On potential field models of the solar corona
On potential field models of the solar corona
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DOI：
10.1086/171430
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发表时间：
1992-06
期刊：
影响因子：
--
通讯作者：
Y.-M. Wang;N. Sheeley
中科院分区：
文献类型：
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作者：
Y.-M. Wang;N. Sheeley
无电流近似已被广泛应用于从磁图观测推断日冕的磁结构。在这种计算中，势场通常与观测到的光球场的视距分量直接匹配。然而，这种方法是无效的，因为磁图测量适用于深大气层，那里的磁场是非电位的，（对于在Fe I λ5250线上进行的观测）几乎是径向的。一种更好的方法是只将势场的径向分量与光球数据相匹配（假设场线是径向取向的，对视线投影进行了校正），同时允许切向场分量的不连续
The current-free approximation has been widely used to infer the magnetic structure of the solar corona from magnetograph observations. In such calculations, the potential field is usually matched directly to the observed line-of-sight component of the photospheric field. However, this procedure is invalid because the magnetograph measurements apply to deep atmospheric layers where the magnetic field is nonpotential and (for observations made in the Fe I λ5250 line) nearly radial. A better approach is to match only the radial component of the potential field to the photospheric data (corrected for line-of-sight projection on the assumption that the field lines are radially oriented), while allowing a discontinuity in the tangential field components