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Observations of the black hole X-ray binaries GX 339-4 and V404 Cygni havebrought evidence of a strong correlation between radio and X-ray emissionduring the hard spectral state; however, now more and more sources, theso-called `outliers', are found with a radio emission noticeably below theestablished `standard' relation. Several explanations have already beenconsidered, but the existence of dual tracks is not yet fully understood.  We suggest that in the hard spectral state re-condensation of gas from thecorona into a cool, weak inner disk can provide additional soft photons forComptonization, leading to a higher X-ray luminosity in combination with ratherunchanged radio emission, which presumably traces the mass accretion rate. Asan example, we determined how much additional luminosity due to photons from anunderlying disk would be needed to explain the data from the representativeoutlier source H1743-322. From the comparison with calculations of Comptonspectra with and without the photons from an underlying disk, we find that therequired additional X-ray luminosity lies well in the range obtained fromtheoretical models of the accretion flow. The radio/X-ray luminosity relationresulting from Comptonization of additional photons from a weak, cool innerdisk during the hard spectral state can explain the observations of the outliersources, especially the data for H1743-322, the source with the most detailedobservations. The existence or non-existence of weak inner disks on the twotracks might point to a difference in the magnetic fields of the companionstars. These could affect the effective viscosity and the thermal conductivity,hence also the re-condensation process.

The relation between radio and X-ray luminosity of black hole binaries: affected by inner cool disks?