  During outbursts, the observational properties of black hole X-ray binaries
(BHXBs) vary on timescales of days to months. These relatively short timescales
make these systems ideal laboratories to probe the coupling between accreting
material and outflowing jets as a the accretion rate varies. In particular, the
origin of the hard X-ray emission is poorly understood and highly debated. This
spectral component, which has a power-law shape, is due to Comptonisation of
photons near the black hole, but it is unclear whether it originates in the
accretion flow itself, or at the base of the jet, or possibly the interface
region between them. In this paper we explore the disk-jet connection by
modelling the multi-wavelength emission of MAXI J1836-194 during its 2011
outburst. We combine radio through X-ray spectra, X-ray timing information, and
a robust joint-fitting method to better isolate the jet's physical properties.
Our results demonstrate that the jet base can produce power-law hard X-ray
emission in this system/outburst, provided that its base is fairly compact and
that the temperatures of the emitting electrons are sub-relativistic. Because
of energetic considerations, our model favours mildly pair-loaded jets carrying
at least 20 pairs per proton. Finally, we find that the properties of the X-ray
power spectrum are correlated with the jet properties, suggesting that an
underlying physical process regulates both.
