模拟太阳活动区的微波偏振成像光谱日冕磁象
Coronal Magnetography of a Simulated Solar Active Region from Microwave Imaging Spectropolarimetry
摘要：
我们模拟了扩展欧文斯谷太阳能阵列（EOVSA）无线电图像产生的多个频率从一个模型太阳活动区，嵌入在一个现实的太阳盘模型，并探讨了不同的光谱分析方案，以评估实现EOVSA的最重要的科学目标之一-日冕磁图的潜力所产生的数据立方体。在本文中，我们专注于模拟的回旋共振和自由-自由辐射从磁盘上的太阳活动区模型与现实的复杂性，在电子密度，温度和磁场分布。我们比较磁场参数外推的图像数据立方体沿视线后，折叠通过EOVSA仪器配置文件与原始（展开）的参数中使用的模型。我们发现，即使是最容易自动化的，基于图像的分析方法（0级）提供合理的定量结果，虽然他们受到系统的影响，由于有限的采样在傅立叶（UV）平面。最后，我们注意到潜在的错误，由于错误识别谐波的陀螺仪频率，并讨论了应用更复杂的基于光谱的分析方案（1级），以解决问题的情况下，改善紫外线覆盖和空间分辨率的前景。
英文摘要：
We have simulated the Expanded Owens Valley Solar Array (EOVSA) radio images generated at multiple frequencies from a model solar active region, embedded in a realistic solar disk model, and explored the resulting datacube for different spectral analysis schemes to evaluate the potential for realizing one of EOVSA's most important scientific goals--coronal magnetography. In this paper, we focus on modeling the gyroresonance and free-free emission from an on-disk solar active region model with realistic complexities in electron density, temperature and magnetic field distribution. We compare the magnetic field parameters extrapolated from the image datacube along each line of sight after folding through the EOVSA instrumental profile with the original (unfolded) parameters used in the model. We find that even the most easily automated, image-based analysis approach (Level 0) provides reasonable quantitative results, although they are affected by systematic effects due to finite sampling in the Fourier (uv) plane. Finally, we note the potential for errors due to misidentified harmonics of the gyrofrequency, and discuss the prospects for applying a more sophisticated spectrally-based analysis scheme (Level 1) to resolve the issue in cases where improved uv coverage and spatial resolution are available.
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