We study the solar flare of July 19, 2000 of M6.4/3N class, which occurred in the active region NOAA 9087. Echelle Zeeman spectrograms of this flare were obtained with the horizontal solar telescope of the Astronomical Observatory of Taras Shevchenko National University of Kyiv. Physical conditions were compared for two times corresponding to the pre-peak and peak phases of the flare in area of a small sunspot. It was found that the effective magnetic field \(B\)_eff by Fe I 6301.5 and Fe I 6302.5 lines was almost the same for both times and both spectral lines. However, \(B\)_eff in peak phase measured by the splitting of the emission peaks of Fe II and H\(\upbeta \) lines turned out to be 300–500 G stronger than those by the above-mentioned Fe I lines, whereas by D3 He I line it was found to be close to zero. This may indicate a local magnetic field increase in height range from temperature minimum region to the lower chromosphere. A semi-empirical model of the photospheric layers of the flare, constructed on a base of observations of Fe I 5123.7 and Fe I 5434.5 lines by solving the inverse problem for non-equilibrium radiative transfer using Tikhonov stabilizers, shows the moderate increasing of temperature (∼300 K) in altitude range 250–500 km. The radial velocities were decreased during peak phase. The micro-turbulent velocity was increased in the photosphere layers before the flare peak, while during the peak phase it was significantly decreased. The obtained results indicate that in the pre-peak phase the altitude perturbations in the photosphere were larger than in the peak phase.

我们研究了2000年7月19日发生在活动区NOAA 9087上的M6.4 / 3N类太阳耀斑。该耀斑的Echelle Zeeman光谱图是使用塔拉斯·舍甫琴科国立大学天文台的水平太阳望远镜获得的。基辅 将物理条件进行了两次比较，分别对应于一个小黑子区域内耀斑的峰前和峰期。已发现，Fe I 6301.5和Fe I 6302.5谱线的有效磁场\（B \）_eff在时间和谱线上都几乎相同。但是，通过分裂Fe II和H的发射峰来测量峰相中的（B \）_eff （\ upbeta \）事实证明，这些线比上述Fe I线强300–500 G，而D3 He I线的强度接近零。这可能表明局部磁场在从温度最小区域到较低色球层的高度范围内增加。通过使用Tikhonov稳定剂解决非平衡辐射转移的反问题，在观察Fe I 5123.7和Fe I 5434.5线的基础上构建了火炬光球层的半经验模型，结果表明温度适度升高（在250-500 km的海拔范围内约为300 K）。在峰值阶段，径向速度降低了。在耀斑峰值之前，微球速度在光球层中增加，而在峰值阶段则显着降低。