The origin of discrete multiple stellar populations in globular clusters

K. Bekki, T. Jerabkova, P. Kroupa

Research output: Contribution to journalArticle

Abstract

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) (

LanguageEnglish
Pages2242-2253
Number of pages12
JournalMonthly Notices of the Royal Astronomical Society
Volume471
Issue number2
DOIs
StatePublished - Oct 2017

Cite this

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title = "The origin of discrete multiple stellar populations in globular clusters",
abstract = "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) (",
keywords = "stars: formation, globular clusters: general, galaxies: star clusters: general, INITIAL MASS FUNCTION, ASYMPTOTIC GIANT BRANCH, SELF-ENRICHMENT SCENARIO, DOUBLE MAIN-SEQUENCE, UV LEGACY SURVEY, STAR-CLUSTERS, ABUNDANCE PATTERNS, EVOLUTION, MODEL, POLLUTION",
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year = "2017",
month = "10",
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language = "English",
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journal = "Monthly Notices of the Royal Astronomical Society",
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The origin of discrete multiple stellar populations in globular clusters. / Bekki, K.; Jerabkova, T.; Kroupa, P.

In: Monthly Notices of the Royal Astronomical Society, Vol. 471, No. 2, 10.2017, p. 2242-2253.

Research output: Contribution to journalArticle

TY - JOUR

T1 - The origin of discrete multiple stellar populations in globular clusters

AU - Bekki,K.

AU - Jerabkova,T.

AU - Kroupa,P.

PY - 2017/10

Y1 - 2017/10

N2 - 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) (

AB - 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) (

KW - stars: formation

KW - globular clusters: general

KW - galaxies: star clusters: general

KW - INITIAL MASS FUNCTION

KW - ASYMPTOTIC GIANT BRANCH

KW - SELF-ENRICHMENT SCENARIO

KW - DOUBLE MAIN-SEQUENCE

KW - UV LEGACY SURVEY

KW - STAR-CLUSTERS

KW - ABUNDANCE PATTERNS

KW - EVOLUTION

KW - MODEL

KW - POLLUTION

U2 - 10.1093/mnras/stx1609

DO - 10.1093/mnras/stx1609

M3 - Article

VL - 471

SP - 2242

EP - 2253

JO - Monthly Notices of the Royal Astronomical Society

T2 - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

SN - 0035-8711

IS - 2

ER -