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OB stars are important constituents for the ecology of the Universe, andthere are only a few studies on their pulsational properties detailed enough toprovide important feedback on current evolutionary models. Our goal is toanalyse and interpret the behaviour present in the CoRoT light curve of theB0.5 IV star HD 51756 observed during the second long run of the space mission,and to determine the fundamental stellar parameters from ground-basedspectroscopy gathered with the CORALIE and HARPS instruments after checking forsigns of variability and binarity, thus making a step further in mapping thetop of the Beta Cep instability strip. We compare the newly obtainedhigh-resolution spectra with synthetic spectra of late O-type and early B-typestars computed on a grid of stellar parameters. We match the results withevolutionary tracks to estimate stellar parameters. We use various time seriesanalysis tools to explore the nature of the variations present in the lightcurve. Additional calculations are carried out based on distance and historicalposition measurements of the components to impose constraints on the binaryorbit. We find that HD 51756 is a wide binary with both a slow (v sin i \approx28 km s^-1) and a fast (v sin i \approx 170 km s^-1) early-B rotator whoseatmospheric parameters are similar (T_eff \approx 30000 K and log g \approx3.75). We are unable to detect pulsation in any of the components, and weinterpret the harmonic structure in the frequency spectrum as sign ofrotational modulation, which is compatible with the observed and deducedstellar parameters of both components. The non-detection of pulsation modesprovides a feedback on the theoretical treatment, given that non-adiabaticcomputations applied to appropriate stellar models predict the excitation ofboth pressure and gravity modes for the fundamental parameters of this star.

CoRoT high-precision photometry of the B0.5 IV star HD 51756