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Motivated by the large body of literature around the phenomenologicalproperties of accreting black hole (BH) and neutron star (NS) X-ray binaries inthe radio:X-ray luminosity plane, we carry out a comparative regressionanalysis on 36 BHs and 41 NSs in hard X-ray states, with data over 7 dex inX-ray luminosity for both. The BHs follow a radio to X-ray (logarithmic)luminosity relation with slope $\beta=0.59\pm0.02$, consistent with the NSs'slope ($\beta=0.44^{+0.05}_{-0.04}$) within 2.5$\sigma$. The best-fittingintercept for the BHs significantly exceeds that for the NSs, cementing BHs asmore radio loud, by a factor $\sim$22. \This discrepancy can not be fullyaccounted for by the mass or bolometric correction gap, nor by the NS boundarylayer contribution to the X-rays, and is likely to reflect physical differencesin the accretion flow efficiency, or the jet powering mechanism. Onceimportance sampling is implemented to account for the different luminositydistributions, the slopes of the non-pulsating and pulsating NS subsamples areformally inconsistent ($>3\sigma$), unless the transitional millisecond pulsars(whose incoherent radio emission mechanism is not firmly established) areexcluded from the analysis. We confirm the lack of a robust partitioning of theBH data set into separate luminosity tracks.

Hard state neutron star and black hole X-ray binaries in the radio:X-ray luminosity plane