the best fit model derived in this study providedthe best agreement between Ti I and Ti II abundances indicating abetter choice of log g ， of the three sets of stellaratmosphere models， Comparing the best fit model of this study with Brown Wallerstein 1992，similar comments can be made. In general the light elementalabundances agree within 1​σ1\sigma. Sc II and Zn I are also enhancedusing this model compared to Brown Wallerstein 1992， at least in terms of Ti. ，。

while Ti II is stillsignificantly depleted. However。