ALMA是太阳色球层的理想探测器
ALMA as the ideal probe of the solar chromosphere
摘要：
太阳色球层的本质，它的结构和动力学，仍然远远没有得到正确的理解，尽管密集的研究。在这里，我们指出了在毫米波长的色球观测解决这个长期存在的问题的潜力。利用Carlsson和Stein提出的太阳色球层复杂动态模型进行的计算表明，毫米辐射对色球层中的动态过程极其敏感，寻找动态特征的适当波长在0.8-5.0毫米范围内。该模型还表明，ALMA将提供的毫米波长高分辨率观测，将具有对热气体和冷气体都起反应的独特性质，因此将具有区分太阳大气的竞争模型的潜力。因此，用BIMA阵列（分辨率为12角秒）在3.5毫米处对安静太阳进行观测所获得的初步结果显示出幅度为50-150 K、频率为1.5-8 mHz的显著振荡，其趋势是网络间的短周期振荡和网络区域的长周期振荡。然而，需要更高的空间分辨率，如ALMA提供的分辨率，才能清楚地区分太阳大气层内的特征，并与综合动态模拟的输出进行充分的比较。
英文摘要：
The very nature of the solar chromosphere, its structuring and dynamics, remains far from being properly understood, in spite of intensive research. Here we point out the potential of chromospheric observations at millimeter wavelengths to resolve this long-standing problem. Computations carried out with a sophisticated dynamic model of the solar chromosphere due to Carlsson and Stein demonstrate that millimeter emission is extremely sensitive to dynamic processes in the chromosphere and the appropriate wavelengths to look for dynamic signatures are in the range 0.8-5.0 mm. The model also suggests that high resolution observations at mm wavelengths, as will be provided by ALMA, will have the unique property of reacting to both the hot and the cool gas, and thus will have the potential of distinguishing between rival models of the solar atmosphere. Thus, initial results obtained from the observations of the quiet Sun at 3.5 mm with the BIMA array (resolution of 12 arcsec) reveal significant oscillations with amplitudes of 50-150 K and frequencies of 1.5-8 mHz with a tendency toward short-period oscillations in internetwork and longer periods in network regions. However higher spatial resolution, such as that provided by ALMA, is required for a clean separation between the features within the solar atmosphere and for an adequate comparison with the output of the comprehensive dynamic simulations.
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