光球与色球和日冕的耦合
Coupling from the photosphere to the chromosphere and the corona
摘要：
太阳大气层的特点是相互竞争的物理过程的复杂相互作用：对流，辐射，传导和磁场。在低层大气中，太阳对流及其过冲的最明显的印记是颗粒斑。除了这个主要的尺度之外，空间尺度的分布或多或少是平滑的，无论是朝向更小的尺度还是更大的尺度，使得太阳本质上是一个多尺度物体。对流和过冲使光球层有了自己的面孔，但也是上面的层，即色球层和日冕的驱动者。磁场的配置有效地耦合大气层在许多空间尺度上，例如，在环的形式，被锚定在对流区，并继续通过大气层进入色球层和日冕。磁场也是一个重要的结构剂的小，颗粒大小的规模，虽然（流体动力学）冲击波也发挥了重要作用-特别是在互联网的气氛中，大多数弱场占主导地位。根据最近的观测和数值模拟结果，我们试图提出一个全面的图片安静的太阳大气作为一个高度间歇性和动态系统。
英文摘要：
The atmosphere of the Sun is characterized by a complex interplay of competing physical processes: convection, radiation, conduction, and magnetic fields. The most obvious imprint of the solar convection and its overshooting in the low atmosphere is the granulation pattern. Beside this dominating scale there is a more or less smooth distribution of spatial scales, both towards smaller and larger scales, making the Sun essentially a multi-scale object. Convection and overshooting give the photosphere its face but also act as drivers for the layers above, namely the chromosphere and corona. The magnetic field configuration effectively couples the atmospheric layers on a multitude of spatial scales, for instance in the form of loops that are anchored in the convection zone and continue through the atmosphere up into the chromosphere and corona. The magnetic field is also an important structuring agent for the small, granulation-size scales, although (hydrodynamic) shock waves also play an important role -- especially in the internetwork atmosphere where mostly weak fields prevail. Based on recent results from observations and numerical simulations, we attempt to present a comprehensive picture of the atmosphere of the quiet Sun as a highly intermittent and dynamic system.
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