Solar prominences: theory and models
Solar prominences: theory and models
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DOI：
10.1007/s41116-018-0016-2
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发表时间：
2018-10
影响因子：
20.9
通讯作者：
S. Gibson
中科院分区：
文献类型：
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作者：
S. Gibson
磁场将太阳能中相对较冷的物质悬浮在一个热的日冕中。要全面了解太阳的活动，最终需要复杂和动态的模型，并通过跨越太阳大气层的观测进行约束和验证。我们从观测中获得了这种理解的核心，这些观测给了我们关于支撑和围绕日珥的“磁骨架”结构的信息。然后，复杂的磁流体动力学模拟为骨架添加了血肉，演示了热变化等离子体如何脉冲通过以形成日珥，以及等离子体和磁场如何动态地相互作用。
Magnetic fields suspend the relatively cool material of solar prominences in an otherwise hot corona. A comprehensive understanding of solar prominences ultimately requires complex and dynamic models, constrained and validated by observations spanning the solar atmosphere. We obtain the core of this understanding from observations that give us information about the structure of the “magnetic skeleton” that supports and surrounds the prominence. Energetically-sophisticated magnetohydrodynamic simulations then add flesh and blood to the skeleton, demonstrating how a thermally varying plasma may pulse through to form the prominence, and how the plasma and magnetic fields dynamically interact.