Astrophysics with Radioactive Isotopes 2026, Traverse City, MI, USA

Session

Afternoon II

26 May 2026, 16:00

The Hagerty Center, Traverse City, Michigan, USA

27. When Stars Attack! Astrophysical Implications of Live 60Fe and 244Pu in Terrestrial and Lunar Archives

Brian Fields (University of Illinois)

26/05/2026, 16:00

Invited talk (30min + 10min Q&A)

Recent nearby stellar explosions can deliver their ejecta to the Earth and Moon, leaving a telltale signature in the form of live (not decayed) radioisotopes in the geological record. Remarkably, there is now a wealth of evidence that this has occurred: live ${}^{60}{\rm Fe}$ is found globally and in lunar regolith samples, and recently ${}^{244}{\rm Pu}$ is also detected. These point to...

33. Single Degenerate Double Detonation Type Ia Supernova from Quiescent Helium Accretion

Dr Amir Michaelis (Technion – Israel Institute of Technology)

27/05/2026, 16:00

Contributed talk (15min + 5min Q&A)

We investigate a sub-Chandrasekhar mass double detonation pathway for Type Ia supernovae arising from single degenerate helium accreting carbon-oxygen white dwarfs. Using one-dimension recurrent nova evolution code we evolve a 0.7 solar mass white dwarf through steady accretion at 10^-8 solar mass per year until it reaches 1.1 solar mass, yielding realistic, time evolved helium rich profiles....

23. Lifetime Measurements of 23Mg Excited State Significant in Nova Nucleosynthesis of 22Na

Lexanne Weghorn

27/05/2026, 16:20

Contributed talk (15min + 5min Q&A)

The 1275-keV gamma-ray line from decay of the radionuclide $^{22}$Na (${t _ {1/2}}$ = 2.6 y) is a prominent candidate for detection by space-based gamma ray telescopes, including the COSI mission scheduled to launch in 2027. Accurate models of the production and destruction of $^{22}$Na during novae are sought in order to determine the sensitivity required by observational missions as well as...

32. Implications of a weakening N = 126 shell closure away from stability for r-process astrophysical conditions

Mengke Li (UC Berkeley)

28/05/2026, 15:40

Invited talk (30min + 10min Q&A)

The formation of the third 𝑟-process abundance peak near 𝐴 ∼ 195 is highly sensitive to both nuclear structure far from stability and the astrophysical conditions that produce the heaviest elements. In particular, the 𝑁 = 126 shell closure plays a crucial role in shaping this peak. Experimental data hints that the shell weakens as proton number departs from 𝑍 = 82, a trend largely missed by...