no code implementations • 9 Feb 2021 • Fiorenzo Vincenzo, Todd A. Thompson, David H. Weinberg, Emily J. Griffith, James W. Johnson, Jennifer A. Johnson
We test the hypothesis that the observed first-peak (Sr, Y, Zr) and second-peak (Ba) s-process elemental abundances in low-metallicity Milky Way stars, and the abundances of the elements Mo and Ru, can be explained by a pervasive r-process contribution originating in neutrino-driven winds from highly-magnetic and rapidly rotating proto-neutron stars (proto-NSs).
Astrophysics of Galaxies High Energy Astrophysical Phenomena Solar and Stellar Astrophysics
