We review the properties of solar magneto-convection in the top half of the convection zones scale heights (from 20 Mm below the visible surface to the surface, and then through the photosphere to the temperature minimum). Convection is a highly non-linear and nonlocal process, so it is best studied by numerical simulations. We focus on simulations that include sufficient detailed physics so that their results can be quantitatively compared with observations.The solar surface is covered with magnetic features with spatial sizes ranging from unobservably small to hundreds of megameters. Three orders of magnitude more magnetic flux emerges in the quiet Sun than emerges in active regions. In this review we focus mainly on the properties of the quiet Sun magnetic field.The Sun's magnetic field is produced by dynamo action throughout the convection zone, primarily by stretching and twisting in the turbulent downflows. Diverging convective upflows and magnetic buoyancy carry magnetic flux toward the surface and sweep the field into the surrounding downflow lanes where the field is dragged downward. The result is a hierarchy of undulating magnetic Ω- and U-loops of different sizes. New magnetic flux first appears at the surface in a mixed polarity random pattern and then collects into isolated unipolar regions due to underlying larger scale magnetic structures. Rising magnetic structures are not coherent, but develop a filamentary structure. Emerging magnetic flux alters the convection properties, producing larger, darker granules.Strong field concentrations inhibit transverse plasma motions and, as a result, reduce convective heat transport toward the surface which cools. Being cooler, these magnetic field concentrations have a shorter scale height and become evacuated. The field becomes further compressed and can reach strengths in balance with the surrounding gas pressure. Because of their small internal density, photons escape from deeper in the atmosphere. Narrow evacuated field concentrations get heated from their hot sidewalls and become brighter than their surroundings. Wider magnetic concentrations are not heated so they become darker, forming pores and sunspots.

中文翻译：

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太阳表面磁对流

我们回顾了对流区上半部分尺度高度（从可见表面以下20 Mm到表面，然后穿过光球到最低温度）的太阳磁对流特性。对流是一个高度非线性且非局部的过程，因此最好通过数值模拟进行研究。我们专注于包含足够详细的物理过程的模拟，以便可以将其结果与观察结果进行定量比较。太阳表面覆盖有磁特征，其空间大小从不可观察的小到数百兆米不等。在安静的太阳中产生的磁通量比在活动区域​​中产生的磁通量多三个数量级。在这篇评论中，我们主要关注安静的太阳磁场的性质。整个对流区中的发电机作用产生磁场，主要是通过湍流向下流的拉伸和扭曲。对流上升气流和磁力浮力使磁通流向地面，并将磁场扫入周围的下降流道，在该处向下拖动磁场。结果是起伏的电磁Ω-和ü-不同大小的环。新的磁通量首先以混合极性随机模式出现在表面，然后由于下方较大的磁性结构而聚集到孤立的单极区域中。上升的磁性结构不是相干的，而是形成丝状结构。新兴的磁通量改变了对流特性，产生了更大，更暗的颗粒。强磁场集中会抑制等离子体的横向运动，并因此减少对流向冷却表面的对流热传递。这些磁场集中度较低时，它们的标尺高度较短，并且被抽成真空。磁场被进一步压缩，并可以达到与周围气压平衡的强度。由于其内部密度小，光子会从更深的大气层中逸出。狭窄的疏散场集中度从其热侧壁被加热，并变得比周围环境明亮。较宽的磁场浓度不会被加热，因此会变得更暗，形成毛孔和黑子。