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

Many globular clusters (GCs) are known to host multiple populationsdistinguishable by their light-element content. Less common are GCs displayingiron abundance spreads which are seen as evidence for enrichment through corecollapse supernovae (SNe). We present a simple analytical method to estimatethe number of SNe required to have occurred in a GC from its metallicity andiron abundance spread. We then use this result to estimate how long starformation (SF) lasted to build the GC. We apply our method to up-to-datemeasurements and find that, assuming the correctness of these measurements,multiple SNe (up to $10^5$) are required in most GCs with iron abundancespreads. The number of SNe events which contributed to the enrichment of theGCs studied here is typically a factor of 10 less than the expected number ofSNe in a canonical initial mass function (IMF). This indicates that gasexpulsion from the forming GC occurred after the first 10 per cent of SNeexploded. We compute that for the GCs typically SF ends after only a few Myr(extending up to $\approx 30 ~\rm Myr$ in a few cases). We also discusspossible improvements of this method and especially its sensitivity to theerror of iron abundance measurements of individual stars of a GC. The methodpresented here can quickly give an estimate for the number of SNe required toexplain the iron abundance spread in a GC without the requirement of anyhydrodynamical simulations.

How many explosions does one need? -- Quantifying supernovae in globular clusters from iron abundance spreads