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

A catalog compiling the parameters of 346 open clusters, including theirmetallicities, positions, ages, and velocities has been composed. The elementsof the Galactic orbits for 272 of the clusters have been calculated.Spectroscopic determinations of the relative abundances, [el/Fe], for 14elements synthesized in various nuclear processes averaged over data from 109publications are presented for 90 clusters. Since no systematic effectsdistorting the relative abundances of the studied elements in these clustershave been found, these difference suggest real differences between clusterswith high, elongated orbits and field stars. In particular, this supports theearlier conclusion, based on an analysis of the elements of the Galacticorbits, that some clusters formed as a result of interactions betweenhigh-velocity, metal-poor clouds and the interstellar medium of the Galacticthin disk. On average, clusterswith high, elongated orbits and metallicities${\rm [Fe/H]} < - 0.1$ display lower relative abundances of the primary \'aelements than do field stars. The low [O,Mg/Fe] ratios of these clusters can beunderstood if the high-velocity clouds that gave rise to them were formed ofinterstellar material from regions where the star-formation rate and/or themasses of Type II supernovae were lower than near the Galactic plane. It isalso shown that, on average, the relative abundances of the primary$\alpha$-elements are higher in relatively metal-rich clusters with high,elongated orbits than in field stars. This can be understood if clusters with${\rm [Fe/H]} > - 0.1$ formed as a result of interactions between metal-richclouds with intermediate velocities and the interstellar medium of the Galacticdisk; such clouds could form from returning gas in a so-called "Galacticfountain".

Peculiarities of {\alpha}-element abundances in Galactic open clusters