Schad Thomas A, Petrie Gordon J D, Kuhn Jeffrey R, Fehlmann Andre, Rimmele Thomas, Tritschler Alexandra, Woeger Friedrich, Scholl Isabelle, Williams Rebecca, Harrington David, Paraschiv Alin R, Szente Judit
National Solar Observatory, 22 'Ōhi'a Kū Street, Makawao, HI 96768, USA.
National Solar Observatory, 3665 Discovery Drive, Boulder, CO, 80303, USA.
Sci Adv. 2024 Sep 13;10(37):eadq1604. doi: 10.1126/sciadv.adq1604. Epub 2024 Sep 11.
Regular remote sensing of the magnetic field embedded within the million-degree solar corona is severely lacking. This reality impedes fundamental investigations of the nature of coronal heating, the generation of solar and stellar winds, and the impulsive release of energy into the solar system via flares and other eruptive phenomena. Resulting from advancements in large aperture solar coronagraphy, we report unprecedented maps of polarized spectra emitted at 1074 nm by Fe atoms in the active corona. We detect clear signatures of the Zeeman effect that are produced by the coronal magnetic field along the optically thin path length of its formation. Our comparisons with global magnetohydrodynamic models highlight the valuable constraints that these measurements provide for coronal modeling efforts, which are anticipated to yield subsequent benefits for space weather research and forecasting.
对百万度太阳日冕中嵌入的磁场进行常规遥感观测严重不足。这一现状阻碍了对日冕加热本质、太阳风和恒星风的产生以及通过耀斑和其他爆发性现象向太阳系脉冲式释放能量等方面的基础研究。基于大口径太阳日冕仪的进展，我们报告了活动日冕中铁原子在1074纳米处发射的偏振光谱的前所未有的图谱。我们检测到了日冕磁场在其形成的光学薄路径长度上产生的清晰的塞曼效应特征。我们与全球磁流体动力学模型的比较突出了这些测量为日冕建模工作提供的宝贵约束，预计这将为空间天气研究和预报带来后续益处。
