Comparative Study of Data-driven Solar Coronal Field Models Using a Flux Emergence Simulation as a Ground-truth Data Set
Comparative Study of Data-driven Solar Coronal Field Models Using a Flux Emergence Simulation as a Ground-truth Data Set
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使用通量出现模拟作为地面实况数据集的数据驱动的太阳日冕场模型的比较研究
DOI：
10.3847/1538-4357/ab6b1f
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发表时间：
2020-01
影响因子：
4.9
通讯作者：
Inoue Satoshi
中科院分区：
文献类型：
--
作者：
Toriumi Shin;Takasao Shinsuke;Cheung Mark C. M.;Jiang Chaowei;Guo Yang;Hayashi Keiji;Inoue Satoshi
为了更好地了解日冕磁场以及耀斑和日冕物质抛射等动态活动，测量日冕磁场的时间演变并准确估计磁能是至关重要的。最近，一种新的建模技术，称为数据驱动的日冕场模型，其中的磁场的时间演化是由一系列的光球磁场和速度场的地图驱动，已被开发和揭示的耀斑生产活动区的动力学。在这里，我们报告的第一个定性和定量评估不同的数据驱动的模型使用磁通量出现模拟地面实况（GT）数据集。我们比较了GT场与由四种数据驱动算法从GT光球场重建的场。据发现，在最低限度，磁绳结构复制在所有的日冕场模型。然而，定量分析结果显示出一定程度的模型依赖性。在大多数情况下，磁能和相对磁螺旋度与GT值相当或至多为GT值的两倍。再生磁通绳具有各种尺寸的S形形状（与GT一致）、垂直站立的磁环或填充结构。观测到的差异可以归因于高度非力自由输入光球场，从日冕场重建，和建模的限制，如背景大气的处理，底部边界设置，和空间分辨率。
For a better understanding of the magnetic field in the solar corona and dynamic activities such as flares and coronal mass ejections, it is crucial to measure the time-evolving coronal field and accurately estimate the magnetic energy. Recently, a new modeling technique called the data-driven coronal field model, in which the time evolution of magnetic field is driven by a sequence of photospheric magnetic and velocity field maps, has been developed and revealed the dynamics of flare-productive active regions. Here we report on the first qualitative and quantitative assessment of different data-driven models using a magnetic flux emergence simulation as a ground-truth (GT) data set. We compare the GT field with those reconstructed from the GT photospheric field by four data-driven algorithms. It is found that, at minimum, the flux rope structure is reproduced in all coronal field models. Quantitatively, however, the results show a certain degree of model dependence. In most cases, the magnetic energies and relative magnetic helicity are comparable to or at most twice of the GT values. The reproduced flux ropes have a sigmoidal shape (consistent with GT) of various sizes, a vertically standing magnetic torus, or a packed structure. The observed discrepancies can be attributed to the highly non-force-free input photospheric field, from which the coronal field is reconstructed, and to the modeling constraints such as the treatment of background atmosphere, the bottom boundary setting, and the spatial resolution.
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太阳磁场模型和观测中的磁螺旋度估计。
影响因子：
10.3
作者：
Valori Gherardo;Pariat Etienne;Anfinogentov Sergey;Chen Feng;Georgoulis Manolis K.;Guo Yang;Liu Yang;Moraitis Kostas;Thalmann Julia K.;Yang Shangbin
通讯作者：
Yang Shangbin
影响因子：
2.8
作者：
W. Pesnell;B. Thompson;P. Chamberlin
通讯作者：
W. Pesnell;B. Thompson;P. Chamberlin
影响因子：
20.9
作者：
K. Shibata;T. Magara
通讯作者：
K. Shibata;T. Magara
DOI：
10.1086/175188
发表时间：
1995
期刊：
The Astrophysical Journal
影响因子：
--
作者：
T. Metcalf;L. Jiao;A. Mcclymont;R. Canfield;H. Uitenbroek
通讯作者：
T. Metcalf;L. Jiao;A. Mcclymont;R. Canfield;H. Uitenbroek
DOI：
10.1088/0004-637x/783/2/102
发表时间：
2013-12
期刊：
The Astrophysical Journal
影响因子：
--
作者：
A. Malanushenko;A. Malanushenko;C. Schrijver;M. DeRosa;M. Wheatland
通讯作者：
A. Malanushenko;A. Malanushenko;C. Schrijver;M. DeRosa;M. Wheatland