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We estimate the amount of angular momentum transferred by the low-frequencyoscillations detected in the rapidly rotating hot Be star HD 51452. Here, weassume that the oscillations detected are stochastically excited by convectivemotions in the convective core of the star, that is, we treat the oscillationsas forced oscillations excited by the periodic convective motions of the corefluids having the frequencies observationally determined. With theobservational amplitudes of the photometric variations, we determine theoscillation amplitudes, which makes it possible to estimate the net amount ofangular momentum transferred by the oscillations using the wave-meanflowinteraction theory. Since we do not have any information concerning theazimuthal wavenumber $m$ and spherical harmonic degree $l$ for each of theoscillations, we assume that all the frequencies detected are prograde orretrograde in the observer's frame and they are all associated with a singlevalue of $m$ both for even modes ($l=|m|$) and for odd modes ($l=|m|+1$). Weestimate the amount of angular momentum transferred by the oscillations for$|m|=1$ and 2, which are typical $|m|$ values for Be stars, and find that theamount is large enough for a decretion disc to form around the star. Therefore,transport of angular momentum by waves stochastically excited in the core of Bestars might be responsible for the Be phenomenon.

Angular momentum transport by stochastically excited oscillations in rapidly rotating massive stars