## 2. Potential magnetic field configurationsThe coronal magnetic field structure is treated in Cartesian
coordinates with the Potential magnetic fields are characterised by and, in what follows, we shall assume
, i.e. we consider a
This is just a particular case of the more general force-free solution and the expression for can be obtained from the Grad-Shafranov equation with , To determine the flux function in the corona
() one must integrate this partial
differential equation, imposing some boundary conditions. We prescribe
the value of the flux function at the photospheric level,
, and assume that © European Southern Observatory (ESO) 1999 Online publication: November 3, 1999 |