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Fig. 4


Flux variation over the orbital period of AR Sco. Data pointsrepresents integration over a 10 min interval (15 min at 9 GHz), sufficient to average over the 2 min beat period flux variation. Results are shown for 1 GHz bands centred at 1.5, 4.5, 5.5, 8.5 and 9.5 GHz. The data are phase-foldedin the interval between 0 and 1, and repeated between 1 and 2 for clarity. For comparison we also show the W1m optical data as small points in the bottom two lines. The optical data in each observation have been phase folded and the mean in each phase bin calculated; their fluxes are arbitrarily scaled to indicate orbital phase and shape in the optical. Where more than one point occurs at a given frequency and phase, it indicates measurements in different orbits.

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