29 November 2023 to 3 December 2023
Africa/Johannesburg timezone
The Welcome Function for ANPC 2023 will be on Tuesday 28 November 2023 at 18h30

39Ca and its relevance in nuclear astrophysics

1 Dec 2023, 15:05
15m
Oral Nuclear Astrophysics Session 9

Speaker

Sifundo Binda (iThemba LABS and Wits University)

Description

Elemental abundances are excellent probes of classical novae (CN). Sensitivity studies show that $^{38}$K($p$,$\gamma$)$^{39}$Ca reaction-rate uncertainties modify the abundance of calcium by a factor of 60 in CN ejecta. Existing direct [1,2] and indirect measurements [3,4] are in contradiction concerning the energies and strengths of important resonances in the $^{38}$K($p$,$\gamma$)$^{39}$Ca reaction. Direct measurements of the lowest three known $\ell$ = 0 resonances at $E_\mathrm{r}$ = 386, 515, and 679 keV have greatly reduced the uncertainties on the reaction rate for this reaction [1,2]. However, considerable uncertainty remains in the spectroscopy of $^{39}$Ca and subsequently, in the $^{38}$K($p$,$\gamma$)$^{39}$Ca reaction rate. A subsequent $^{40}$Ca($^{3}$He,$^4$He)$^{39}$Ca experiment using the SplitPole at TUNL [3] concluded that one of the resonances ($E_\mathrm{r}$ = 701.3 or $E_\mathrm{r}$ = 679 keV depending on the source of the nuclear data) may have been misplaced in the DRAGON target during the direct measurement and that tentative new states at $E_\mathrm{x}$ = 5908, 6001, and 6083 keV ($E_\mathrm{r}$ = 137, 230, and 312 keV) could correspond to important resonances in $^{38}$K($p$,$\gamma$)$^{39}$Ca. Resonance energies have an exponential effect on the reaction rate and the possible new resonances induce a 40\% uncertainty in the $^{38}$K($p$,$\gamma$)$^{39}$Ca reaction rate [3]. To resolve these, $^{39}$Ca was studied using the $^{40}$Ca($p,d$)$^{39}$Ca reaction at forward angles with a proton beam energy of 66 MeV using the K600 magnetic spectrometer. These measurements are aimed at verifying the properties of levels in the region where discrepancies between various experiments persist. Preliminary results from the measurements will be presented.

[1] Lotay et al. PRL 116,132701 (2016)
[2] Christian et al. PRC 97 025802 (2018)
[3] Setoodehnia et al. PRC 98 055804 (2018)
[4] Hall et al. PRC 101, 015804 (2020)

This work is based on the research supported by the National Research Foundation (NRF) doctoral postgraduate scholarship (UID 141287) and the Southern African Institute for Nuclear Technology and Sciences (SAINTS) Prestigious Doctoral Scholarship.

Attendance Type In-person

Primary author

Sifundo Binda (iThemba LABS and Wits University)

Co-authors

Dr Phillip Adsley (Department of Physics and Astronomy, Texas AM University, Texas, USA.) Dr Lindsay Donaldson (iThemba Laboratory for Accelerator Based Sciences) Dr Luna Pellegri (University of the Witwatersrand and iThemba LABS) Dr Armand Bahini (iThemba LABS) Mr Jacob Bekker (University of the Witwatersrand) Dr Johann Brummer (iThemba LABS) Ms Thuthukile Khumalo (Wits University and iThemba LABS) Dr Kgashane Malatji (iThemba LABS) Refilwe Emil Molaeng (University of the Witwatersrand and iThemba LABS) Dr Retief Neveling (iThemba LABS)

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