We argue that the solar g-modes are unlikely to have caused the discrete peaks in the power spectrum of the solar wind flux observed by Thomson et al (1995). The lower limit to the energy of individual g-modes, using the amplitudes given by Thomson et al., is estimated to be at least 10~(36) ergs for low-order g-modes; the resulting surface velocity amplitude is at least 50 cm s~(-1), larger than the observational upper limit (5 cm s~(-1)). We suggest that the most likely source for the excitation of solar g-modes is turbulent stresses in the convection zone. The surface velocity amplitude of low-degree and low-order g-modes resulting from this process is estimated to be of order 10~(-2) cm s~(-1). This amplitude is interestingly close to the detection threshold of the SOHO satellite. The long lifetime of g-modes (～10~6 yr for low-order modes) should be helpful in detecting these small-amplitude pulsations.
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机译：我们认为，Thomson等人（1995年）观察到的太阳g模式不太可能引起太阳风通量功率谱中的离散峰。使用Thomson等人给出的幅度，单个g模式能量的下限估计对于低阶g模式至少为10〜（36）erg。所得的表面速度振幅至少为50 cm s〜（-1），大于观测上限（5 cm s〜（-1））。我们建议最有可能激发太阳g模式的原因是对流区内的湍流应力。由此过程产生的低阶和低阶g模的表面速度振幅估计为10〜（-2）cm s〜（-1）。有趣的是，该幅度接近SOHO卫星的检测阈值。 g模式的使用寿命长（低阶模式约为10〜6 yr）应有助于检测这些小幅度脉动。
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