Sunspot seismology: accounting for magnetohydrodynamic wave processes using imaging spectropolarimetry
S. P. Rajaguru
备注：
7 pages, 2 figures, published in Proceedings of the First Asia-Pacific Solar Physics Meeting, Astronomical Society of India (ASI) Conference Series, 2011, Vol. 2, pp 181-188 Edited by Arnab Rai Choudhuri & Dipankar Banerjee
声波吸收，模式转换和传输的太阳黑子日震推断的影响被广泛讨论，但尚未占他们已被证明是困难的缺乏一致的框架内日震建模。在这里，讨论的问题和问题，近地表磁流体力学主机通过复杂的相互作用的辐射转移，测量问题，和MHD波过程，我提出了一些可能性完全从观测分析的基础上成像光谱偏振。特别是，我提出了一些结果波的演变作为观测高度和磁场的垂直倾斜度的函数，来自一个高节奏的成像光谱偏振观测的太阳黑子及其周围环境的仪器IBIS（NSO/Sac峰，美国）。这些观测是在磁敏感（Fe I 6173 A）和磁不敏感（Fe I 7090 A）的上部光球吸收线上进行的。这里估计的太阳黑子光球层内的波旅行时间的贡献将需要从反演建模程序中删除，因为反演建模程序没有规定要考虑它们。
英文摘要：
The effects of acoustic wave absorption, mode conversion and transmission by a sunspot on the helioseismic inferences are widely discussed, but yet accounting for them has proved difficult for lack of a consistent framework within helioseismic modelling. Here, following a discussion of problems and issues that the near-surface magnetohydrodynamics hosts through a complex interplay of radiative transfer, measurement issues, and MHD wave processes, I present some possibilities entirely from observational analyses based on imaging spectropolarimetry. In particular, I present some results on wave evolution as a function of observation height and inclination of magnetic field to the vertical, derived from a high-cadence imaging spectropolarimetric observation of a sunspot and its surroundings using the instrument IBIS (NSO/Sac Peak, USA). These observations were made in magnetically sensitive (Fe I 6173 A) and insensitive (Fe I 7090 A) upper photospheric absorption lines. Wave travel time contributions from within the photospheric layers of a sunspot estimated here would then need to be removed from the inversion modelling procedure, that does not have the provision to account for them.
Spectropolarimetry of Atomic and Molecular Lines near 4135nm
利用4135nm附近的光球原子和分子吸收谱线进行了新的空间扫描偏振光谱黑子观测。测量了几条原子谱线之间的相对分裂，结果表明与组态相互作用和中间耦合计算的值一致。在4137nm处的Fe I谱线中观察到大的分裂，显示出多个Stokes V分量和不寻常的线性偏振。这条谱线将成为宁静太阳磁场的灵敏探测器，其磁灵敏度比著名的1565nm Fe I谱线高2.5倍。
Spectropolarimetry of Sunspot Penumbrae -- A Comprehensive Study of the Evershed Effect Using High Resolution Data from the Space-Borne Solar Observatory HINODE
在同一半影（三角斑）内有两个磁极性本影的太阳黑子通常但并不总是与耀斑有关。我们提出了第一个近红外（NIR）观测（Fe I 1078.3 nm和Si I 1078.6 nm光谱）与特内里费岛的真空塔望远镜（VTT）在特内里费岛的特内里费岛红外偏振仪（TIP）获得2012年6月17日，这提供了准确和灵敏的诊断，以仔细检查复杂的字段沿磁中性线的三角洲内的活动区域NOAA 11504点。我们检查矢量磁场，视线（LOS）的速度，和水平自行车，而不活跃的三角洲点。我们发现磁矢量场从主本影到相反极性（δ本影）的平滑过渡，但在距δ本影一定距离处的极性反转线上，水平磁场不连续。磁场随着高度的增加而减小，在三角本影上方减小到原来的两倍。后者被其自身的Evershed流所包围。来自主本影的埃弗谢德流在将点分成两部分的线处结束。这条线的标志是在Ca II 854.2 nm线中出现中心发射。沿着这条线，出现了两个符号的高色球层LOS速度。我们检测到的剪切流内的水平通量输送速度平行于分界线。
Chromospheric resonator model for sunspot revealed by multi-height observation of umbral wave
Key Laboratory of Solar Activity and Space Weather, School of Aerospace, Harbin Institute of Technology, Shenzhen, Guangdong, China（哈尔滨工业大学深圳学院航天学院太阳活动与空间天气重点实验室）；Shenzhen Key Laboratory of Numerical Prediction for Space Storm, School of Aerospace, Harbin Institute of Technology, Shenzhen, Guangdong, China（哈尔滨工业大学深圳学院航天学院空间风暴数值预测深圳市重点实验室）；Department of Physics, Indian Institute of Technology (BHU), Varanasi-221005, India（印度瓦拉纳西贝拿勒斯印度理工学院物理系）
