毫米波长太阳的网间区域
Inter-network regions of the Sun at millimetre wavelengths
摘要：
波长在1毫米左右的连续强度提供了一个很好的方式来探测太阳色球层。未来的高分辨率毫米阵列，如阿塔卡马大型毫米阵列（ALMA），将为正在进行的关于这一层的热结构和动力学的争论提供宝贵的投入。合成亮温图计算的基础上的三维辐射（磁）流体动力学（MHD）模拟。虽然0.3毫米的毫米连续谱主要来自上层光球层，但这里考虑的较长波长映射了低层和中层色球层。有效的形成高度一般随波长增加，也从磁盘中心向太阳翼。平均强度贡献函数通常是相当宽的，在某些情况下，它们甚至是双峰的，因为在模型色球层中有来自热激波和冷激波后区域的贡献。考虑到氢离子化平衡的偏差，电子密度和光学深度的变化不太强烈。其结果是更窄的地层高度范围。平均亮温随波长的增加而增加，并向临边方向增加。相对对比度以与平均强度相同的方式取决于波长，但是朝向肢体减小。亮温分布对波长和盘位置的依赖性可以用模式大气中形成高度的差异和温度起伏随高度的变化来解释。
英文摘要：
The continuum intensity at wavelengths around 1 mm provides an excellent way to probe the solar chromosphere. Future high-resolution millimetre arrays, such as the Atacama Large Millimeter Array (ALMA), will thus produce valuable input for the ongoing controversy on the thermal structure and the dynamics of this layer. Synthetic brightness temperature maps are calculated on basis of three-dimensional radiation (magneto-)hydrodynamic (MHD) simulations. While the millimetre continuum at 0.3mm originates mainly from the upper photosphere, the longer wavelengths considered here map the low and middle chromosphere. The effective formation height increases generally with wavelength and also from disk-centre towards the solar limb. The average intensity contribution functions are usually rather broad and in some cases they are even double-peaked as there are contributions from hot shock waves and cool post-shock regions in the model chromosphere. Taking into account the deviations from ionisation equilibrium for hydrogen gives a less strong variation of the electron density and with it of the optical depth. The result is a narrower formation height range. The average brightness temperature increases with wavelength and towards the limb. The relative contrast depends on wavelength in the same way as the average intensity but decreases towards the limb. The dependence of the brightness temperature distribution on wavelength and disk-position can be explained with the differences in formation height and the variation of temperature fluctuations with height in the model atmospheres.
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