Recent observational advances have enabled high resolution mapping of $^{44}$Ti in core-collapse supernova (CCSN) remnants. Comparisons between observations and 3D models provide stringent constraints on the CCSN mechanism. However, recent work has identified several uncertain nuclear reaction rates that influence $^{44}$Ti and $^{56}$Ni production in model calculations. We use MESA (Modules...
The $^{15}$O($\alpha$,$\gamma$)$^{19}$Ne reaction is one of the two breakout reactions from the hot CNO cycle into the rp process, and is crucial to the thermonuclear runaway that causes type I X-ray bursts on accreting neutron stars [1]. In order to determine the branching ratio the resonance partial width of the entrance and exit channels of the reaction are needed. While $\Gamma_{\gamma}$...
The CNO cycle is the dominant energy source for large main sequence stars and significantly contributes to the hydrogen burning in asymptotic giant branch stars. Of the reactions in the CNO cycle, the $^{14}$N(p,$\gamma$)$^{15}$O reaction is the slowest and therefore it regulates the energy production, lifetime, and abundance distribution of a given star. Measurements of this cross section...
Using a radio-frequency quadrupole ion trap to confine radioactive ions allows indirect measurements of beta-delayed neutron (BDN) emission. By determining the recoil energy of an ion it is possible to determine the source of the recoil, as neutron emission can impart significantly more energy than is imparted by beta decay alone. This method avoids most of the systematic errors associated...
