Astron. Astrophys. 364, 785792 (2000)
3. Numerical results
We have solved numerically Eq. (29) and Eq. (30) in two
dimensions with three field components using a fast Fourier transform
method. The problem with a periodic boundarycondition with respect to
y is considered. The initial conditions which is satisfied to
is chosen as
where is a period and
is the width of the electromagnetic
envelope. Evolution of the solution of Eq. (29) and Eq. (30)
with the initial condition (31) is given in Figs. 24. These
parameters are chosen as

Fig. 1. The distribution of initial electric field


Fig. 2. Collapse development of selfgenerated magnetic field when


Fig. 3. Collapse development of selfgenerated magnetic field when


Fig. 4. Collapse development of selfgenerated magnetic field when

The distribution of the initial electric field is shown in
Fig. 1. For coronal active regions, the numerical solution for
Eqs. (29) and (30) show that the magnetic field selfgenerated by
transverse plasmons with frequency
would collapse (see Figs. 24). The level contours of
at successive times are shown in
Figs. 24 for two dimensional geometry. In other words, due to
selfcompressing, a stronger magnetic field could be produced in a
small region.Quantities in Figs. 14 are dimensionless. For
coronal active regions, their relations to dimensional ones are(taking
)
© European Southern Observatory (ESO) 2000
Online publication: January 29, 2001
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