Title: Accretion and ejection around black hole binaries: the role of viscosity and cooling
Abstract: Accreting black hole binaries (BHBs) are powerful X-ray emitters. The X-ray flux arises from two key accretion flow components: the geometrically thin standard accretion disk and its X-ray corona. The phenomenology of X-ray observations of BHBs is very rich and has been exhaustively studied. To date, however, there is a little agreement on the physics behind these accretion states. To go beyond the standard model of a stable accretion flow, with no corona and only a parametric viscosity of unknown origin, it is necessary to rely on a promising physical solution. Here I will discuss the flow solution to fit the observation of several black hole binaries from different satellites. The importance of the cooling and viscosity in triggering different spectral states will also be discussed.