  We investigate the relation between the two modes of outflow (wind and jet)
in radio-loud active galactic nuclei (AGN). For this study we have carried out
a systematic and homogeneous analysis of XMM-Newton spectra of a sample of 16
suitable radio-loud Seyfert-1 AGN. The ionised winds in these AGN are
parameterised through high-resolution X-ray spectroscopy and photoionisation
modelling. We discover a significant inverse correlation between the column
density NH of the ionised wind and the radio-loudness parameter R of the jet.
We explore different possible explanations for this NH-R relation and find that
ionisation, inclination, and luminosity effects are unlikely to be responsible
for the observed relation. We argue that the NH-R relation is rather a
manifestation of the magnetic driving mechanism of the wind from the accretion
disk. Change in the magnetic field configuration from toroidal to poloidal,
powering either the wind or the jet mode of the outflow, is the most feasible
explanation for the observed decline in the wind NH as the radio jet becomes
stronger. Our findings provide evidence for a wind-jet bimodality in radio-loud
AGN and shine new light on the link between these two modes of outflow. This
has far-reaching consequences for the accretion disk structure and the wind
ejection mechanism.
