Rotating Convective Core Excites Non-Radial Pulsations to Cause Rotational Modulations in Early-Type Stars

Abstract

We discuss low-frequency g modes excited by resonant couplings with weakly unstable oscillatory convective modes in the rotating convective core in early-type main-sequence stars. Our non-adiabatic pulsation analyses including the effect of Coriolis force for $2M_{\odot }$ main-sequence models show that if the convective core rotates slightly faster than the surrounding radiative layers, g modes in the radiative envelope are excited by a resonance coupling. The frequency of the excited g mode in the inertial frame is close to $|m{\Omega }_{\mathrm{c}}|$ with $m$ and ${\Omega }_{\mathrm{c}}$ being the azimuthal order of the g mode and the rotation frequency of the convective core, respectively. These g mode frequencies are consistent with those of photometric rotational modulations and harmonics observed in many early-type main-sequence stars.

accepted for publication in MNRAS; 12 pages, 15 figures

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