English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

An overview of the sources for heavy elements in the early Galaxy is given.It is shown that observations of abundances in metal-poor stars can be usedalong with a basic understanding of stellar models to guide the search for thesource of the heavy r-process nuclei (r-nuclei). Observations show that thissource produces very little of the elements from C through Zn including Fe.This strongly suggests that O-Ne-Mg core-collapse supernovae (SNe) fromprogenitors of ~8-11M_sun are the source for the heavy r-nuclei. It is shownthat a two-component model based on the abundances of Fe (from Fe core-collapseSNe) and Eu (from O-Ne-Mg core-collapse SNe) gives very good quantitativepredictions for the abundances of all the other elements in metal-poor stars.

Chemical Evolution of Heavy Elements in the Early Galaxy: Implications for Stellar Sources