Numerical simulations of magnetic Kelvin-Helmholtz instability at a twisted solar flux tube

被引：8
|
作者：
Murawski, K. [1 ]
Chmielewski, P. [1 ,2 ]
Zaqarashvili, T. V. [3 ,4 ,5 ]
Khomenko, E. [6 ]
机构：
[1] UMCS, Grp Astrophys, Ul Radziszewskiego 10, PL-20031 Lublin, Poland
[2] Inst Plasma Phys & Laser Microfus, Hery St 23, PL-01497 Warsaw, Poland
[3] Graz Univ, Inst Phys, IGAM, Univ Pl 5, A-8010 Graz, Austria
[4] Ilia State Univ, Abastumani Astrophys Observ, GE-0162 Tbilisi, Georgia
[5] Austrian Acad Sci, Space Res Inst, Schmiedlstr 6, A-8042 Graz, Austria
[6] Inst Astrofis Canarias, E-38205 Tenerife, Spain
来源：
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2016年 / 459卷 / 03期
基金：
奥地利科学基金会;
关键词：
Sun:; atmosphere; TORSIONAL ALFVEN WAVES; STAGGERED MESH SCHEME; DYNAMICS; CORONA; STABILITY; DRIVEN;
D O I：
10.1093/mnras/stw703
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
The paper aims to study the response of a solar small-scale and weak magnetic flux tube to photospheric twisting motions. We numerically solve three-dimensional ideal magnetohydrodynamic equations to describe the evolution of the perturbation within the initially static flux tube, excited by twists in the azimuthal component of the velocity. These twists produce rotation of the magnetic field lines. Perturbation of magnetic field lines propagates upwardly, driving vertical and azimuthal flow as well as plasma compressions and rarefactions in the form of eddies. We conclude that these eddies result from the sheared azimuthal flow which seeds Kelvin-Helmholtz instability (KHI) between the flux tube and the ambient medium. Numerically obtained properties of the KHI confirm the analytical predictions for the occurrence of the instability.
引用
收藏
页码：2566 / 2572
页数：7
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