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 $2\,M_\odot$ 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 $|m\Omega_{\rm c}|$ with $m$ and $\Omega_{\rm c}$ 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.

中文翻译：

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旋转对流核心激发非径向脉动导致早型恒星的旋转调制

我们讨论了由共振耦合激发的低频 g 模式，在早型主序星的旋转对流核心中具有弱不稳定振荡​​对流模式。我们的非绝热脉动分析包括科里奥利力对 $2\,M_\odot$ 主序模型的影响表明，如果对流核心旋转得比周围辐射层稍快，辐射包络中的 g 模式会被共振激发耦合。惯性系中激发 g 模式的频率接近 $|m\Omega_{\rm c}|$，其中 $m$ 和 $\Omega_{\rm c}$ 是 g 模式的方位角阶次，分别为对流核心的旋转频率。这些 g 模式频率与在许多早型主序星中观察到的光度旋转调制和谐波的频率一致。