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Accreting stellar-mass black holes appear to populate two branches in aradio:X-ray luminosity plane. We have investigated the X-ray variabilityproperties of a large number of black hole low-mass X-ray binaries, with theaim of unveiling the physical reasons underlying the radio-loud/radio-quietnature of these sources, in the context of the known accretion-ejectionconnection. A reconsideration of the available radio and X-ray data from asample of black hole X-ray binaries confirms that being radio-quiet is the morenormal mode of behaviour for black hole binaries. In the light of this we choseto test, once more, the hypothesis that radio loudness could be a consequenceof the inclination of the X-ray binary. We compared the slope of the`hard-line' (an approximately linear correlation between X-ray count rate andrms variability, visible in the hard states of active black holes), the orbitalinclination, and the radio-nature of the sources of our sample. We found thathigh-inclination objects show steeper hard-lines than low-inclination objects,and tend to display a radio-quiet nature (with the only exception of V404 Cyg),as opposed to low-inclination objects, which appear to be radio-loud(er). Whilein need of further confirmation, our results suggest that - contrary to whathas been believed for years - the radio-loud/quiet nature of black-hole lowmass X-ray binaries might be an inclination effect, rather than an intrinsicsource property. This would solve an important issue in the context of theinflow-outflow connection, thus providing significant constraints to the modelsfor the launch of hard-state compact jets.

Radio-loudness in black hole transients: evidence for an inclination effect