Speaker
Description
We present a framework that combines state-of-the-art three-dimensional general relativistic magnetohydrodynamic (3D GRMHD) simulations with radiative transfer calculations to directly compare theoretical predictions with multiwavelength observations of Galactic black hole transients (GBHT). Using the H-AMR code, we simulate black hole accretion flows in both SANE and MAD magnetic configurations across different Eddington-scaled luminosities. To emulate outburst evolution, we apply a rescaling prescription that artificially shortens relevant accretion timescales while preserving the physical relationships between density, magnetic field, and radiation energy densities.
Simulation outputs are post-processed with the RAPTOR ray-tracing code to generate synchrotron and synchrotron self-Compton (SSC) spectra, light curves, and synthetic images. We further employ SIXTE to produce X-ray spectra corresponding to current and future observatories, enabling direct observational comparisons. Our framework will enable the reconstruction of hardness–intensity diagram from first-principles simulations and opens a pathway toward studying timing properties, variability, and state transitions in unprecedented detail.
In this presentation, we will report on initial results (SEDs, X-ray spectra, synthetic images) below 10^-5 Eddington Luminosity, and report on future improvements to the current framework. The X-ray spectra at low luminosities reproduce photon indices consistent with observed GBHT populations. Three-dimensional reconstructions of emission regions show that synchrotron photons predominantly originate near the event horizon and the jet sheath, while SSC photons are produced over a broader spatial extent.