测量太阳磁性的隐藏方面
Measuring the Hidden Aspects of Solar Magnetism
摘要：
2008年是天体物理学磁场发现100周年，当时乔治·埃勒里·黑尔记录了太阳黑子中谱线的塞曼分裂。随着巴布科克的光电磁力仪的引入，人们很快就清楚地看到，太阳黑子外的太阳磁场是极其结构化的。当空间分辨率提高时，所测量的场强被发现变得更大。因此，有必要提出超越空间分辨率极限的方法，并在不依赖所用望远镜质量的情况下诊断固有磁场特性。线比技术是在20世纪70年代初发展起来的，它揭示了这样一幅图景：我们在磁图中看到的大部分磁通量都起源于高度成束的、具有微小体积填充因子的千克场。这导致了对嵌入在相当无场介质中的离散强场磁通量管的解释，以及整个行业的磁通量管模型越来越复杂。随着高精度成像偏振仪的出现，这种磁场模式现在已经被打破，这种偏振仪使我们能够应用所谓的“第二太阳光谱”来诊断塞曼诊断法所隐藏的太阳磁场方面。据发现，光球体积的大部分是沸腾与中等强度，纠缠领域。在新的范例中，该领域表现得像一个具有高度自相似性的分形，跨越约8个数量级的规模大小，下至10米的规模。
英文摘要：
2008 marks the 100th anniversary of the discovery of astrophysical magnetic fields, when George Ellery Hale recorded the Zeeman splitting of spectral lines in sunspots. With the introduction of Babcock's photoelectric magnetograph it soon became clear that the Sun's magnetic field outside sunspots is extremely structured. The field strengths that were measured were found to get larger when the spatial resolution was improved. It was therefore necessary to come up with methods to go beyond the spatial resolution limit and diagnose the intrinsic magnetic-field properties without dependence on the quality of the telescope used. The line-ratio technique that was developed in the early 1970s revealed a picture where most flux that we see in magnetograms originates in highly bundled, kG fields with a tiny volume filling factor. This led to interpretations in terms of discrete, strong-field magnetic flux tubes embedded in a rather field-free medium, and a whole industry of flux tube models at increasing levels of sophistication. This magnetic-field paradigm has now been shattered with the advent of high-precision imaging polarimeters that allow us to apply the so-called "Second Solar Spectrum" to diagnose aspects of solar magnetism that have been hidden to Zeeman diagnostics. It is found that the bulk of the photospheric volume is seething with intermediately strong, tangled fields. In the new paradigm the field behaves like a fractal with a high degree of self-similarity, spanning about 8 orders of magnitude in scale size, down to scales of order 10 m.
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