A W Hood 1992 Plasma Phys. Control. Fusion 34 411 doi:10.1088/0741-3335/34/4/002
A W Hood
Show affiliationsThe review begins with an introduction to some of the various solar phenomena that may be investigated using stability theory. The geometry of the coronal magnetic field for many models is either a loop or an arcade and it is the stability properties of these structures that are investigated. The author presents a simple physical description of the basic MHD instabilities and describes the main difference between laboratory and coronal plasmas due to the presence of an extremely dense plasma at the footpoints of the coronal magnetic fieldlines. The implications of this density interface are discussed. Linear stability theory is applied to some solar situations and some non-linear simulations are discussed.
95.30.Qd Magnetohydrodynamics and plasmas
96.60.Hv Electric and magnetic fields
Issue 4 (April 1992)
A W Hood 1992 Plasma Phys. Control. Fusion 34 411
S P Collins et al 2009 J. Phys.: Conf. Ser. 190 012045
J A Foxman and J M Robbins 2005 Nonlinearity 18 2775
Evgueni Kleimenov et al 2009 J. Phys.: Conf. Ser. 190 012035
S V Gupta 2004 Metrologia 41 361
The ALICE Collaboration et al 2008 JINST 3 S08002
M I Boyanov et al 2009 J. Phys.: Conf. Ser. 190 012193
A S Mahmoud et al 2001 Supercond. Sci. Technol. 14 311
The LHCb Collaboration et al 2008 JINST 3 S08005
John A Dykema and James G Anderson 2006 Metrologia 43 287