The Physics of Quiet Sun Magnetic Fields

安静太阳磁场的物理学

• 批准号: 0737836
• 负责人: William Abbett
• 金额: $ 31.11万
• 依托单位: University of California-Berkeley
• 依托单位国家: 美国
• 项目类别: Continuing Grant
• 财政年份: 2007
• 资助国家: 美国
• 起止时间: 2007-11-01 至 2011-10-31
• 项目状态: 已结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=0737836&HistoricalAwards=false
• 关键词: Physics; Quiet; Sun; Magnetic; Fields

The Principal Investigator (PI) plans to study the origin and evolution of the Quiet Sun magnetic field and atmosphere by performing 3D magnetohydrodynamic simulations of the combined convection zone-to-corona system. The computational domain will include the highly stratified layers of the upper convection zone, photosphere, chromosphere, transition region, and low-corona (from approximately 3 Mm below the visible surface, out to the low-density, magnetically-dominated corona). The proposing team will develop a new numerical code, capable of simultaneously evolving these spatially and temporally disparate regimes, to address whether the magnetic field generated by a convective surface dynamo can account for the observed properties of the Quiet Sun magnetic field and atmosphere. The new code would also model the magnetic connectivity between sub-surface magnetic structures and the magnetic field that fills the solar corona. The investigators will study the sizes and spatial distribution of magnetic elements in the combined system, the topological evolution of the magnetized corona, the energy and magnetic helicity transport through the solar atmosphere, the dissipation of energy in the corona, and the radiative energies and diagnostics from the corona and other layers of the atmosphere. The simulated datasets that will result from this study can be used to directly test helioseismic inversion techniques, commonly-used velocity inversion techniques designed to obtain surface flows, and the many extrapolation techniques used to characterize the magnetic structure of the solar corona. In addition, the studies outlined in this proposal will greatly aid in the analysis and interpretation of high-resolution observations obtained by instruments such as Hinode, SDO, SOLIS, and ATST.

首席研究员 (PI) 计划通过对对流区到日冕组合系统进行 3D 磁流体动力学模拟，研究安静太阳磁场和大气的起源和演化。计算域将包括上对流区、光球层、色球层、过渡区和低日冕（从可见表面以下约 3 Mm 处，到低密度、磁主导日冕）的高度分层层。提议团队将开发一种新的数字代码，能够同时演化这些空间和时间上不同的状态，以解决对流表面发电机产生的磁场是否可以解释观察到的安静太阳磁场和大气的特性。新代码还将模拟地下磁结构与填充日冕的磁场之间的磁连通性。 研究人员将研究组合系统中磁性元素的尺寸和空间分布、磁化日冕的拓扑演化、穿过太阳大气的能量和磁螺旋度传输、日冕中的能量耗散，以及日冕和大气层其他层的辐射能量和诊断。这项研究产生的模拟数据集可用于直接测试日震反演技术、旨在获得表面流的常用速度反演技术以及用于表征日冕磁结构的许多外推技术。此外，本提案中概述的研究将极大地有助于分析和解释由 Hinode、SDO、SOLIS 和 ATST 等仪器获得的高分辨率观测结果。