JINA - Segue Virtual Journal,
27 June 2025
Volume 20, Issue 18 (18 Articles)
- # 2 - Current Galactic Chemical Evolution models fail to explain rising Na-abundances of young thick disc stars
- E. K. Owusu (School of Science, University of New South Wales Canberra, Australia Defence Force Academy, Australia, ARC Centre of Excellence for All-Sky Astrophysics in 3 Dimensions, Max-Planck-Institut f"ur Astronomie, Heidelberg, Germany, Heidelberger Institut f"ur Theoretische Studien, Heidelberg, Germany), A. J. Ruiter (School of Science, University of New South Wales Canberra, Australia Defence Force Academy, Australia, ARC Centre of Excellence for All-Sky Astrophysics in 3 Dimensions, Max-Planck-Institut f"ur Astronomie, Heidelberg, Germany, Heidelberger Institut f"ur Theoretische Studien, Heidelberg, Germany, OzGrav: The ARC Centre of Excellence for Gravitational Wave Discovery, Hawthorn, Australia), A. J. Kemp (Institute of Astronomy), S. Buder (ARC Centre of Excellence for All-Sky Astrophysics in 3 Dimensions, Research School of Astronomy, Astrophysics, Australian National University, Australia), I. R. Seitenzahl (Heidelberger Institut f"ur Theoretische Studien, Heidelberg, Germany), N. Rodriguez-Segovia (School of Science, University of New South Wales Canberra, Australia Defence Force Academy, Australia), R. Pakmor (Max Planck Institute for Astrophysics, Garching, Germany), G. C. Cinquegrana (ARC Centre of Excellence for All-Sky Astrophysics in 3 Dimensions, School of Physics, Astronomy, Monash University, Clayton, Australia), N. Storm (Max-Planck-Institut f"ur Astronomie, Heidelberg, Germany, Heidelberg University, Heidelberg, Germany), P. Eitner (Max-Planck-Institut f"ur Astronomie, Heidelberg, Germany, Heidelberg University, Heidelberg, Germany), M. Bergemann (Max-Planck-Institut f"ur Astronomie, Heidelberg, Germany)
- https://arxiv.org/abs/2506.17711
This material is based upon work supported in part by the U.S. Department of Energy, Office of Science, Office of Nuclear Physics, under Award Number DE-SC0026204.
