Local Helioseismology of Sunspots: Current Status and Perspectives
Local Helioseismology of Sunspots: Current Status and Perspectives
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DOI：
10.1007/s11207-012-9996-6
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发表时间：
2010-10
期刊：
影响因子：
2.8
通讯作者：
A. Kosovichev
中科院分区：
文献类型：
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作者：
A. Kosovichev
太阳黑子的形成机制和稳定性是太阳物理学和天体物理学中最长久、最有趣的谜题之一。太阳黑子受地下动力学控制，无法直接观测。近年来，通过数值模拟和局部日震学的研究，我们对强场湍流磁化等离子体的物理性质的认识取得了实质性进展。模拟和日震测量都极具挑战性，但越来越清楚的是，理解太阳黑子之谜的关键是模型和观测之间的协同作用。最近的观测和辐射MHD数值模式对太阳黑子半影中的Evershed流提供了令人信服的解释。此外，它们还导致了对太阳黑子的理解，即在上层对流区湍流等离子体中自组织的磁结构，这是由大规模动力学维持的。太阳黑子的局部日震诊断仍有许多不确定因素，本文对其中的一些不确定因素进行了讨论。然而，在解决这些不确定性、通过新的高分辨率观测验证基本结果、通过数值模拟测试日震技术以及比较不同方法获得的结果等方面已经取得了重大成就。例如，最近对hinospace任务的日震学数据的分析成功地解决了几个不确定性和担忧（如倾斜场和相速过滤效应），这些不确定性和担忧可能会影响对太阳黑子的地下波速结构和流模式的推断。为了更好地理解太阳黑子现象，进一步改进日震学方法，研究太阳活动区域从磁通量产生到耗散的整个生命周期是非常重要的。太阳动力学观测任务已经开始为此类调查提供数据。
Mechanisms of the formation and stability of sunspots are among the longest-standing and intriguing puzzles of solar physics and astrophysics. Sunspots are controlled by subsurface dynamics, hidden from direct observations. Recently, substantial progress in our understanding of the physics of the turbulent magnetized plasma in strong-field regions has been made by using numerical simulations and local helioseismology. Both the simulations and helioseismic measurements are extremely challenging, but it is becoming clear that the key to understanding the enigma of sunspots is a synergy between models and observations. Recent observations and radiative MHD numerical models have provided a convincing explanation for the Evershed flows in sunspot penumbrae. Also, they lead to the understanding of sunspots as self-organized magnetic structures in the turbulent plasma of the upper convection zone, which are maintained by a large-scale dynamics. Local helioseismic diagnostics of sunspots still have many uncertainties, some of which are discussed in this review. However, there have been significant achievements in resolving these uncertainties, verifying the basic results by new high-resolution observations, testing the helioseismic techniques by numerical simulations, and comparing results obtained by different methods. For instance, a recent analysis of helioseismology data from theHinodespace mission has successfully resolved several uncertainties and concerns (such as the inclined-field and phase-speed filtering effects) that might affect the inferences of the subsurface wave-speed structure of sunspots and the flow pattern. It is becoming clear that for the understanding of the phenomenon of sunspots it is important to further improve the helioseismology methods and investigate the whole life cycle of active regions, from magnetic flux emergence to dissipation. TheSolar Dynamics Observatorymission has started to provide data for such investigations.