal evolution) models. These simulations range over many luminosities in a manner similar to the evolution of an outburst, from 10^-17 to 10^-3 Eddington Luminosity. The Monte Carlo ray-tracing code RAPTOR is then used to create spectra based on Compton, synchrotron, and bremsstrahlung photons. These spectra help illustrate the physical structure of the system at a given time and compare to quantities such as the amount of magnetic flux present in the system. In this talk, we will present analysis on these MAD and SANE BHXRB systems and share how quantities such as magnetic flux affect the proceedings of an outburst, as well as discuss development of the ray-tracing code. We will present changes in the spectra that highlight physical changes in the BHXRB system as well as the power spectra. Through comparisons of these two, we can narrow down potential origin sources of variability.