  We examine the impact of the strength of the E_R = 127 keV, 26Al(p,g)27Si
resonance on 26Al production in classical nova explosions and asymptotic giant
branch (AGB) stars. Thermonuclear 26Al(p,g)27Si reaction rates are determined
using different assumed strengths for this resonance and representative stellar
model calculations of these astrophysical environments are performed using
these different rates. Predicted 26Al yields in our models are not sensitive to
differences in rates determined using zero and a commonly stated upper limit
corresponding to wg_UL = 0.0042 micro-eV for this resonance strength. Yields of
26Al decrease by 6% and, more significantly, up to 30%, when a strength of 24 x
wg_UL = 0.1 micro-eV is assumed in the adopted nova and AGB star models,
respectively. Given that the value of wg_UL was deduced from a single,
background-dominated 26Al(3He,d)27Si experiment where only upper limits on
differential cross sections were determined, we encourage new experiments to
confirm the strength of the 127 keV resonance.

Solar and Stellar Astrophysics