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The O9V star HD 46202, which is a member of the young open cluster NGC 2244,was observed by the CoRoT satellite in October/November 2008 during a short runof 34 days. From the very high-precision light curve, we clearly detect betaCep-like pulsation frequencies with amplitudes of ~0.1 mmag and below. Acomparison with stellar models was performed using a chi^2 as a measure for thegoodness-of-fit between the observed and theoretically computed frequencies.The physical parameters of our best-fitting models are compatible with the onesdeduced spectroscopically. A core overshooting parameter alpha_ov = 0.10 +-0.05 pressure scale height is required. None of the observed frequencies aretheoretically excited with the input physics used in our study. Moretheoretical work is thus needed to overcome this shortcoming in how weunderstand the excitation mechanism of pulsation modes in such a massive star.A similar excitation problem has also been encountered for certain pulsationmodes in beta Cep stars recently modelled asteroseismically.

An asteroseismic study of the O9V star HD 46202 from CoRoT space-based photometry