BRIDGCE-IReNA AM 2023

Session

Stars and Yields

13 Sept 2023, 09:00

CSEC Board Room (CSEC, James Clerk Maxwell Building, Edinburgh (UK))

Conveners

Stars and Yields

• Claudia Lederer-Woods (University of Edinburgh)

66. Indirect Neutron-Capture Constraints for the Astrophysical i-Process

Andrea Richard (Lawrence Livermore National Laboratory)

13/09/2023, 09:00

Neutron-capture nucleosynthesis occurs via a variety of processes depending on the astrophysical sites and conditions. Recent observations and stellar evolution models of carbonenhanced metal poor stars (CEMP) and Rapidly Accreting White Dwarf stars (RAWDs) suggest that an intermediate process, known as the i-process, exists between the traditional s- and r-processes, and is necessary to...

25. The impact of binary stars on the dust and metal evolution of galaxies

Dr Rob Yates (University of Hertfordshire)

13/09/2023, 09:45

At the BRIDGCE meeting last year, I presented the technical implementation of the binary stellar evolution (BSE) code, BINARY_C, into the cosmological-scale galaxy evolution simulation, L-GALAXIES. This implementation is now fully complete, providing us with a set of comprehensive final results describing the impact of binary stars on the dust and metal evolution of galaxies (Yates et al.,...

9. Close Hierarchical Triples and Tertiary Tides

Yan Gao

13/09/2023, 10:05

In recent years, close hierarchical triples have been shown to be increasingly important when it comes to understanding many astrophysical phenomena, including but not limited to SNe Ia and BBHs. However, our understanding of them is yet incomplete. This talk will focus on a recently-discovered tidal process that is active in these systems, and its implications on stellar evolution will be discussed.

20. Stellar Wind Yields of Very Massive Stars

Erin Higgins (Armagh Observatory & Planetarium)

13/09/2023, 10:25

The most massive stars provide an essential source of recycled material for young clusters and galaxies. While very massive stars (VMS, M>100 M⊙) are relatively rare compared to O stars, they lose disproportionately large amounts of mass already from the onset of core H-burning. VMS have optically thick winds with elevated mass-loss rates in comparison to optically thin standard O-star winds....