As one of the most violent activities in the solar atmosphere, white-light flares (WLFs) are generally known for their enhanced white-light (or continuum) emission, which primarily originates in the solar lower atmosphere. However, we know little about how white-light emission is produced. In this study, we aim to investigate the response of the continua at 3600 and 4250 and also the Hα and Lyα lines during WLFs modeled using radiative hydrodynamic simulations. We take non-thermal electron beams as the energy source for the WLFs in two different initial atmospheres and vary their parameters. Our results show that the model with non-thermal electron beam heating clearly shows enhancements in the continua at 3600 and 4250 as well as in the Hα and Lyα lines. A larger electron beam flux, a smaller spectral index, or an initial penumbral atmosphere leads to a stronger emission increase at 3600 , 4250 and in the Hα line. The Lyα line, however, is more obviously enhanced in a quiet-Sun initial atmosphere with a larger electron beam spectral index. It is also notable that the continua at 3600 and 4250 and the Hα line exhibit a dimming at the start of heating and reach their peak emissions after the peak time of the heating function, while the Lyα line does not show such behaviors. These results can serve as a reference for the analysis of future WLF observations.

作为太阳大气中最剧烈的活动之一，白光耀斑 (WLF) 通常以其增强的白光（或连续谱）发射而闻名，其主要起源于太阳低层大气。然而，我们对白光发射是如何产生的知之甚少。在这项研究中，我们旨在研究连续波在 3600 和 4250 处的响应，以及在使用辐射流体动力学模拟建模的 WLF 期间的 Hα和Lyα谱线。我们将非热电子束作为 WLFs 在两种不同初始大气中的能源并改变它们的参数。我们的结果表明，具有非热电子束加热的模型清楚地显示了 3600 和 4250 的连续波以及 H α和 Ly的增强α线。较大的电子束通量、较小的光谱指数或初始半影大气导致在 3600、4250 和 H α线处的发射增加更强。然而，在具有较大电子束光谱指数的安静的太阳初始大气中， Ly α线更明显地增强。还值得注意的是，3600 和 4250 处的连续谱以及 H α线在加热开始时表现出调光，并在加热函数的峰值时间后达到其峰值排放，而 Ly α线没有表现出这种行为。这些结果可以作为未来WLF观测分析的参考。