非分辨色球磁场的偏振诊断
Polarimetric Diagnostics of Unresolved Chromospheric Magnetic Fields
摘要：
近十年来，HeI 10830的分光偏振测量一直被应用于太阳色球层的磁诊断。这种共振线是非常通用的，因为它在盘和离臂结构中都是可见的，并且它对弱场汉勒效应和强场塞曼效应都具有良好的灵敏度。最近对活动区灯丝的观测表明，线偏振主要是由横向塞曼效应决定的，几乎没有或根本没有散射偏振。这是令人惊讶的，因为在传统的散射情况下，HeI水平应该是显著极化的。为了解释所观察到的碰撞或辐射过程引起的原子去极化水平，人们必须引用比目前已知的双折射值大几个数量级的等离子体密度。我们表明，这种去极化可以很自然地解释的存在下，一个未解决的，高度纠缠的磁场，平均给有序的领域推断光谱偏振数据，在典型的时间和空间尺度的观测。在这种情况下，我们提出了一个模型的极化HeI 10830，并讨论了其影响的磁诊断的双折射和针状，并在太阳大气中的未解决的磁场分布的一般研究。
英文摘要：
For about a decade, spectro-polarimetry of HeI 10830 has been applied to the magnetic diagnostics of the solar chromosphere. This resonance line is very versatile, as it is visible both on disk and in off-limb structures, and it has a good sensitivity to both the weak-field Hanle effect and the strong-field Zeeman effect. Recent observations of an active-region filament showed that the linear polarization was dominated by the transverse Zeeman effect, with very little or no hint of scattering polarization. This is surprising, since the HeI levels should be significantly polarized in a conventional scattering scenario. To explain the observed level of atomic depolarization by collisional or radiative processes, one must invoke plasma densities larger by several orders of magnitude than currently known values for prominences. We show that such depolarization can be explained quite naturally by the presence of an unresolved, highly entangled magnetic field, which averages to give the ordered field inferred from spectro-polarimetric data, over the typical temporal and spatial scales of the observations. We present a modeling of the polarized HeI 10830 in this scenario, and discuss its implications for the magnetic diagnostics of prominences and spicules, and for the general study of unresolved magnetic field distributions in the solar atmosphere.
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