Data from the Helioseismic and Magnetic Imager (HMI) on board the Solar Dynamics Observatory (SDO) on the components of the magnetic field vector in the photosphere for 39 active regions (AR) of the 24th solar activity cycle are used to calculate the parameters of the electric current. The time variations in the electric current parameters in the AR over the time the region is within ±35° of the central meridian are studied. An attempt is made to relate the parameters of the current in the photosphere and their dynamics to the level of flare activity of the region. These studies have yielded the following results: (1) The change in the total unsigned current in an AR is synchronous or quasi-synchronous with changes in the magnetic flux; (2) A relation between the total unsigned current and the flare index (FI) exists, but is weak (correlation k = 0.48); (3) The imbalance of the vertical electric currents for all 39 of the AR studied here was low and did not exceed a few percent, which indicates closure of the current structures on all scales within an AR; (4) The highest correlation ( k = 0.72) with the flare index is observed for a time averaged absolute value of the density of the vertical electric current; (5) Statistical studies yield a critical level of <| j z |> equal to 2.7 mA/m 2 : when this level is exceeded in an AR, flares with higher x-ray classes (M and X) are observed and when the current density falls below the threshold value, there is a reduction in the flare productivity of the region; (6) For the example of two regions with an emerging magnetic flux it is shown that pumping magnetic energy into the corona requires some time; the time interval between the jump in <| j z |> and the onset of the development of the first powerful flares in x-ray classes M and X is at least 12-20 hours; (7) The character of the relation between the time variations in the average value of the density of the horizontal current <| j ⊥ |> and the imbalance in the vertical current ρ jz with the level of flare activity of an AR is more complicated and requires separate, more detailed studies.

中文翻译：

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太阳活动区电流参数的动力学及其与耀斑指数的关系

来自太阳动力学天文台 (SDO) 上的日震和磁成像仪 (HMI) 的关于第 24 个太阳活动周期的 39 个活动区 (AR) 光球层中磁场矢量分量的数据用于计算以下参数：电流。研究了 AR 中电流参数在该区域在中央子午线 ±35° 范围内的时间变化。尝试将光球层中的电流参数及其动力学与该地区的耀斑活动水平联系起来。这些研究得出了以下结果： (1) AR 中总无符号电流的变化与磁通量的变化同步或准同步；(2) 总无符号电流与耀斑指数 (FI) 之间存在关系，但很弱（相关性 k = 0.48）；(3) 这里研究的所有 39 个 AR 的垂直电流不平衡都很低，不超过几个百分点，这表明 AR 内所有尺度的电流结构都已闭合；(4) 垂直电流密度的时间平均绝对值与耀斑指数的相关性最高(k = 0.72)；(5) 统计研究得出的临界水平 <| jz |> 等于 2.7 mA/m 2 ：当 AR 中超过该水平时，观察到具有更高 X 射线类别（M 和 X）的耀斑，并且当电流密度低于阈值时，该地区的火炬生产力；(6) 对于具有出现磁通量的两个区域的示例，表明将磁能泵入电晕需要一些时间；<| 跳转之间的时间间隔 jz |> 并且在 X 射线 M 和 X 级中出现第一个强大耀斑的开始时间至少为 12-20 小时；(7) 水平电流密度平均值随时间变化的关系特征<| j ⊥ |> 以及垂直电流 ρ jz 与 AR 耀斑活动水平的不平衡更复杂，需要单独、更详细的研究。