SKA continuum surveys at low frequencies (< 1 GHz) should be ideal to probe the cosmic radio dipole already in the Early Science phase for two reasons. First, it is not necessary to cover the full area of the 3π surveys, since a sparse sampling spread out over all of the accessible sky should be sufficient for a first estimate. And second, a focus on low frequencies and bright sources will pick primarily AGNs which have a much higher mean redshift than the SFG. Figure 1 illustrates the accuracy that we can hope to achieve for a measurement of the radio dipole based on a linear estimator (Crawford 2009;Rubart & Schwarz 2013). Our estimates are based on differential number counts from surveys in small and deep fields and simulations (Wilman et al. 2008). Our expectations for all-sky continuum surveys are summarized in Table 1. We find that the cosmic radio dipole can be measured at high statistical significance, even taking realistic **data** cuts into account (e.g. masking the galaxy and very bright extragalactic sources, or morphology, spectral index or flux cuts).