Time series of photospheric magnetic parameters of solar active regions (ARs) are used to answer the question whether scaling properties of fluctuations embedded in such time series help to distinguish between flare-quiet and flaring ARs. We examine a total of 118 flare-quiet and 118 flaring AR patches, Helioseismic and Magnetic Imager Active Region Patches (called HARPs), which were observed from 2010 to 2016 by the Helioseismic and Magnetic Imager (HMI) on board the Solar Dynamics Observatory (SDO). Specifically, the scaling exponent of fluctuations is derived applying the Detrended Fluctuation Analysis (DFA) method to a dataset of 8-day time series of 18 photospheric magnetic parameters at 12-min cadence for all HARPs under investigation. We first find a statistically significant difference in the distribution of the scaling exponent between the flare-quiet and flaring HARPs, in particular for some space-averaged, signed parameters associated with magnetic field line twist, electric current density, and current helicity. The flaring HARPs tend to show higher values of the scaling exponent compared to those of the flare-quiet ones, even though there is considerable overlap between their distributions. In addition, for both the flare-quiet and the flaring HARPs the DFA analysis indicates that i) time series of most of various magnetic parameters under consideration are non-stationary, and ii) time series of the total unsigned magnetic flux and the mean photospheric magnetic free energy density in general present a non-stationary, persistent property, while the total unsigned flux near magnetic polarity inversion lines and parameters related to current density show a non-stationary, anti-persistent trend in their time series.

中文翻译：

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耀斑安静与耀斑活动区域的光球磁参数的时间序列分析：波动的标度特性

太阳活动区 (AR) 的光球磁参数时间序列用于回答嵌入在此类时间序列中的波动的缩放特性是否有助于区分耀斑平静区和耀斑 AR 的问题。我们检查了 2010 年至 2016 年间由太阳动力学天文台上的日震和磁成像仪 (HMI) 观测到的总共 118 个静止的耀斑和 118 个耀斑 AR 斑块、日震和磁成像仪活动区域斑块（称为 HARP）（ SDO)。具体来说，波动的标度指数是将去趋势波动分析 (DFA) 方法应用于所有被调查的 HARP 的 12 分钟节奏的 18 个光球磁参数的 8 天时间序列数据集得出的。我们首先发现，在静息和耀斑 HARP 之间缩放指数的分布存在统计学上的显着差异，特别是对于与磁场线扭曲、电流密度和电流螺旋度相关的一些空间平均的带符号参数。尽管它们的分布之间存在相当大的重叠，但与耀斑安静的 HARP 相比，耀斑的 HARP 往往显示出更高的缩放指数值。此外，对于静止和耀斑的 HARPs，DFA 分析表明 i) 所考虑的大多数各种磁参数的时间序列是非平稳的，以及 ii) 总无符号磁通量和平均光球层的时间序列磁自由能密度通常呈现非平稳、持久的特性，