Physics
Scientific paper
Jun 1986
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986soph..105..291m&link_type=abstract
Solar Physics (ISSN 0038-0938), vol. 105, June 1986, p. 291-306.
Physics
9
Magnetohydrodynamic Stability, Magnetohydrostatics, Plasma Equilibrium, Solar Corona, Boundary Value Problems, Euler-Lagrange Equation
Scientific paper
An energy method is used to determine a condition for local instability of field lines in magnetohydrostatic equilibrium which are rooted in the photosphere. The particular equilibrium studied is isothermal and two-dimensional and may model a coronal arcade of loops where varitions along the axis of the arcade are weak enough to be ignorable. It is found that when β < 0.34 the equilibrium is stable. When β = 0.34 a magnetic neutral line appears at the photosphere and it is marginally stable. When β > 0.34 a magnetic island is present and all the field lines inside the island are unstable as well as some beyond it. As β increases, the size of the island and the extent of unstable field lines increase. The effect of the instability is likely to be to create small-scale filamentation in the solar corona and to enhance the global transport coefficients.
Hood Alan William
Melville J. P.
Priest Eric R.
No associations
LandOfFree
The ideal magnetohydrodynamic stability of a line-tied coronal magnetohydrostatic equilibrium does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with The ideal magnetohydrodynamic stability of a line-tied coronal magnetohydrostatic equilibrium, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and The ideal magnetohydrodynamic stability of a line-tied coronal magnetohydrostatic equilibrium will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1834275