模拟全球太阳日冕：细丝手征观测和表面模拟
Modelling the Global Solar Corona: Filament Chirality Observations and Surface Simulations
摘要：
在日冕全球磁场的背景下，太阳灯丝的半球图案被认为是。在最近的工作中，麦凯和范Ballegooijen已经表明，对于一对相互作用的磁双极，观察到的手征模式可以通过每个半球的双极倾斜角和螺旋度的主导范围来解释。这项研究的目的是通过理论和观测之间的直接比较来测试这一早期结果，使用新开发的模拟实际表面和三维日冕磁场在6个月的时间内，在全球范围内。在本文中，我们考虑两个关键组成部分的研究，首先是观察的255个灯丝的样品的灯丝手征，其次是我们的新模拟的大规模表面磁场。基于通量传输模型，这些将被用作未来三维日冕模拟的下边界条件。我们的技术与其他作者的技术有很大的不同，在其他作者的技术中，日冕场要么被假设为纯粹的电势，要么必须每27天重置一次，以保持光球场的准确性。在我们的例子中，我们确保插入新出现的双极活动区的准确性，根据观测到的光球天气磁图。大规模的表面字段显示保持准确的6个月期间，没有任何重置。这项新技术将使未来的模拟能够考虑日冕磁场中螺旋度和剪切的长期积累和传输，持续数月或数年。
英文摘要：
The hemispheric pattern of solar filaments is considered in the context of the global magnetic field of the solar corona. In recent work Mackay and van Ballegooijen have shown how, for a pair of interacting magnetic bipoles, the observed chirality pattern could be explained by the dominant range of bipole tilt angles and helicity in each hemisphere. This study aims to test this earlier result through a direct comparison between theory and observations, using newly-developed simulations of the actual surface and 3D coronal magnetic fields over a 6-month period, on a global scale. In this paper we consider two key components of the study; firstly the observations of filament chirality for the sample of 255 filaments, and secondly our new simulations of the large-scale surface magnetic field. Based on a flux-transport model, these will be used as the lower boundary condition for the future 3D coronal simulations. Our technique differs significantly from those of other authors, where the coronal field is either assumed to be purely potential, or has to be reset back to potential every 27 days in order that the photospheric field remain accurate. In our case we ensure accuracy by the insertion of newly-emerging bipolar active regions, based on observed photospheric synoptic magnetograms. The large-scale surface field is shown to remain accurate over the 6-month period, without any resetting. This new technique will enable future simulations to consider the long-term build-up and transport of helicity and shear in the coronal magnetic field, over many months or years.
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