论文标题
M矮人的耀斑和旋转，可居住区域可访问苔丝行星检测
Flares and rotation of M dwarfs with habitable zones accessible to TESS planet detections
论文作者
论文摘要
我们表征了M矮人的磁性活动，以向行星群落提供有关恒星能量输入的信息；特别是，除了直接观察到苔丝的光耀斑的频率外，我们还旨在估算相应的X射线火炬频率，从而利用在两个波段中同时观察到的一小部分已知事件。我们确定了112 m矮小的苔丝幅度<= 11.5，苔丝可以探测整个可居住区域的过渡区。这112颗恒星从主要任务中有1276个两分钟的曲折苔丝光曲线，我们搜索了旋转调制和耀斑。我们研究旋转与耀斑之间以及耀斑特性之间的联系，例如耀斑振幅 - 持续关系和累积耀斑能量频率分布（FFD）。假设每种光耀斑都与X射线频带中的耀斑相关，并利用出版的同时开普勒/K2和XMM-Newton Flare研究，我们估计我们检测到的Tess Flare事件发布的X射线能量。我们的校准还涉及苔丝和K2带中的耀斑能量之间的关系。我们在大约32％的目标中检测到了2500多个光耀斑事件，并且发现仅在12颗恒星的可靠旋转周期，这是大约11％的一小部分。对于这12个目标，我们提出了累积的FFD和FFD Power Law。我们通过校准X射线光耀斑能量来构建X射线频带中的FFD。在没有直接观察到的主要序列恒星的X射线FFD的情况下，我们的预测可以用于估计典型的快速旋转早期或中间矮人的高能输入的高能输入。
We characterize the magnetic activity of M dwarfs to provide the planet community with information on the energy input from the star; in particular, in addition to the frequency of optical flares directly observed with TESS, we aim at estimating the corresponding X-ray flare frequencies, making use of the small pool of known events observed simultaneously in both wavebands. We identified 112 M dwarfs with a TESS magnitude <= 11.5 for which TESS can probe the full habitable zone for transits. These 112 stars have 1276 two-minute cadence TESS light curves from the primary mission, which we searched for rotational modulation and flares. We study the link between rotation and flares and between flare properties, for example the flare amplitude-duration relation and cumulative flare energy frequency distributions (FFDs). Assuming that each optical flare is associated with a flare in the X-ray band, and making use of published simultaneous Kepler/K2 and XMM-Newton flare studies, we estimate the X-ray energy released by our detected TESS flare events. Our calibration also involves the relation between flare energies in the TESS and K2 bands. We detected more than 2500 optical flare events on a fraction of about 32% of our targets and found reliable rotation periods only for 12 stars, which is a fraction of about 11%. For these 12 targets, we present cumulative FFDs and FFD power law fits. We construct FFDs in the X-ray band by calibrating optical flare energies to the X-rays. In the absence of directly observed X-ray FFDs for main-sequence stars, our predictions can serve for estimates of the high-energy input to the planet of a typical fast-rotating early- or mid-M dwarf.
