星斑映射与自适应并行退火 II. 应用于TESS数据：M矮星耀斑恒星AU Microscopii、YZ Canis Minoris和EV Lacertae
Starspot mapping with adaptive parallel tempering. II. Application to TESS data for M-dwarf flare stars, AU Microscopii, YZ Canis Minoris, and EV Lacertae
AI总结：
本研究利用自适应并行退火算法对三颗M矮星耀斑恒星的TESS光变曲线进行星斑建模，发现耀斑频率与旋转相位无强相关，并归因于星斑始终可见，同时解释了光变曲线变化源于星斑大小和纬度变化。
摘要：
星斑和恒星耀斑是恒星磁活动的指示器。储存在星斑周围的磁能被认为是耀斑的起源，但两者之间的联系尚未完全理解。为了研究从光变曲线推断的星斑位置与其中耀斑发生之间的关系，我们使用论文I中实现的代码，对三颗M矮星耀斑恒星AU Mic、YZ CMi和EV Lac的TESS光变曲线进行星斑建模。该代码通过自适应并行退火算法高效地推断多个恒星/星斑参数。我们发现，对于每颗恒星，耀斑发生频率不一定与光变曲线的旋转相位相关。星斑建模的结果表明，星斑在所有相位下始终对视线可见，我们提出这可能是旋转相位与耀斑频率之间没有或较少相关性的原因之一。此外，AU Mic和YZ CMi的光变曲线振幅和形状在不同TESS周期之间的两年内发生了变化。星斑建模的结果表明，这可以通过星斑大小和纬度的变化来解释。
英文摘要：
Starspots and stellar flares are indicators of stellar magnetic activity.The magnetic energy stored around spots is thought to be the origin of flares, but the connection is not completely understood. To investigate the relation between spot locations deduced from the light curves and occurrence of flares therein, we perform starspot modeling for TESS light curves of three M-dwarf flare stars, AU Mic, YZ CMi, and EV Lac, using the code implemented in Paper I. The code enables to deduce multiple stellar/spot parameters by the adaptive parallel tempering algorithm efficiently. We found that flare occurrence frequency is not necessarily correlated with the rotation phases of the light curve for each star. The result of starspot modeling shows that either spot is always visible to the line of sight in all phases, and we suggest that this can be one of the reasons that there is no or less correlation between rotation phases and flare frequency. In addition, the amplitude and shape of the light curve for AU Mic and YZ CMi have varied in two years between different TESS Cycles. The result of starspot modeling suggests that this can be explained by the variations of spot size and latitude.
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