年轻的类太阳恒星V530 Per的表面磁性和日珥的短期变化

Cang Tianqi, P. Petit, J. Donati, C. Folsom
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引用次数: 1

摘要

V530 Per是年轻疏散星团英仙座α的一个类太阳成员,具有超短的旋转周期(P ~ 0.32d)。我们报告了两个使用espadon的光谱偏振运动,旨在表征其磁活动和大尺度磁场的短期变化。利用2006年和2018年获得的时间分辨偏振光谱观测数据,通过塞曼-多普勒成像重建了V530 Per的亮度分布和大尺度磁场几何形状。使用相同的数据集,我们还通过Hα发射的断层扫描绘制了日珥的空间分布。在这两个时期,我们重建了一个大的黑斑,占据了V530 Per的极地区域,而在低纬度地区重建了较小的(暗斑和亮斑)。最大场强达到了~ 1 kG。日珥模式在日珥半径附近呈现稳定分量。在2018年,我们还观察到快速演变的α发射结构,时间尺度从几分钟到几天不等。Hα的快速演化与在斑点或磁覆盖范围内检测到的任何光球变化无关。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
Short-term variations of surface magnetism and prominences of the young sun-like star V530 Per
Abstract V530 Per is a solar-like member of the young open cluster α Persei, with an ultra-short rotation period (P∼0.32d). We report on two spectropolarimetric campaigns using ESPaDOnS, aimed at characterizing the short-term variability of its magnetic activity and large-scale magnetic field. We used time-resolved spectropolarimetric observations obtained in 2006 and 2018 and reconstructed the brightness distribution and large-scale magnetic field geometry of V530 Per through Zeeman-Doppler imaging. Using the same data sets, we also mapped the spatial distribution of prominences through tomography of Hα emission. We reconstruct, at both epochs, a large, dark spot occupying the polar region of V530 Per while smaller (dark and bright) spots were reconstructed at lower latitudes. The maximal field strength reached ∼1 kG. The prominence pattern displayed a stable component that was confined close to the corotation radius. In 2018, we also observed rapidly evolving Hα emitting structures, over timescales ranging from minutes to days. The fast Hα evolution was not linked to any detected photospheric changes in the spot or magnetic coverage.
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