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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{Fg091_feld_col.ps} \end{figure}$ Figure 1: Structure of a typical magnetic field perturbation generated by the Hall-drift induced instability from a toroidal crustal background field having a maximum field strength of about 10¹⁴ G. The growth time of the perturbation is of the order of $5~\times~ 10^4$ years. The neutron star model behind relies on the Pandharipande-Smith equation of state, its crustal thickness $d\sim 3800$ m. The vertical scale z is arbitrarily limited to z=d/10=386 m, where the magnetic field strength is reduced by a factor of about 3 compared with its surface value. The distance between adjacent spots in x-direction $\sim$ 1.1 km, in y-direction $\sim$ 3 km (see Fig. 2 for that dimension). Colour encoding corresponds to the normal field component, $<\cdot >_x$ denotes the average with respect to x. All magnetic field values are given in units of 10¹² G, z₄ is in units of 10⁴ cm.
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In the text

$\begin{figure} \par\includegraphics[width=9.2cm,clip]{Fg091_drauf_col.ps}\par \end{figure}$ Figure 2: The same magnetic field perturbation as in Fig. 1 but viewed from above and zoomed into a smaller x interval. Note, that this field has to be superimposed on the global dipolar field having its pole in the vicinity of one of the spot centers to get the actual open magnetic field lines.
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In the text

$\begin{figure} \par\includegraphics[width=9.2cm,clip]{Fg091_drauf_col.ps}\par \end{figure}$	Figure 2: The same magnetic field perturbation as in Fig. 1 but viewed from above and zoomed into a smaller x interval. Note, that this field has to be superimposed on the global dipolar field having its pole in the vicinity of one of the spot centers to get the actual open magnetic field lines.
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