Probing astrophysically important states in $^{26}$Mg nucleus to study neutron sources for the $s$-Process

Understand

The $^{22}$Ne($\alpha$,n)$^{25}$Mg reaction is the dominant neutron source for the slow neutron capture process ($s$-process) in massive stars and contributes, together with the $^{13}$C($\alpha$,n)$^{16}$O, to the production of neutrons for the $s$-process in Asymptotic Giant Branch (AGB) stars.

• However, the reaction is endothermic and competes directly with the $^{22}$Ne($\alpha,\gamma)^{26}$Mg radiative capture.
• The uncertainties for both reactions are large owing to the uncertainty in the level structure of $^{26}$Mg near the alpha and neutron separation energies.
• These uncertainties are affecting the s-process nucleosynthesis calculations in theoretical stellar models.