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Strongly-magnetized ($B\geq10^{12}$ G) accreting neutron stars (NSs) areprime targets for studying the launching of jets by objects with a solidsurface; while classical jet-launching models predict that such NSs cannotlaunch jets, recent observations and models argue otherwise. Transient Be/X-raybinaries (BeXRBs) are critical laboratories for probing this poorly-exploredparameter space for jet formation. Here, we present the coordinated monitoringcampaigns of three BeXRBs across four outbursts: giant outbursts of SAX2103.5+4545, 1A 0535+262, and GRO J1008-57, as well as a Type-I outburst of thelatter. We obtain radio detections of 1A 0535+262 during ten out of twentyobservations, while the other targets remained undetected at typical limits of$20$-$50$ $\mu$Jy. The radio luminosity of 1A 0535+262 positively correlateswith its evolving X-ray luminosity, and inhabits a region of the $L_X$-$L_R$plane continuing the correlation observed previously for the BeXRB SwiftJ0243.6+6124. We measure a BeXRB $L_X$-$L_R$ coupling index of $\beta = 0.86\pm 0.06$ ($L_R \propto L_X^\beta$), similar to the indices measured in NS andblack hole low-mass X-ray binaries. Strikingly, the coupling's $L_R$normalisation is $\sim 275$ and $\sim 6.2\times10^3$ times lower than in thosetwo comparison samples, respectively. We conclude that jet emission likelydominates during the main peak of giant outbursts, but is only detectable forclose-by or super-Eddington systems at current radio sensitivities. We discussthese results in the broader context of X-ray binary radio studies, concludingthat our results suggest how supergiant X-ray binaries may host a currentlyunidentified additional radio emission mechanism.

Radio monitoring of transient Be/X-ray binaries and the inflow-outflow coupling of strongly-magnetized accreting neutron stars