Top panel: logarithmic power density spectrum of the CoRoT photometry for the O star HD 46150 is shown in black, and the best-fit model obtained using Eq. (1) is shown as the solid green line, with its red and white components shown as red short-dashed and blue long-dashed lines, respectively. Middle panel: posterior distributions from the Bayesian MCMC, with best-fit parameters obtained from Gaussian fits (shown in black) to the 1D histograms (shown in blue). Bottom panel: a sliding Fourier transform in the (linear) frequency range of 0 ≤ ν ≤ 4 d⁻¹ using a 15-d bin and a step of 0.1 d.