发表机构
University of Colorado Boulder; Cooperative Institute for Research in Environmental Sciences; National Solar Observatory; Predictive Science Inc.（科罗拉多大学博尔德分校; 环境科学合作研究所; 国家太阳观测台; 预测科学公司）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本文通过三维全局日冕MHD模拟，研究日冕加热与磁场标度对低中日冕全局性质的影响，发现增加总热量会提升开放通量并改变K日冕形态，为低分辨率模型的亚网格修正提供依据。
AI 中文摘要
太阳磁场是日冕加热和太阳风加速的关键驱动因素，二者共同影响日冕的可观测形态，同时确定开放磁通量的磁连通性与大小。本文通过分析一系列受数据约束的、适用于太阳极小期的三维全局日冕热力学磁流体动力学（MHD）模拟，研究日冕加热如何影响日冕的磁热状态。我们通过修改用于日冕加热的波-湍流驱动（WTD）模型的输入坡印廷通量，以及通过标度内边界磁场，改变沉积在日冕中的总热量。我们量化了模拟中磁场、热力学以及磁热综合效应的影响。研究发现，增加总热量会导致开放通量的大小更高，且在1.5至6个太阳半径（Rsun）范围内的K日冕中呈现更明显的开放白光形态。我们量化了等离子体β的演化及其如何驱动模拟间的形态差异。我们还将这些模拟与一个极高分辨率的参考解进行了比较，该参考解在表面边界条件中包含小尺度磁场信息。这一比较为低（较低）分辨率模型的“亚网格”修正的进一步发展提供了见解，以最佳地代表日冕和内日球层的结构与可观测特征。
英文摘要
The magnetic field of the Sun is a key driver of coronal heating and solar wind acceleration. In tandem, these influence the observable morphology of the corona, along with defining the magnetic connectivity and magnitude of open magnetic flux. Here,we investigate how coronal heating affects the magnetothermal state of the 3D global corona by analyzing a series of data-constrained, thermodynamic magnetohydrodynamic (MHD) simulations for solar minimum conditions. We vary the overall heat deposited in the corona via modifying the input Poynting flux of a wave-turbulence-driven (WTD) model for coronal heating and by scaling the inner boundary magnetic field. We quantify the magnetic, thermodynamic, and combined magnetothermal effects on our simulations. We find that increasing the overall amount of heat leads to a higher magnitude of open flux and a more visibly open white-light morphology in the K-Corona between 1.5 and 6 Rsun. We quantify how plasma beta evolves and drives morphological differences between simulations. We also compare these runs to an extremely high-resolution reference solution that includes small-scale magnetic information in the surface boundary condition. This latter comparison provides insight into the further development of 'subgrid' corrections for low(er) resolution models to best represent the structure and observables of the corona and inner heliosphere.
CommentsAccepted to ApJ
