Updated reaction rate of Mg25(p,γ)Al26 and its astrophysical implication

$^{26}\mathrm{Al}$ with a half-life of $7.17\ifmmode\times\else\texttimes\fi{}{10}^{5}$ years is one of the most significant nuclides in $\ensuremath{\gamma}$-ray astronomy and presolar grains of meteorites. Its main production mechanism in the $\mathrm{H}$-burning MgAl cycle is the $^{25}\mathrm{Mg}(p,\ensuremath{\gamma})^{26}\mathrm{Al}$ reaction. In the temperature region of 0.05--0.3 GK of astrophysical interest, the astrophysical $^{25}\mathrm{Mg}(p,\ensuremath{\gamma})^{26}\mathrm{Al}$ reaction rate is dominated by the resonant capture of several low-energy resonances. In this work, we report the results of a complete experimental investigation of the ${E}_{\mathrm{c}.\mathrm{m}.}=92$, 130, and 189 keV resonances in the $^{25}\mathrm{Mg}(p,\ensuremath{\gamma})^{26}\mathrm{Al}$ reaction with the Jinping Underground Nuclear Astrophysics Experimental Facility. The updated thermonuclear $^{25}\mathrm{Mg}(p,\ensuremath{\gamma})^{26}\mathrm{Al}$ reaction rate is (32--39)% higher than that obtained at the Laboratory for Underground Nuclear Astrophysics around 0.07--0.09 GK, mainly due to the 32% enhancement of the 92-keV resonance strength. The astrophysical impact of our new rate on the $^{26}\mathrm{Al}$ yield in a 5 ${\mathrm{M}}_{\ensuremath{\bigodot}}$ low-metallicity asymptotic giant branch star is investigated, in which an increase of (45--79)% in the $^{26}\mathrm{Al}$ yield is found by adopting our new $^{25}\mathrm{Mg}(p,\ensuremath{\gamma})^{26}\mathrm{Al}$ rates.