Validation of MHD Model Predictions of the Corona with LASCO-C2 Polarized Brightness Images
Validation of MHD Model Predictions of the Corona with LASCO-C2 Polarized Brightness Images
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DOI：
10.1007/s11207-019-1549-9
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发表时间：
2019-11
期刊：
影响因子：
2.8
通讯作者：
P. Lamy;O. Floyd;Z. Mikić;P. Riley
中科院分区：
文献类型：
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作者：
P. Lamy;O. Floyd;Z. Mikić;P. Riley
在我们对日冕的理解方面取得进展，需要将由测量磁场驱动的先进磁流体动力学模型的结果，特别是基本的加热模型，与日冕观测进行彻底的比较。到目前为止，比较主要涉及日冕的全球形态，从模型计算的合成图像与观测图像进行比较。我们更进一步，通过使用MHD模型产生的三维电子密度计算的偏振辐射与由LASCO-C2日冕仪获得的经过良好校准的偏振图像之间进行详细的定量比较，并辅之以来自莫纳罗亚太阳观测站Mark IV和K-Cor仪器的地面图像，以将比较扩展到内日冕区域1.0 - 2.5，C2无法访问。我们利用对几次日食进行的高分辨率和高质量MHD预测（2008年8月1日、2010年7月11日、2012年11月13日、和2017年8月21日）以及帕克太阳探测器的第一次近日点通过（2018年11月5日）使用两种不同的三维MHD模型，依靠热力学或波湍流驱动的方法来加热日冕。这两种模型一般都能够匹配观测到的日冕结构和光度学，尽管保真度不同，但没有明显的解释。然而，出现了两个限制，最大类型的日冕的复杂性和时间间隔之间完成的磁力测量和预测。
Progress in our understanding of the solar corona requires that the results of advanced magnetohydrodynamic models driven by measured magnetic fields, and particularly the underlying heating models, be thoroughly compared with coronal observations. The comparison has so far mainly concerned the global morphology of the corona, synthetic images calculated from the models being compared with observed images. We go one step further by performing detailed quantitative comparisons between the calculated polarized radianceusing the three-dimensional electron density produced by MHD models and well calibrated polarized images obtained by theLarge Angle Spectrometric CoronagraphLASCO-C2 coronagraph complemented by ground-based images when available from theMauna Loa Solar ObservatoryMark IV and K-Cor instruments to extend the comparison to the inner coronal region 1.0 – 2.5, which is inaccessible to C2. We take advantage of the high-resolution and high-quality MHD predictions performed for several solar eclipses (1 August 2008, 11 July 2010, 13 November 2012, and 21 August 2017) and for the first perihelion passage of theParker Solar Probe(5 November 2018) using two different three-dimensional MHD models relying on either a thermodynamic or a wave-turbulence-driven methodologies to heat the corona. Both models are generally able to match the observed structure and photometry of the corona albeit with various degrees of fidelity for which there is no obvious explanation. However, two limitations emerge, the complexity of coronae of the maximum type and the time lapse between the completion of the magnetograph measurements and the prediction.