Emergence and interaction of twisted flux tubes in the Sun

被引:35
作者
Archontis, V. [1 ]
Hood, A. W. [1 ]
Brady, C. [1 ]
机构
[1] Univ St Andrews, Sch Math & Stat, St Andrews KY16 9SS, Fife, Scotland
基金
英国科学技术设施理事会;
关键词
Sun : magnetic fields; Sun : corona; magnetohydrodynamics (MHD);
D O I
10.1051/0004-6361:20066508
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
Aims. We present results from numerical simulations that study the interaction of a pair of twisted, buoyant magnetic flux tubes, which rise from the solar interior into the outer atmosphere of the Sun. The aim of our new model is to reproduce some of the dynamic solar phenomena in a self-consistent manner. Methods. We perform non-linear simulations in 2.5D numerical experiments by solving the compressible and resistive MHD equations using a Lagrangian remap, shock capturing code (Lare2D). For some aspects of the problem, we consider the evolution of the system using both uniform and locally enhanced resistivity. Results. The two flux tubes start to rise at the same time but from a different height below the photosphere. The leading ( first) tube, which is originally located nearer to the surface, rises and eventually expands above the photosphere forming a magnetized atmosphere for the upcoming system (second tube). Current sheets, high-velocity reconnection jets, plasmoids, loop brightnenings and arcade flare-like structures are formed, for the first time in such numerical experiments, self-consistently by the emergence, expansion and the dynamical interaction between the two emerging flux systems.
引用
收藏
页码:367 / 376
页数:10
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