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

The differences in the relationships between the physical parameters and thechemical-element abundances in accreted globular star clusters and those formedinside the Galaxy have been investigated. The information on the supposedformation sites of the clusters based on the Gaia~DR2 data is borrowed from theliterature. Those sources estimate the probability of belonging to the Galacticbulge and disk, as well as to six known events of the merger of dwarf satellitegalaxies with the Milky Way, for 151~globular clusters. It is shown that allmetal-poor ($\rm{[Fe/H]}<-1.0$) genetically related globular clusters have highrelative abundances of $\alpha$-elements. According to modern views, since typeII supernovae release more $\alpha$-elements into the interstellar medium withincreasing mass, it has been suggested that masses of type II supernovae in theGalaxy were greater than in the accreted galaxies. It is proved that theclusters of the low-energy group, which were considered accreted, aregenetically related to a single protogalactic cloud, same as the unstratifiedclusters UKS~1 and Liller~1, which most likely belong to the bulge. It is shownthat not only the lower but also the upper limits of the clusters' massesdecrease with an increase in the average radius of their orbits. The latterfact is explained by a decrease in the masses of emerging clusters with adecrease in the masses of their host galaxies. It is demonstrated that anextremely multicomponent stellar population is observed only in accretedglobular clusters with an initial mass $>10^{6}M_{\odot}$. It has beensuggested that these clusters retained all the matter ejected by their evolvedstars, from which new generations of stars formed due to long evolution farfrom our Galaxy.

Physical and Chemical Properties of Galactic Global Clusters with Various Origins Identified from the Gaia DR2 Data