论文标题
他们的主人巨星的狂热行星的无线电蚀
Radio eclipses of exoplanets by the winds of their host stars
论文作者
论文摘要
迄今为止，搜索超级无线电排放的搜索导致了零结论性检测。从观察到的频率范围，望远镜灵敏度到发射的光束，已经提出了各种解释。在最近的一篇论文中，我们说明，系外行星可以通过宿主恒星风的无线电光球绕，该区域以特定频率在特定频率上呈光学厚，对于大部分轨道。结果，源自行星的无线电发射可以被宿主星的风吸收或“黯然失色”。在这里，我们研究了恒星风和轨道参数的性质如何影响行星被恒星风黯然失色的轨道的比例。我们表明，具有低密度风的行星旋转的恒星在无线电中检测更有利。就轨道参数而言，从过境行星发射可以逃脱最容易的风。我们将模型应用于$τ$ 〜BOO行星系统，并表明观察行星轨道的比例被主机恒星的风覆盖，可以使用来限制恒星风的特性。但是，我们开发的模型将需要与单独的方法一起使用，以消除恒星风的质量损失率和温度。
The search for exoplanetary radio emission has resulted in zero conclusive detections to date. Various explanations for this have been proposed, from the observed frequency range, telescope sensitivity, to beaming of the emission. In a recent paper, we illustrated that exoplanets can orbit through the radio photosphere of the wind of the host star, a region that is optically thick at a specific frequency, for a large fraction of their orbits. As a result, radio emission originating from the planet could be absorbed or `eclipsed' by the wind of the host star. Here we investigate how the properties of the stellar wind and orbital parameters affect the fraction of the orbit where the planet is eclipsed by the stellar wind. We show that planets orbiting stars with low density winds are more favourable for detection in the radio. In terms of the orbital parameters, emission from transiting planets can escape the stellar wind easiest. We apply our model to the $τ$~Boo planetary system, and show that observing the fraction of the planet's orbit where it is eclipsed by the wind of the host star could be used to constrain the properties of the stellar wind. However, our model developed would need to be used in conjunction with a separate method to disentangle the mass-loss rate and temperature of the stellar wind.
