用数值模拟量化冷星的环境
Quantification of the environment of cool stars using numerical simulations
摘要：
恒星通过引力、辐射和磁场与行星相互作用。虽然磁活动随着时间的推移而减少，但减少了相关的高能量（例如，日冕XUV辐射，耀斑），恒星风持续整个系统的演变。它们的累积效应将对恒星和可能的轨道外行星起主导作用，以这种方式影响预期的可居住条件。然而，在低质量主序星的恒星风的观测是有限的，这促使使用模型作为一种途径，探索这些风看起来像什么，他们如何表现。在这里，我们提出的结果，从一个网格的三维国家的最先进的恒星风模型的冷恒星（光谱类型F到M）。我们探讨了不同的恒星属性（质量，半径，旋转，磁场）所产生的磁化风（质量和角动量损失，终端速度，风拓扑结构）的特性所发挥的作用，并隔离所涉及的参数之间的最重要的依赖关系。这些结果将被用来建立标度律，以补充缺乏恒星风观测约束。
英文摘要：
Stars interact with their planets through gravitation, radiation, and magnetic fields. Although magnetic activity decreases with time, reducing associated high-energy (e.g., coronal XUV emission, flares), stellar winds persist throughout the entire evolution of the system. Their cumulative effect will be dominant for both the star and for possible orbiting exoplanets, affecting in this way the expected habitability conditions. However, observations of stellar winds in low-mass main sequence stars are limited, which motivates the usage of models as a pathway to explore how these winds look like and how they behave. Here we present the results from a grid of 3D state-of-the-art stellar wind models for cool stars (spectral types F to M). We explore the role played by the different stellar properties (mass, radius, rotation, magnetic field) on the characteristics of the resulting magnetized winds (mass and angular momentum losses, terminal speeds, wind topology) and isolate the most important dependencies between the parameters involved. These results will be used to establish scaling laws that will complement the lack of stellar wind observational constraints.
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