低质量恒星集合中的耀发纬度
Flaring Latitudes in Ensembles of Low Mass Stars
AI总结：
本研究提出一种改编自fleck软件的新方法，利用耀斑等待时间分布的均值与标准差诊断低质量恒星的耀发纬度，在Kepler观测的G型矮星样本上验证了技术，并指出结合黑子与耀斑集合方法可提升表面磁场定位能力。
摘要：
恒星光球层中小尺度磁场的分布是我们理解低质量恒星磁性的重要要素。它们的空间分布将恒星内部产生的磁场与外部日冕及大尺度磁场联系起来，进而影响行星的空间天气。遗憾的是，我们缺乏能在大多数低质量恒星上定位这些磁场的技术。一种策略是利用磁场聚集区附近发生的耀斑来定位这些区域。\n我们探索了一种新方法，该方法改编自黑子模拟软件fleck，用于研究耀发时间随活动纬度的变化。我们利用经验关系构建类似于Kepler（开普勒太空望远镜）和Transiting Exoplanet Survey Satellite（TESS，凌日系外行星巡天卫星）观测到的耀斑光变曲线，在其中搜索耀斑，并利用耀斑之间的等待时间来确定活动纬度的位置。\n我们发现，等待时间分布的均值和标准差提供了一种独特的耀发纬度诊断方法，其结果与活动区数量相关。当恒星拥有3个或更少反复耀发的活动区、且活动纬度宽度低于20度时，纬度的恢复效果最佳；当其中任一参数增大时，关于活动纬度位置的信息会逐渐丢失。我们在Kepler卫星观测到的一组耀发G型矮星样本上验证了该技术，此外还提出，结合针对黑子和耀斑的集合方法，可以克服各自单独技术在表面磁场定位方面的局限性。
英文摘要：
The distribution of small-scale magnetic fields in stellar photospheres is an important ingredient in our understanding of the magnetism of low mass stars. Their spatial distribution connects the field generated in the stellar interior with the outer corona and the large scale field, and thereby affects the space weather of planets. Unfortunately, we lack techniques that can locate them on most low-mass stars. One strategy is to localize field concentrations using the flares that occur in their vicinity. We explore a new method that adapts the spot simulation software fleck to study the modulation of flaring times as a function of active latitude. We use empirical relations to construct flare light curves similar to those available from Kepler and the Transiting Exoplanet Survey Satellite (TESS), search them for flares, and use the waiting times between flares to determine the location of active latitudes. We find that the mean and standard deviation of the waiting time distribution provide a unique diagnostic of flaring latitudes as a function of the number of active regions. Latitudes are best recovered when stars have three or less active regions that flare repeatedly, and active latitude widths below 20 deg; when either increases, the information about the active latitude location is gradually lost. We demonstrate our technique on a sample of flaring G dwarfs observed with the Kepler satellite, and furthermore suggest that combining ensemble methods for spots and flares could overcome the limitations of each individual technique for the localization of surface magnetic fields.
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