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Through the years numerous attempts have been made to connect thephenomenology and physics of mass accretion onto stellar-mass and super-massiveblack holes in a scale-invariant fashion. In this paper, we explore thisconnection at the radiatively-efficient (and non-jetted) end of accretion modesby comparing the relationship between the luminosity of the accretion disk andcorona in the two source classes. We analyse 458 RXTE-PCA archival observationsof the X-ray binary (XRB) GX339-4 focusing on the soft and soft-intermediatestates, which have been suggested to be analogous to radiatively efficient AGN.The observed scatter in the $\log L_{disk}-\log L_{corona}$ relationship ofGX339-4 is high ($\sim0.43\,$dex) and significantly larger than in arepresentative sample of radiatively-efficient, non- or weakly-jetted AGN($\sim0.30\,$dex). On the face of it, this would appear contrary to thehypothesis that the systems simply scale with mass. On the other hand we alsofind that GX339-4 and our AGN sample show different $\dot{m}$ and $\Gamma$distributions, with the latter being broader in GX339-4 (dispersion of$\sim0.16$ cf. $\sim0.08$ for AGN). GX339-4 also shows an overall softer slope,with mean $\sim2.20$ as opposed to $\sim2.07$ for the AGN sample. Remarkably,once similarly broad $\Gamma$ and $\dot{m}$ distributions are selected, the AGNsample overlaps nicely with GX339-4 observations in the mass-normalised $\logL_{disk}-\log L_{corona}$ plane, with a scatter of $\sim0.30-0.33\,$dex. Thisindicates that a mass-scaling of properties might hold after all, with ourresults being consistent with the disk-corona systems in AGN and XRBsexhibiting the same physical processes, albeit under different conditions forinstance in terms of temperature, optical depth and/or electron energydistribution in the corona, heating-cooling balance, coronal geometry and/orblack hole spin.

Do stellar-mass and super-massive black holes have similar dining habits?