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Understanding the Emission Region Geometry in Weakly Accreting Black Holes

Sera Markoff, University of Amsterdam

In the last several years, multiwavelength monitoring programs have allowed us to develop a general description of the observational characteristics of accreting black holes as they journey through their outburst cycles. Driven seemingly to a large extent by the accretion rate, these sources display an almost predictable series of physical changes which have been grouped into both transient and more stable accretion states. Despite the phenomenology, there is currently no consensus on the underlying physical picture for most of these states. However, a great deal of data are now available to help develop such a framework. In this poster I present some recent results from modeling the relatively stable hard accretion state, associated with a steady jet and predominantly non-thermal radio, IR/O and X-ray emission. By fitting multiple sources, including the AGN-equivalent of the hard state, low-luminosity AGN, we are able to construct a consistent physical picture of the hard state emission geometry. I discuss how we are using these results to form inputs for more sophisticated studies using simulations of \textsl{a priori} physics to study conditions for jet launching, as well as the time-dependent transition to the accretion disk-dominated soft state.