are about equal (ratio of $\sim 1$), compared to a ratio of $> 3$ near apastron. The results presented in Fig. \[fig:min\] suggest that the hard and soft X-ray components reside close to the secondary, and are not originated in the tail of the WCR. We also note that the observation point at phase $0.042$ is better fitted with a model that includes the conical shell (Fig. \[fig:NH\]) than with a spherical primary wind, also shown as the solid blue line in Fig. \[fig:min\]. This points is well after the X-ray minimum, and this is an expected result. The point at phase $-0.01$ can be marginally fitted if the WCR does exist, by changing somewhat the unknown parameters. However, it seems we can better fit it by assuming that the WCR is already highly disrupted at that time. Namely, the collapse of the WCR starts around $-0.01$ or somewhat earlier, as suggested by A06.

We note that the observed column density at phase $0.47$ of $N_H=17\times10^{22} \cm^{-2}$ (H07) occurred when the $2-10 \keV$ emission was $10-15 \%$ above its average value during that time (Corcoran 2005). This could result from a higher density of the primary wind. According to the 