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Radio monitoring of transient Be/X-ray binaries and the inflow-outflow coupling of strongly-magnetized accreting neutron stars
J. van den Eijnden, N. Degenaar, T. D. Russell, J. C. A. Miller-Jones, A. Rouco Escorial, R. Wijnands, G. R. Sivakoff, J. V. Hernández Santisteban
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Strongly-magnetized (B≥10¹² G) accreting neutron stars (NSs) are prime targets for studying the launching of jets by objects with a solid surface; while classical jet-launching models predict that such NSs cannot launch jets, recent observations and models argue otherwise. Transient Be/X-ray binaries (BeXRBs) are critical laboratories for probing this poorly-explored parameter space for jet formation. Here, we present the coordinated monitoring campaigns of three BeXRBs across four outbursts: giant outbursts of SAX 2103.5+4545, 1A 0535+262, and GRO J1008-57, as well as a Type-I outburst of the latter. We obtain radio detections of 1A 0535+262 during ten out of twenty observations, while the other targets remained undetected at typical limits of $20$-$50$ μJy. The radio luminosity of 1A 0535+262 positively correlates with its evolving X-ray luminosity, and inhabits a region of the L_X-L_R plane continuing the correlation observed previously for the BeXRB Swift J0243.6+6124. We measure a BeXRB L_X-L_R coupling index of β= 0.86 ±0.06 (L_R ∝L_X^β), similar to the indices measured in NS and black hole low-mass X-ray binaries. Strikingly, the coupling's L_R normalisation is ∼275 and ∼6.2×10³ times lower than in those two comparison samples, respectively. We conclude that jet emission likely dominates during the main peak of giant outbursts, but is only detectable for close-by or super-Eddington systems at current radio sensitivities. We discuss these results in the broader context of X-ray binary radio studies, concluding that our results suggest how supergiant X-ray binaries may host a currently unidentified additional radio emission mechanism.
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