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Magnetic Buoyancy with Viscosity and Ohmic Dissipation and Flux Tube Formation

Published online by Cambridge University Press:  19 July 2016

V.D. Kuznetsov
V.D. Kuznetsov*
Affiliation:
IZMIRAN, Troitsk, Moscow Region 142092, USSR

Extract

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In the framework of the magnetohydrodynamic equations with dissipative terms in the form of turbulent viscosity (Vt) the linear stage of the instability of a subphotospheric field with respect to magnetic buoyancy is considered. For an exponential in z, isothermal plane-parallel atmosphere with a constant Alfvenic velocity the perturbations of the form are described by differential equation with constant coefficients. The qualitative dependence of the growth rate of instability on transverse wave number is determined (see Figures 1 and 2) and characteristic scales of the magnetic tubes are evaluated at the linear stage of instability (Kuznetsov, 1987, 1988).

Type
II. The Solar Interior
Information
Symposium - International Astronomical Union , Volume 142: Basic Plasma Processes on the Sun , 1990 , pp. 58 - 59
Copyright
Copyright © Kluwer 1990 

References

Kuznetsov, V.D. (1987) ‘A typical sizes of the flux tubes in the unstable atmosphere with turbulent viscosity and ohmic dissipation’, Magnitnaya Gidrodinamika 2, 13–18 (in Russian).Google Scholar
Kuznetsov, V.D. (1988) ‘Magnetic field fragmentation into flux tubes in sub photospheric layers of the Sun’, in: Mogilevskiy, E.I. (ed.), Fizika Solnechnoy Aktivnosti , Nauka, Moscow, pp. 30–35 (in Russian).Google Scholar
Parker, E.N. (1979) ‘Cosmical Magnetic Fields’ , Clarendon Press, Oxford.Google Scholar