SOLIS/VSM数据的第一非线性无力场外推
First nonlinear force-free field extrapolations of SOLIS/VSM data
摘要：
研究了活动区日冕磁场结构及其时间演化。我们试图比较一个活动区在一个非常安静的时期，在耀斑的同一地区的磁位形。可能是第一次，我们使用矢量磁像数据从天气光学长期调查的太阳巡天（SOLIS）模拟日冕磁场作为一个序列的非线性无力平衡。我们研究了2007年6月7日观测到的活动区NOAA 10960，在一个小的C1.0耀斑的时间节奏10分钟和6个快照在一个安静的时期。活动区的总磁能约为$3 \times 10^{25}$ J，耀斑前自由磁能约为位场能的5%。在耀斑期间释放了一部分多余的能量，在平静期开始时几乎产生了一种潜在的配置。在研究期间，日冕磁场能量仅比位场能量高百分之几，因此只发生了一次小的C1.0耀斑。这是与早期研究的活动区10540相比，其中的自由磁能比产生两个M级耀斑的势场高约60%。然而，自由磁能积累之前，并在耀斑期间被释放，这似乎是大，小耀斑的情况。
英文摘要：
We study the coronal magnetic field structure inside active regions and its temporal evolution. We attempt to compare the magnetic configuration of an active region in a very quiet period with that for the same region during a flare. Probably for the first time, we use vector magnetograph data from the Synoptic Optical Long-term Investigations of the Sun survey (SOLIS) to model the coronal magnetic field as a sequence of nonlinear force-free equilibria. We study the active region NOAA 10960 observed on 2007 June 7 with three snapshots taken during a small C1.0 flare of time cadence 10 minutes and six snapshots during a quiet period. The total magnetic energy in the active region was approximately $3 \times 10^{25}$ J. Before the flare the free magnetic energy was about 5% of the potential field energy. A part of this excess energy was released during the flare, producing almost a potential configuration at the beginning of the quiet period. During the investigated period, the coronal magnetic energy was only a few percent higher than that of the potential field and consequently only a small C1.0 flare occurred. This was compared with an earlier investigated active region 10540, where the free magnetic energy was about 60% higher than that of the potential field producing two M-class flares. However, the free magnetic energy accumulates before and is released during the flare which appears to be the case for both large and small flares.
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