A quantitative method to optimise magnetic field line fitting of observed coronal loops

被引:39
作者
Carcedo, L [1 ]
Brown, DS
Hood, AW
Neukirch, T
Wiegelmann, T
机构
[1] Univ St Andrews, Sch Math & Stat, St Andrews KY16 9SS, Fife, Scotland
[2] Max Planck Inst Aeron, D-37191 Katlenburg Lindau, Germany
关键词
D O I
10.1023/B:SOLA.0000013045.65499.da
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
Many authors use magnetic-field models to extrapolate the field in the solar corona from magnetic data in the photosphere. The accuracy of such extrapolations is usually judged qualitatively by eye, where a less judgemental quantitative approach would be more desirable. In this paper, a robust method for obtaining the best fit between a theoretical magnetic field and intensity observations of coronal loops on the solar disk will be presented. The method will be applied to Yohkoh data using a linear force-free field as an illustration. Any other theoretical model for the magnetic field can be used, provided there is enough freedom in the model to optimize the fit.
引用
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页码:29 / 40
页数:12
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