论文标题
用动力磁层建模α$^2 $ CVN的光度变异性
Modeling the Photometric Variability of Alpha$^2$ CVn with a Dynamical Magnetosphere
论文作者
论文摘要
Alpha $^2 $ CANUM VESORUM（AM CVN）是一个具有奇特化学特征和周期性变化的强磁性星，长期以来一直归因于磁元素通过光电孔扩散，从而导致整个恒星表面的化学点。但是，对其他磁热星的最新研究与表面上方的磁层云一致。在这里，我们采用了一种新的方法，以简化的动力学磁层（DM）和倾斜的偏移磁性偶极子来建模AM CVN，以重现其传播的系外行星调查卫星（TESS）变异性。我们的偶极模型还很好地复制了Silvester，Kochukhov和Wade（2014）的AM CVN的磁表面图。它的紫外线可变性，来自IUE档案光谱，也与传统的红色模型一致。我们进一步讨论了磁层对系统中其他可观察量的含义，以结论不太可能在AM CVN中存在。
Alpha$^2$ Canum Venaticorum (AM CVn) is a strongly magnetic star with peculiar chemical signatures and periodic variability that have been long attributed to the diffusion of magnetic elements through the photosphere, leading to chemical spots across the stellar surface. However, recent studies of other magnetic hot stars are consistent with magnetospheric clouds above the surface. Here we take a renewed approach to modeling AM CVn with a simplified dynamical magnetosphere (DM) and a tilted, offset magnetic dipole to reproduce its Transiting Exoplanet Survey Satellite (TESS) variability. Our dipole model also reproduces well the magnetic surface map of AM CVn from Silvester, Kochukhov, & Wade (2014). Its ultraviolet variability, from IUE archival spectra, is also consistent with traditional reddening models. We further discuss the implications of a magnetosphere on other observable quantities from the system to conclude that it is unlikely to be present in AM CVn.
