must be incorporated; one that extinguishes the conical shell. We take this process to be accretion onto the secondary star. For that, our calculation of $N_H$ with the WCR included is not applicable at all during the minimum, i.e., the phase period $\sim 0-0.035$. The flow structure around the secondary is more complicated, as it includes the accretion process, and possibly a polar outflow (jets) that results the extra soft source during the X-ray minimum (see section \[sec:ex\]). The column density during the minimum might be better represented by an undisturbed primary wind in the entire space. As we are not sure where the polar outflow is shocked and forms the X-ray emitting regions, we take 3 possibilities for its location: At the location of the secondary itself (which is the average of two opposite jets); a region above the primary (perpendicular to the equatorial plane) of $y_x=0.25r$, and of $y_x=0.5r$. In Fig. \[fig:min\] the column density to the X-ray emitting region in the cases is plotted during the X-ray minimum, and $20$ days (a phase of $0.01$) before and after the minimum.

We note that during the X-ray minimum the column densities toward the hard and soft X-ray sources 