模拟行星恒星周围的环境- II。恒星风和内部天体层
Simulating the environment around planet-hosting stars - II. Stellar winds and inner astrospheres
摘要：
我们提出了一个全面的数值模拟的结果，周围的环境三个系外行星宿主恒星（HD 1237，HD 22049和HD 147513）。我们的模拟考虑了目前用于日光层空间天气研究的最新模型之一。大规模的磁场地图，恢复与塞曼多普勒成像的层析成像技术的两个实现，用于驱动每个系统中的稳态解决方案。这篇论文包含了对恒星风和内部天体层的描述，而日冕结构之前在Alvarado-Gómez et al.（2016）中进行了讨论。分析包括恒星风的磁流体动力学性质，相关的质量和角动量损失率，以及每个系统中的天体层电流片的拓扑结构。所考虑的情况下，包括两个参考太阳模拟活动的最小值和最大值之间进行了系统的比较。对于HD 1237，我们研究了发达的恒星风的结构之间的相互作用，和一个可能的磁层在这个系统中的行星周围的质量。我们发现，粒子注入到行星大气的过程是由星风的密度分布而不是速度分布决定的。在这种情况下，我们预测在这个系统中，在40 MHz的最大系外行星无线电发射12毫焦耳，假设在近星点通道的高密度流光的交叉。此外，结合Alvarado-Gómez等人（2016）进行的分析，我们首次获得了完全模拟的质量损失-活动关系，并在Wood等人（2005 a）提出的基于天体层探测的关系的背景下进行了比较和讨论。最后，我们提供了这些系统的恒星风的三维特性的表征，在其宜居带的内部边缘。
英文摘要：
We present the results of a comprehensive numerical simulation of the environment around three exoplanet-host stars (HD 1237, HD 22049, and HD 147513). Our simulations consider one of the latest models currently used for space weather studies in the Heliosphere. Large-scale magnetic field maps, recovered with two implementations of the tomographic technique of Zeeman-Doppler imaging, serve to drive steady-state solutions in each system. This paper contains the description of the stellar wind and inner astrosphere, while the coronal structure was previously discussed in Alvarado-Gómez et al. (2016). The analysis includes the magneto-hydrodynamical properties of the stellar wind, the associated mass and angular momentum loss rates, as well as the topology of the astrospheric current sheet in each system. A systematic comparison among the considered cases is performed, including two reference solar simulations covering activity minimum and maximum. For HD 1237, we investigate the interactions between the structure of the developed stellar wind, and a possible magnetosphere around the Jupiter-mass planet in this system. We find that the process of particle injection into the planetary atmosphere is dominated by the density distribution rather than velocity profile of the stellar wind. In this context, we predict a maximum exoplanetary radio emission of 12 mJy at 40 MHz in this system, assuming the crossing of a high-density streamer during periastron passage. Furthermore, in combination with the analysis performed in Alvarado-Gómez et al. (2016), we obtain for the first time a fully simulated mass loss-activity relation, which is compared and discussed in the context of the relation based on astrospheric detections proposed by Wood et al. (2005a). Finally, we provide a characterisation of the 3D properties of the stellar wind of these systems, at the inner edges of their habitable zones.
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