  Recent determinations of the internal composition and structure of two
helium-atmosphere variable white dwarf stars, GD 358 and CBS 114, have led to
conflicting implied rates for the ^{12}C(alpha,gamma)^{16}O reaction. If we
assume that both stars were formed through single-star evolution, then the
initial analyses of their pulsation frequencies must have differed in some
systematic way. I present improved fits to the two sets of pulsation data,
helping to resolve the tension between the initial results.
