Twenty-seven new stellar envelope models have been constructed using the new Livermore opacities to see if the discrepancy between the masses of the double-mode RR Lyrae variables using pulsation and evolution theories can be reconciled. For these extreme Population II variables (Z = 0.0001 to 0.0004), the large opacity increases found from the extensive line absorptions of iron around 250,000 K seen in Population I compositions are not realized. If the Z is 0.001, period ratios decrease from the original Cox, Hodson, and Clancy values by more than 0.01, leading to double-mode masses more than 0.3 M. larger, but such a large Z is not reasonable for these stars. It is discovered that opacity decreases below a temperature of 10(5) K, due to more narrow lines of hydrogen than used in the Los Alamos opacities, can also decrease theoretical period ratios. This opacity decrease, as with the higher temperature increases, studied extensively before for other types of yellow giant variable stars, produces steeper temperature increases and more shallow density gradients in the regions where the pulsation eigenvectors can feel the stellar structure. This leads to longer periods for all modes, with the fundamental mode being increased in period the most. Thus it appears that period ratios should be smaller and theoretical double-mode masses about 0.1 M. larger than those using earlier opacities that were higher at lower temperatures and lower at higher temperatures. Small opacity increases at about 250,000 K can increase the more metal content RRd variables in the Oosterhoff I clusters by another 0.1 M.. This essentially eliminates the inconsistency between masses from the two globular cluster types and between those determined from pulsation and evolution theories.
