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Article information
2001 , Volume 6, ¹ 6, p.81-92
Romanov D.V., Romanov K.V.
Numerical modelling of development of thin magnetic tube slow wave instability in convection zone of the Sun
Magnetohydrodynamics of instability of thin magnetic tube within the limits of convective zone of the Sun is investigated in the paper. It is shown that slow wave instability is determining factor for the tube evolution. Slow wave instability leads to the strong changing of tube geometry, where the parts, which are emerging to the solar surface, and the parts, which are fixing near the bottom of convection zone, are segregated. Typical time of slow wave instability development can be significantly smaller, than the time of magnetic field confinement, which is found by calculations with use of one-dimensional models. The fixation of some tubes near the bottom of convection zone and the presence of differential rotation explicate the motion of the observed magnetic structures with respect to the sun surface.
[full text] Classificator Msc2000:- *76M20 Finite difference methods
- 76W05 Magnetohydrodynamics and electrohydrodynamics
- 85A30 Hydrodynamic and hydromagnetic problems
Keywords: solar convective zone, flux tube, solar modeling, magnetic flux storage, chromosphere, magnetohydrodynamics
Author(s):
Romanov D V
Office: Krasnoyarsk State Economic Institute
Address: Russia, Krasnoyarsk
E-mail: ds@kgtei.kts.ru
Romanov KonstantinV.
PhD.
Office: Krasnoyarsk State University of Railways Transport
Address: Russia, Krasnoyarsk
Bibliography link:
Romanov D.V., Romanov K.V. Numerical modelling of development of thin magnetic tube slow wave instability in convection zone of the Sun // Computational technologies. 2001. V. 6. ¹ 6. P. 81-92
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