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 Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

Metal enrichment by the first-generation (Pop III) stars is the very firststep of the matter cycle in the structure formation and it is followed by theformation of extremely metal-poor (EMP) stars. To investigate the enrichmentprocess by the Pop III stars, we carry out a series of numerical simulationsincluding the feedback effects of photoionization and supernovae (SNe) of PopIII stars with a range of masses of minihaloes (MHs), M_halo , and Pop IIIstars, M_PopIII . We find that the metal-rich ejecta reaches neighbouringhaloes and external enrichment (EE) occurs when the halo binding energy issufficiently below the SN explosion energy, E_SN . The neighbouring haloes areonly superficially enriched, and the metallicity of the clouds is [Fe/H] < -5.Otherwise, the SN ejecta falls back and recollapses to form enriched cloud,i.e. internal enrichment (IE) process takes place. In case that a Pop III starexplodes as a core-collapse SNe (CCSNe), MHs undergo IE, and the metallicity inthe recollapsing region is -5 < [Fe/H] < -3 in most cases. We conclude that IEfrom a single CCSN can explain the formation of EMP stars. For pair-instabilitySNe (PISNe), EE takes place for all relevant mass range of MHs, consistent withno observational sign of PISNe among EMP stars.

Metal-poor star formation triggered by the feedback effects from Pop III stars