演化孔隙边界的磁性
Magnetic properties on the boundary of an evolving pore
摘要：
上下文对本影边界的磁性分析得出了Jurcak判据，该判据指出，稳定太阳黑子中的本影-半影边界同样由恒定的垂直磁场Bver_crit和0.5的宁静太阳连续强度Iqs定义。垂直磁场强于Bver_crit的本影是稳定的，而垂直磁场弱于Bver_crit的本影是不稳定的，并且倾向于消失。目的。探讨孔隙边界垂直磁场临界值的存在及其在磁性结构演化中的作用。方法.我们分析了SDO/HMI矢量场图校正散射光的时间节奏为12分钟，在26.5小时内。强度阈值（Ic = 0.55 Iqs）被用来定义孔隙边界和时间演化的磁性研究。结果观察到孔隙演化的阶段性：（1）在初始阶段，总磁场强度（B）和垂直磁场（Bver）分别增加到1920 G和1730 G，然后孔隙进入稳定阶段;（3）在第二形成阶段，孔隙尺寸迅速增长，边界B和Bver减小。在新形成的区域，Bver大部分保持在1731 G以下，B保持在1921 G以下;（4）最终，孔隙开始衰变。我们发现，总体上，具有Bver<1731 G或等效地B<1921 G的孔隙区域比满足该标准的区域分解得更快。结论.孔的最稳定的区域，类似于本影边界的情况下，由Bver的临界值，这是比较稳定的太阳黑子中发现的。此外，在该案例研究中，相同的孔隙面积可以类似地由总磁场强度的临界值很好地限定。
英文摘要：
Context. Analyses of magnetic properties on umbrae boundaries led to the Jurcak criterion, which states that umbra-penumbra boundaries in stable sunspots are equally defined by a constant value of the vertical magnetic field, Bver_crit, and by 0.5 continuum intensity of the quiet Sun, Iqs. Umbrae with vertical magnetic fields stronger than Bver_crit are stable, whereas umbrae with vertical magnetic fields weaker than Bver_crit are unstable and prone to vanishing. Aims. To investigate the existence of a critical value of the vertical magnetic field on a pore boundary and its role in the evolution of the magnetic structure. Methods. We analysed SDO/HMI vector field maps corrected for scattered light with a temporal cadence of 12 min during a 26.5-hour period. An intensity threshold (Ic = 0.55 Iqs) is used to define the pore boundary and temporal evolutions of the magnetic properties are studied there. Results. We observe stages in the pore evolution: (1)during an initial formation phase, total magnetic field strength (B) and vertical magnetic field (Bver) increase to their maximum values of ~1920 G and ~1730 G, respectively; (2)then the pore reaches a stable phase; (3)in a second formation phase, the pore undergoes a rapid growth in size, along with a decrease in B and Bver on its boundary. In the newly formed area, Bver remains mostly below 1731 G and B remains everywhere below 1921 G; (4)ultimately, pore decay starts. We find overall that pore areas with Bver<1731 G, or equivalently B<1921 G, disintegrate faster than regions that fulfil this criteria. Conclusions. The most stable regions of the pore, similarly to the case of umbral boundaries, are defined by a critical value of Bver that is comparable to that found in stable sunspots. In addition, in this case study, the same pore areas can be similarly well-defined by a critical value of the total magnetic field strength.
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