Effects of flows on viscous and resistive MHD stability

Details Effects of flows on viscous and resistive MHD stability Effects of flows on viscous and resistive MHD stability

Dec 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986nascp2442..465e&link_type=abstract

In NASA. Goddard Space Flight Center Coronal and Prominence Plasmas p 465-468 (SEE N87-20871 13-92)

Physics

Fluid Flow, Magnetohydrodynamic Stability, Mathematical Models, Plasmas (Physics), Solar Corona, Viscosity, Flow Resistance, Magnetic Fields, Nonlinear Equations, Turbulence

Scientific paper

In many solar applications the viscosity appears to be more important than resistivity. In order to discuss the instabilities in solar conditions, an idealized configuration is considered in which the plasma is flowing in the z-direction along the magnetic field B0 with a velocity V0. As far as the velocity is concerned two different velocity profiles, with different hydrodynmaic stability properties are discussed. The results are summarized.

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