Based on auroral observations of a multi channels scanning photometer at Zhongshan Station, Antarctica and solar wind parameters data obtained by WIND Satellite at the upstream of the bow shock in 1997 and 1998, the dependence of the high latitude postnoon auroral intensity upon the solar wind parameters are studied quantitatively. It is shown that the 630 0nm intensity depends on the solar wind parameters more directly than the 557 7nm does. The 630 0nm intensity increases as the solar wind plasma density, dynamic pressure and speed increasing, with a correlation coefficient of 0 84, 0 88 and 0 61 respectively. While the dependence of 557 7nm intensity upon the solar wind parameters are not so clear. The difference between the dependences of 630 0nm and 557 7nm intensities upon the solar wind parameters indicates that the 630 0nm emission is influenced by solar wind more directly than the 557 7nm is, while the 557 7nm emission is related to magnetospheric dynamic processes sometimes.