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

We used a one-zone chemical evolution model to address the question of howmany masses and metallicities are required in grids of massive stellar modelsin order to ensure reliable galactic chemical evolution predictions. We used aset of yields that includes seven masses between 13 and 30 Msun, 15metallicities between 0 and 0.03 in mass fraction, and two different remnantmass prescriptions. We ran several simulations where we sampled subsets ofstellar models to explore the impact of different grid resolutions. Stellaryields from low- and intermediate-mass stars and from Type Ia supernovae havebeen included in our simulations, but with a fixed grid resolution. We comparedour results with the stellar abundances observed in the Milky Way for O, Na,Mg, Si, Ca, Ti, and Mn. Our results suggest that the range of metallicityconsidered is more important than the number of metallicities within thatrange, which only affects our numerical predictions by about 0.1 dex. We foundthat our predictions at [Fe/H] < -2 are very sensitive to the metallicity rangeand the mass sampling used for the lowest metallicity included in the set ofyields. Variations between results can be as high as 0.8 dex, for any remnantmass prescription. At higher [Fe/H], we found that the required number ofmasses depends on the element of interest and on the remnant mass prescription.With a monotonic remnant mass prescription where every model explodes as acore-collapse supernova, the mass resolution induces variations of 0.2 dex onaverage. But with a remnant mass prescription that includes islands ofnon-explodability, the mass resolution can cause variations of about 0.2 to 0.7dex depending on the choice of metallicity range. With such a prescription,explosive or non-explosive models can be missed if not enough masses areselected, resulting in over- or under-estimations of the mass ejected bymassive stars.

Mass and Metallicity Requirement in Stellar Models for Galactic Chemical Evolution Applications