AI 中文总结
该研究利用日出三号上的SUSI仪器观测数据，通过分析19条谱线的视线速度确定波脉冲高度相关时间偏移，发现不同高度波脉冲特征，证明多线方法在研究太阳大气物理条件高度依赖性上的潜力。
AI 中文摘要
我们报告了对低层太阳大气中波脉冲高度相关时间偏移的测量，该测量基于日出三号气球搭载太阳天文台在2024年7月成功的科学飞行期间，使用SUSI仪器获得的高分辨率光谱偏振观测数据。从Ca II H线周围2纳米宽窗口内19条谱线的线芯位置导出的视线速度，用于确定传播脉冲在其各自形成高度处的时间偏移。我们的分析表明，这些偏移大致根据各谱线的计算形成高度排序。对总时长一小时的定点观测的时间偏移进行统计分析发现，从太阳表面附近向上传播到约500 - 700千米高度的波脉冲最为常见，这些高度之间的平均时间滞后为2０到30秒。相位偏移接近零的脉冲也存在，主要在米粒间通道和磁活动增强区域上方。此外，还观测到负时间滞后为10到15秒的向下传播波脉冲，大多在磁活动增强区域上方。所有观测脉冲的一个共同特征是，在较低的250千米内它们显示出零到几秒的小时间滞后，只有在较高层传播脉冲才更占主导。这项研究证明了多线方法在研究太阳大气中物理条件高度依赖性方面的潜力。
英文摘要
We report on the measurement of the height-dependent time shifts of wave pulses in the lower solar atmosphere from high-resolution spectro-polarimetric observations obtained with the SUSI instrument on board the SUNRISE III balloon-borne solar observatory during its successful science flight in July 2024. The line-of-sight velocities derived from the line-core positions of 19 spectral lines in a 2 nm-wide window around the Ca II H line were used to determine the time shifts of propagating pulses at their respective formation heights. Our analysis reveals that these shifts are roughly ordered according to the computed formation heights of the respective spectral lines. A statistical analysis of the time shifts using sit-and-stare observations with a total duration of one hour reveals that wave pulses propagating upwards from near the solar surface to heights of approximately 500-700 km are most common, with average time lags of 20 s to 30 s between these heights. Also present are pulses with close-to-zero phase shifts, predominantly above intergranular lanes and areas of enhanced magnetic activity. Additionally, downward propagating wave pulses with negative time lags of 10 s to 15 s are seen, mostly above areas of enhanced magnetic activity. A common feature of all the observed pulses is that in the lower 250 km they show small time lags of zero to a few seconds, and only at higher layers do the propagating pulses become more dominant. This study demonstrates the potential of the many-line approach for investigating the height dependence of the physical conditions in the solar atmosphere.
Comments11 pages, 5 figures
