标题： 冷却主序星风特性的数值量化 显示英文标题

标题： Numerical quantification of the wind properties of cool main sequence stars

摘要： 当一颗冷星演化时，它会由于磁化恒星风而损失质量和角动量，这会影响它的旋转演化。 这种变化的影响范围从其活动性的改变到对环绕行星大气层的影响。 尽管它们非常重要，但限制冷星恒星风特性的观测数据非常有限。 因此，数值模拟提供了一种理解这些风的结构和特性的有价值方法。 在本工作中，我们使用一种先进的三维MHD代码，通过观测到的大尺度磁场分布，模拟了21颗冷主序星（F型至M型矮星）的磁化风。 我们对解决方案进行了定性和定量的表征，分析了驱动条件（例如光谱类型、旋转、磁场强度）与产生的恒星风参数（例如阿尔芬表面大小、质量损失率、角动量损失率、恒星风速度）之间的依赖关系。 我们将我们的模型与当前关于冷星恒星风的观测知识进行比较，并探讨质量损失率随罗西比数的变化行为。 此外，我们的三维模型涵盖了我们样本中所有恒星的经典宜居带（HZ）。 这使我们能够在HZ的两侧提供恒星风的动态压力，并分析该参数在光谱类型和轨道倾角上的变化。 这里呈现的结果可以用于为未来的恒星风-磁层相互作用研究和通过离子逃逸过程的恒星风对行星大气层的侵蚀研究提供参考。 显示英文摘要

摘要： As a cool star evolves, it loses mass and angular momentum due to magnetized stellar winds which affect its rotational evolution. This change has consequences that range from the alteration of its activity to influences over the atmosphere of any orbiting planet. Despite their importance, observations constraining the properties of stellar winds in cool stars are extremely limited. Therefore, numerical simulations provide a valuable way to understand the structure and properties of these winds. In this work, we simulate the magnetized winds of 21 cool main-sequence stars (F-type to M-dwarfs), using a state-of-the-art 3D MHD code driven by observed large-scale magnetic field distributions. We perform a qualitative and quantitative characterization of our solutions, analyzing the dependencies between the driving conditions (e.g., spectral type, rotation, magnetic field strength) and the resulting stellar wind parameters (e.g., Alfv\'en surface size, mass loss rate, angular momentum loss rate, stellar wind speeds). We compare our models with the current observational knowledge on stellar winds in cool stars and explore the behaviour of the mass loss rate as a function of the Rossby number. Furthermore, our 3D models encompass the entire classical Habitable Zones (HZ) of all the stars in our sample. This allows us to provide the stellar wind dynamic pressure at both edges of the HZ and analyze the variations of this parameter across spectral type and orbital inclination. The results here presented could serve to inform future studies of stellar wind-magnetosphere interactions and stellar wind erosion of planetary atmospheres via ion escape processe.