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Sunspot Modeling: From Simplified Models to Radiative MHD Simulations
Living Reviews in Solar Physics ( IF 23.0 ) Pub Date : 2011-12-01 , DOI: 10.12942/lrsp-2011-3
Matthias Rempel , Rolf Schlichenmaier

We review our current understanding of sunspots from the scales of their fine structure to their large scale (global) structure including the processes of their formation and decay. Recently, sunspot models have undergone a dramatic change. In the past, several aspects of sunspot structure have been addressed by static MHD models with parametrized energy transport. Models of sunspot fine structure have been relying heavily on strong assumptions about flow and field geometry (e.g., flux-tubes, “gaps”, convective rolls), which were motivated in part by the observed filamentary structure of penumbrae or the necessity of explaining the substantial energy transport required to maintain the penumbral brightness. However, none of these models could self-consistently explain all aspects of penumbral structure (energy transport, filamentation, Evershed flow). In recent years, 3D radiative MHD simulations have been advanced dramatically to the point at which models of complete sunspots with sufficient resolution to capture sunspot fine structure are feasible. Here, overturning convection is the central element responsible for energy transport, filamentation leading to fine structure, and the driving of strong outflows. On the larger scale these models are also in the progress of addressing the subsurface structure of sunspots as well as sunspot formation. With this shift in modeling capabilities and the recent advances in high resolution observations, the future research will be guided by comparing observation and theory.

中文翻译:

太阳黑子建模:从简化模型到辐射MHD模拟

我们从黑点的精细结构到大型(全局)结构,包括其形成和衰变过程,回顾了当前对黑子的理解。最近,黑子模型发生了翻天覆地的变化。过去,具有参数化能量传输的静态MHD模型已经解决了黑子结构的几个方面。太阳黑子的精细结构模型在很大程度上依赖于关于流场和场几何的强大假设(例如,通量管,“缝隙”,对流辊),其部分原因是所观察到的半影的丝状结构或解释其原因。维持半影亮度所需的大量能量传输。但是,这些模型都无法自洽地解释半影结构的各个方面(能量传输,细丝化,流出)。近年来,3D辐射MHD模拟已经得到了极大的发展,以至于具有足够分辨率以捕获黑子细微结构的完整黑子模型是可行的。在这里,翻转对流是负责能量传输,细丝化导致精细结构以及驱动强烈流出的主要因素。在更大范围内,这些模型也正在研究黑子的地下结构以及黑子的形成。随着建模能力的这种转变以及高分辨率观测的最新进展,未来的研究将通过比较观测和理论来指导。3D辐射MHD模拟已经得到了极大的发展,以至于具有足够分辨率以捕获黑子精细结构的完整黑子模型是可行的。在这里,翻转对流是负责能量传输,细丝化导致精细结构以及驱动强烈流出的主要因素。在更大范围内,这些模型也正在研究黑子的地下结构以及黑子的形成。随着建模能力的这种转变以及高分辨率观测的最新进展,未来的研究将通过比较观测和理论来指导。3D辐射MHD模拟已经得到了极大的发展,以至于具有足够分辨率以捕获黑子精细结构的完整黑子模型是可行的。在这里,翻转对流是负责能量传输,细丝化导致精细结构以及驱动强烈流出的主要因素。在更大范围内,这些模型也正在研究黑子的地下结构以及黑子的形成。随着建模能力的这种转变以及高分辨率观测的最新进展,未来的研究将通过比较观测和理论来指导。在更大范围内,这些模型也正在研究黑子的地下结构以及黑子的形成。随着建模能力的这种转变以及高分辨率观测的最新进展,未来的研究将通过比较观测和理论来指导。在更大范围内,这些模型也正在研究黑子的地下结构以及黑子的形成。随着建模能力的这种转变以及高分辨率观测的最新进展,未来的研究将通过比较观测和理论来指导。
更新日期:2011-12-01
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