色球湍流作为恒星风质量通量的调节器
Chromospheric turbulence as a regulator of stellar wind mass flux
AI总结：
研究通过一维波驱动风模拟，探讨色球湍流对恒星风质量通量的调节作用，发现抑制色球湍流可使日冕粒子通量增加一个数量级，从而再现日冕磁场强度与质量通量的观测比例关系。
摘要：
太阳和恒星风的质量通量是恒星演化的关键量，但其物理调节机制仍是一个未解问题。特别是传统阿尔芬波驱动模型无法再现观测到的恒星X射线通量与质量损失率之间的比例关系，这主要归因于色球湍流耗散了大量波能量。为解决此问题，我们旨在明确色球湍流在调节恒星风质量通量中的作用。我们进行了单维波驱动风模拟，比较有无色球湍流抑制的案例，以评估其对日冕和风特性的影响。发现抑制色球湍流会导致日冕粒子通量系统性增加，进而使风质量通量增加一个数量级，尤其在中等强磁场区域。这种行为源于日冕基部的Poynting通量和渐近风速的变化。此外，抑制色球湍流的模型能再现日冕磁场强度与质量通量的观测比例关系，而无需引入如磁重联等额外能量输入机制。这些结果将色球湍流识别为调节恒星风质量通量的关键因素，并强调在连接恒星表面和恒星风的模型中纳入其影响的重要性。
英文摘要：
The mass flux of solar and stellar winds is a key quantity for stellar evolution and space weather, yet its physical regulation mechanism remains an unsolved problem. In particular, conventional Alfvén wave--driven models that self-consistently connect the stellar surface to the stellar wind fail to reproduce the observed scaling between stellar X-ray flux and mass-loss rate, a discrepancy that can be largely attributed to the dissipation of a substantial fraction of the wave energy by chromospheric turbulence. To address this issue, we aim to clarify the role of chromospheric turbulence in regulating the stellar wind mass flux. We perform one-dimensional wave-driven wind simulations, comparing cases with and without chromospheric turbulence suppression to assess its impact on coronal and wind properties. We find that suppressing chromospheric turbulence leads to a systematic increase in the coronal particle flux, and hence the wind mass flux, by up to an order of magnitude, particularly in regions of moderately strong magnetic field. This behavior arises from a combination of changes in the Poynting flux at the coronal base and in the asymptotic wind speed. Furthermore, the model with chromospheric turbulence suppression reproduces the observed empirical scaling between coronal magnetic field strength and mass flux without invoking additional energy input mechanisms such as interchange reconnection. These results identify the chromospheric turbulence as a key factor in regulating stellar wind mass flux and highlight the importance of incorporating its effects in models that connect the stellar surface and the stellar wind.
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