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Motivated by the recent detection of stochastically excited modes in themassive star V1449 Aql (Belkacem et al., 2009b), already known to be a $\beta$Cephei, we theoretically investigate the driving by turbulent convection. Byusing a full non-adiabatic computation of the damping rates, together with acomputation of the energy injection rates, we provide an estimate of theamplitudes of modes excited by both the convective region induced by the ironopacity bump and the convective core. Despite uncertainties in the dynamicalproperties of such convective regions, we demonstrate that both are able toefficiently excite $p$ modes above the CoRoT observational threshold and thesolar amplitudes. In addition, we emphasise the potential asteroseismicdiagnostics provided by each convective region, which we hope will help toidentify the one responsible for solar-like oscillations, and to giveconstraints on this convective zone. A forthcoming work will be dedicated to anextended investigation of the likelihood of solar-like oscillations across theHertzsprung-Russell diagram.

Solar-like oscillations in massive main-sequence stars. I. Asteroseismic signatures of the driving and damping regions