The origin of discrete multiple stellar populations in globular clusters

Result code in IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F17%3A10371942" target="_blank" >RIV/00216208:11320/17:10371942 - isvavai.cz</a>

Result on the web

<a href="http://dx.doi.org/10.1093/mnras/stx1609" target="_blank" >http://dx.doi.org/10.1093/mnras/stx1609</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1093/mnras/stx1609" target="_blank" >10.1093/mnras/stx1609</a>

Result language

angličtina

Original language name

The origin of discrete multiple stellar populations in globular clusters

Original language description

Recent observations have revealed that at least several old globular clusters (GCs) in the Galaxy have discrete distributions of stars along the Mg-Al anticorrelation. In order to discuss this recent observation, we construct a new one-zone GC formation model in which the maximum stellar mass (m(max)) in the initial mass function of stars in a forming GC depends on the star formation rate, as deduced from independent observations. We investigate the star formation histories of formingGCs. The principal results are as follows. About 30 Myr after the formation of the first generation (1G) of stars within a particular GC, new stars can be formed from ejecta from asymptotic giant branch (AGB) stars of 1G. However, the formation of this second generation (2G) of stars can last only for [10-20] Myr because the most massive SNe of 2G expel all of the remaining gas. The third generation (3G) of stars are then formed from AGB ejecta approximate to 30 Myr after the truncation of 2G star formation. This cycle of star formation followed by its truncation by SNe can continue until all AGB ejecta is removed from the GC by some physical process. Thus, it is inevitable that GCs have discretemultiple stellar populations in the [Mg/Fe]-[Al/Fe] diagram. Our model predicts that low-mass GCs are unlikely to have discrete multiple stellar populations, and young massive clusters may not have massive OB stars owing to low m(max) (&lt;[20-30] M circle dot) during the secondary star formation.

Czech name

—

Czech description

—

Type

J_imp - Article in a specialist periodical, which is included in the Web of Science database

CEP classification

—

OECD FORD branch

10308 - Astronomy (including astrophysics,space science)

Project

—

Continuities

S - Specificky vyzkum na vysokych skolach

Publication year

2017

Confidentiality

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Name of the periodical

Monthly Notices of the Royal Astronomical Society

ISSN

0035-8711

e-ISSN

—

Volume of the periodical

471

Issue of the periodical within the volume

2

Country of publishing house

GB - UNITED KINGDOM

Number of pages

12

Pages from-to

2242-2253

UT code for WoS article

000409022700067

EID of the result in the Scopus database

—