Speaker
Description
The radioactive nucleus $^{44}$Ti is thought to be produced in Core-Collapse Supernovae (CCSNe) with the amount produced being sensitive to internal dynamics of the explosion. As such, $^{44}$Ti is a potential diagnostic tool for understanding the behaviour of these stellar explosions.
The amount of $^{44}$Ti produced depends not only on the production reactions but also on the destruction reactions, most notably the $^{44}$Ti($\alpha,p$)$^{47}$V reaction which proceeds through states in the compound nucleus $^{48}$Cr. This reaction is usually treated through statistical models (see, for example, the recent study by Chipps and collaborators Phys. Rev. C 102, 035806) but it is not clear that this is valid given the limitations of the levels which can be populated in $^{44}$Ti$+\alpha$ fusion (natural parity, isoscalar) and the influence of $\alpha$-particle clustering behaviour on other $\alpha$-particle induced reactions.
Spectroscopy in the Gamow Window of the $^{44}$Ti($\alpha,p$)$^{47}$V reaction has been performed using the $^{50}$Cr($p,t$)$^{48}$Cr reaction with the K600 magnetic spectrometer at iThemba LABS in South Africa. A number of excited states have been observed, many for the first time, giving insights into the validity of statistical models for the $^{44}$Ti($\alpha,p$)$^{47}V reaction.
| Length of presentation requested | Oral presentation: 8 min + 2 min questions (Poster-type talk) |
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| Please select between one and three keywords related to your abstract | Nuclear physics - experimental |
