X射线耀斑振荡跟踪猎户座恒星形成区沿星盘磁管的等离子体晃动
X-ray flare oscillations track plasma sloshing along star-disk magnetic tubes in Orion star-forming region
摘要：
脉冲X射线发射跟踪等离子体回波在一个非常长的磁管，耀斑在猎户座前主序星（PMS）。在太阳上，耀斑持续几分钟到几个小时，持续时间最长的通常涉及封闭磁管的拱廊。在PMS星中观测到了持久的X射线耀斑。钱德拉星上的高级CCD成像光谱仪（ACIS）从猎户座星团PMS星观测到的长达一天的耀斑的光变曲线中检测到大振幅（~20%）长周期（~3小时）脉动。对V772 Ori和OW Ori上观测到的两个耀斑的详细流体动力学模拟表明，这些脉动可能会跟踪由足够短（约1小时）的热脉冲触发的沿单个长磁管的等离子体晃动。这些磁管的长度（>= 20个太阳半径）足以将恒星与周围的圆盘连接起来。
英文摘要：
Pulsing X-ray emission tracks the plasma echo traveling in an extremely long magnetic tube that flares in an Orion Pre-Main Sequence (PMS) star. On the Sun, flares last from minutes to a few hours and the longest-lasting typically involve arcades of closed magnetic tubes. Long-lasting X-ray flares are observed in PMS stars. Large-amplitude (~20%) long-period (~3 hours) pulsations are detected in the light curve of day-long flares observed by the Advanced CCD Imaging Spectrometer (ACIS) on-board Chandra from PMS stars in the Orion cluster. Detailed hydrodynamic modeling of two flares observed on V772 Ori and OW Ori shows that these pulsations may track the sloshing of plasma along a single long magnetic tube, triggered by a sufficiently short (~1 hour) heat pulse. This magnetic tubes are as long (>= 20 solar radii) as to connect the star with the surrounding disk.
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