Core-collapse supernova γ-ray signatures

From the macrocosm to the microcosm: the CasA supernova remnant and a SiC-X presolar stardust grain differ in size by almost 23 orders of magnitude, yet nuclear reactions govern them both!

The science question

Which nuclear reactions control the radioactive isotopes that let us diagnose core-collapse supernovae?

Radioisotopes such as \(\mathrm{^{44}Ti}\), \(\mathrm{^{56}Ni}\), \(\mathrm{^{22}Na}\), \(\mathrm{^{43}K}\), \(\mathrm{^{47}Sc}\) and \(\mathrm{^{59}Fe}\) can connect the deep physics of an explosion to γ-ray observations, late-time light curves, and presolar grain signatures. The challenge is that the relevant reaction rates are often poorly constrained at stellar energies.

What we do

Identify reactions that control \(\gamma\)-ray emitting isotopes in supernova models.
Measure or constrain key reactions using radioactive-ion beams and indirect spectroscopy.
Connect laboratory rates to predicted \(\gamma\)-ray fluxes, light curves, and isotopic signatures in stardust.
Use supernova remnants and presolar grains as complementary tests of nucleosynthesis.

Part of the experimental setup we used to directly study the 13N(α,p)16O reaction using CRIB at RIKEN.

Student entry points

Analyze reaction data and detector simulations from radioactive-beam experiments.
Run sensitivity studies for radioactive isotope yields in supernova ejecta.
Compare model yields with gamma-ray observables and presolar grain constraints.
Build clear visual links between a nuclear reaction, a radioisotope, and an astronomical signature.

Selected output

M. Abubakar et al., Phys. Rev. C 113, L062802 (2026)
M. Pignatari et al., Astrophys. J. 990 (2025)
A. Psaltis, “Nuclear physics constraints on the γ-ray signatures of core-collapse supernovae”, IReNA Online Seminar (2026)