标题： 光球中瞬变水平磁场的三维视图 显示英文标题

标题： 3D view of transient horizontal magnetic fields in the photosphere

摘要： 我们利用SIRGAUS反演程序推断了太阳耀斑期间穿过光球层的瞬态水平磁场（THMF）的三维磁结构。SIRGAUS代码是SIR（基于响应函数的Stokes反演）的修改版本，允许从观测到的Stokes轮廓中提取有关嵌入大气中的磁通管的磁性和热动力学参数的信息。使用搭载于Hinode卫星上的太阳光学望远镜（SOT）对中心盘面处宁静太阳进行了光谱极化观测，所用谱线为Fe I 630.2 nm。通过130秒周期的重复扫描，我们首先检测到出现在粒细胞内部边缘附近的水平磁场。在第二次扫描中，在水平磁场两端出现正负极性的垂直磁场。然后，水平磁场消失，留下双极性垂直磁场。Stokes光谱反演的结果清楚地表明存在一个磁感应强度为$\sim400$ G的磁通管，该磁通管穿过Fe I 630.2 nm谱线的形成层。该磁通管在$\log\tau_{500} \sim0$位置，时间为$\Delta t$=0秒，并在$\log\tau_{500} \sim-1.7$位置，时间为$\Delta t$=130秒。在$\Delta t$=260秒时，水平部分已经超出所分析谱线的形成区域。观测到的多普勒速度最大为3公里每秒$^{-1}$，与SIRGAUS代码检索到的结构上升运动一致。管子的垂直尺寸小于线形成层的厚度。 THMF 具有一个清晰的$\Omega$形环状结构，其顶端靠近颗粒状细胞的边缘。 该 THMF 所携带的磁通量估计为$3.1\times10^{17}$Mx。 显示英文摘要

摘要： We infer the 3D magnetic structure of a transient horizontal magnetic field (THMF) during its evolution through the photosphere using SIRGAUS inversion code. The SIRGAUS code is a modified version of SIR (Stokes Inversion based on Response function), and allows for retrieval of information on the magnetic and thermodynamic parameters of the flux tube embedded in the atmosphere from the observed Stokes profiles. Spectro-polarimetric observations of the quiet Sun at the disk center were performed with the Solar Optical Telescope (SOT) on board Hinode with Fe I 630.2 nm lines. Using repetitive scans with a cadence of 130 s, we first detect the horizontal field that appears inside a granule, near its edge. On the second scan, vertical fields with positive and negative polarities appear at both ends of the horizontal field. Then, the horizontal field disappears leaving the bipolar vertical magnetic fields. The results from the inversion of the Stokes spectra clearly point to the existence of a flux tube with magnetic field strength of $\sim400$ G rising through the line forming layer of the Fe I 630.2 nm lines. The flux tube is located at around $\log\tau_{500} \sim0$ at $\Delta t$=0 s and around $\log\tau_{500} \sim-1.7$ at $\Delta t$=130 s. At $\Delta t$=260 s the horizontal part is already above the line forming region of the analyzed lines. The observed Doppler velocity is maximally 3 km s$^{-1}$, consistent with the upward motion of the structure as retrieved from the SIRGAUS code. The vertical size of the tube is smaller than the thickness of the line forming layer. The THMF has a clear $\Omega$-shaped-loop structure with the apex located near the edge of a granular cell. The magnetic flux carried by this THMF is estimated to be $3.1\times10^{17}$ Mx.