The variations in extinction and microphysical properties in the upper haze of Venus have a significant impact on the chemistry and radiative balance of its atmosphere. In order to study their spatial and temporal distribution， we analyzed solar occultation data from the Venus Express SPICAV SOIR instruments between 2006 and 2013. To remove the absorption effects of the middle and upper atmosphere of Venus， we used MODTRAN modeling. Then， we retrieved the extinction profiles of the upper haze between 67-92 km using the onion-peeling method. Our findings are as follows： 1） The extinction coefficient of the upper haze generally decreases with increasing altitude， but there are significant variations between different regions. In low latitudes， the extinction increased sharply early in the mission， and the average extinction coefficient of the haze showed minimal changes between day and night. The vertical optical depth of the haze layer was approximately 10^-2. 2） The number density of the upper haze decreases with increasing altitude. From the south to the north pole， the number density first increases and then decreases. 3） The cloud top altitude is higher in low-latitude regions at 82.7 ± 5.8 km， while in polar regions， it is lower with the northern polar region at 73.3 ± 2.4 km and the southern polar region at 79.5 ± 3.5 km. The average scale height of the upper haze layer in the northern polar region is 4.0 ± 0.9 km.