We present simultaneous magnetic field measurements for the limb solar flare of 1981 July 17 using of the Ca II K, Hδ, He I 4471.5 Å and Hβ lines. For two moments during the flare, which differ in time by 16 min, we analyzed Stokes I ± V profiles of these lines from observations made on the Echelle spectrograph of the horizontal solar telescope of the Astronomical Observatory of Taras Shevchenko National University of Kiev. At the time step that was close to the peak phase of the flare, all the spectral lines under study showed very wide emissions, with a full width at half maximum (FWHM) of 3.5–4 Å. An interesting feature was observed in the blue wings of these lines, namely, narrow emission peaks with a FWHM of only 0.25–0.35 Å. For heights of 10–18 Mm above the level of the photosphere, we found that (a) very strong kG magnetic fields (up to about 3 kG) existed at both moments of the flare, (b) the locations with strongest fields, in general, do not coincide for different spectral lines, (c) the polarities of the magnetic field for different spectral lines are in most cases identical, but sometimes they do not coincide. The data obtained indicate a significant inhomogeneity of the magnetic field in the flaring corona and the probable presence of the conditions necessary for magnetic reconnection of field lines.

我们使用 Ca II K、H δ、He  I 4471.5 Å 和 Hβ 线对 1981 年 7 月 17 日的边缘太阳耀斑进行同步磁场测量。在耀斑期间的两个时刻，时间相差 16 分钟，我们分析了斯托克斯I  ±  V这些线的轮廓来自基辅塔拉斯舍甫琴科国立大学天文台水平太阳望远镜的阶梯光谱仪的观测结果。在接近耀斑峰值阶段的时间步长，研究中的所有谱线都显示出非常宽的发射，半峰全宽 (FWHM) 为 3.5-4 Å。在这些谱线的蓝翼中观察到一个有趣的特征，即 FWHM 仅为 0.25-0.35 Å 的窄发射峰。对于光球层以上 10-18 毫米的高度，我们发现（a）在耀斑的两个时刻都存在非常强的 kG 磁场（高达约 3 kG），（b）磁场最强的位置，在一般情况下，不同谱线不重合，(c) 不同谱线的磁场极性在大多数情况下是相同的，但有时它们并不重合。获得的数据表明，耀斑日冕中的磁场存在显着的不均匀性，并且可能存在磁力线磁重联所需的条件。