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

26–30 May 2026
The Hagerty Center, Traverse City, Michigan, USA
US/Eastern timezone

Session

Afternoon II

26 May 2026, 16:00
The Hagerty Center, Traverse City, Michigan, USA

The Hagerty Center, Traverse City, Michigan, USA

Conveners

Afternoon II

  • Daid Kahl (Facility for Rare Isotope Beams, Michigan State University)

Afternoon II

  • Thomas Stephan (University of Chicago)

Afternoon II

  • Chris Fryer (Los Alamos National Laboratory)

Presentation materials

There are no materials yet.

  1. 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...

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  2. 49. Availability of fast radioactive beams at FRIB for nuclear astrophysics
    Dr Daid Kahl (FRIB)
    27/05/2026, 16:00
    Invited talk (30min + 10min Q&A)

    Nuclear reactions frequently involve radioactive species as one or both components in explosive astrophysical scenarios, such as (super)novae, Type I X-ray bursts, and neutron star mergers.  The reaction rates involved in calculating the astronomical observables are frequently unknown or poorly constrained in the Gamow window, requiring both direct and indirect measurements with both stable...

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  3. 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...

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