A Near-half-century Simulation of the Solar Corona
A Near-half-century Simulation of the Solar Corona
复制标题
DOI：
10.3847/2041-8213/ad1934
复制
发表时间：
2024-01
期刊：
影响因子：
--
通讯作者：
Valentin Aslanyan;Karen A. Meyer;R. Scott;A. Yeates
中科院分区：
文献类型：
--
作者：
Valentin Aslanyan;Karen A. Meyer;R. Scott;A. Yeates
我们提出了一个概述的结果，从磁摩擦模型的整个太阳日冕在一个为期47年。模拟自相一致地再现了几十年的太阳现象，在快速爆发和长期的太阳周期之间的持续时间不同，从输入观察到的活跃地区出现在光球。我们已经开发了一种几何方法来使用磁螺旋度来识别和定位在模拟中发生的频繁喷发。这种方法使我们能够将我们的结果与瞬态事件的极紫外观测相匹配。我们已经分析了不断发展的磁拓扑结构，通过计算挤压因子和分割成离散的磁域的分离网络的电晕。模拟结果显示，分离网的动态结构比位场模型预测的更为动态，这可能解释了太阳风的观测结果。
We present an overview of results from a magnetofrictional model of the entire solar corona over a period of 47 yr. The simulation self-consistently reproduces decades of solar phenomena, varying in duration between rapid eruptions and the long-term solar cycles, from an input of observed active regions emerging at the photosphere. We have developed a geometric approach to use magnetic helicity to identify and localize the frequent eruptions that occur in the simulation. This method allows us to match our results to extreme-ultraviolet observations of transient events. We have analyzed the evolving magnetic topology by computing the squashing factor and segmenting the corona into discrete magnetic domains bounded by the Separatrix-Web. The simulations show a more dynamic structure to the Separatrix-Web than is predicted by potential field models, which may explain solar wind observations.