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International Symposium on Nuclei in the Cosmos XVIII (NIC XVIII)

15–20 Jun 2025
Girona
Europe/Brussels timezone

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Session

Stellar Evolution I – Hydrostatic Evolution, AGBs, Massive Stars, S-Process

17 Jun 2025, 12:00
Girona

Girona

Palau de Congressos de Girona Pg. de la Devesa, 35 17001 Girona

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  1. 341. Nucleosynthesis in Low- and Intermediate-Mass Stars
    A Choplin
    17/06/2025, 12:00
    Invited Review Talk
  2. 310. FLASH Session IV
    17/06/2025, 12:30
  3. 158. Nucleosynthesis and wind yields of Very Massive Stars
    Erin Higgins (Queen's University Belfast)
    17/06/2025, 14:15
    Invited Review Talk

    The most massive stars provide an essential source of recycled material for young clusters and galaxies. While very massive stars (VMS, M > 100M$_{\odot}$) are relatively rare compared to O stars, they lose disproportionately large amounts of mass already from the onset of core H-burning. In this talk, I will discuss the impact of stellar wind yields from VMS, calculated for a wide range of...

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  4. 25. The Role of Carbon-Oxygen Shell Interactions in the Nucleosynthesis and Final Fate of Massive Stars
    Lorenzo Roberti (Laboratori Nazionali del Sud)
    17/06/2025, 14:45
    Contributed Talk

    Carbon-oxygen (C-O) shell interactions in the late evolutionary stages of massive stars play a crucial role in determining their final fate and have a significant impact on the pre-supernova and explosive nucleosynthesis. In this talk, I will explore the complex dynamics within C-O shells, and how these interactions drive the production of intermediate and heavy elements. In particular I will...

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  5. 169. Comparing the Elemental Yields from Low-Mass Single and Binary Star Populations
    Zara Osborn (Monash University)
    17/06/2025, 15:00
    Contributed Talk

    Asymptotic giant branch (AGB) stars are evolved stars born with a low mass of about 1-8M⊙, depending on their metallicity. These stars are vital to the chemical enrichment of the universe as they synthesise and eject significant amounts of carbon, nitrogen, fluorine, and about half of the material heavier than iron through the slow neutron capture process. However, one aspect often overlooked...

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  6. 202. Common Envelope Nucleosynthesis: investigation into how nucleosynthesis can vary across different neutron star common envelope binaries
    Alexander Hall-Smith (the University of York)
    17/06/2025, 15:15
    Contributed Talk

    In 2017 the first neutron star merger was observed at LIGO, and for a neutron star binary system to merge within a hubble time the progenitor system must undergo a common envelope phase to dissipate the orbital energy and bring the two compact masses closer together [1]. During the common envelope phase the compact neutron star orbits within the envelope of the companion star and accretes...

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  7. 342. FLASH Session V
    17/06/2025, 15:30
  8. 94. Isomeric State of 176Lu^m and Robustness of A Stellar Thermometer 176Lu/176Hf for the Main s-Process in AGB Stars
    Contributed Talk

    Both 176Lu (t1/2 ∼36 Gyr) and 176Hf are the so-called “s-only nuclei” which are produced literally only by the main component of the slow neutron-capture process (main s-process) in AGB stars. The nucleosynthesis of the isomeric state 176Lu^m (t1/2 ∼3 h) predominates the 176Lu/176Hf ratio because the system does not reach the thermal equilibrium at the temperature of the main s-process. We...

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