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Stellar collisions in globular clusters: Constraints on the initial mass function of the first generation of starsстатья
Статья опубликована в высокорейтинговом журнале
Статья опубликована в журнале из списка Web of Science и/или Scopus- Авторы: Dib S., Kravtsov V.V., Haghi H., Zonoozi A.H., Belinchon J.A.
- Журнал: Astronomy and Astrophysics
- Том: 664
- Год издания: 2022
- Издательство: Springer Verlag
- Местоположение издательства: Germany
- Первая страница: 1
- Последняя страница: 6
- Номер статьи: A145
- DOI: 10.1051/0004-6361/202243556
- Аннотация: Globular clusters display an anticorrelation between the fraction of the first generation of stars (N(G1)/N(tot)) and the slope of thepresent-day mass function of the clusters (α_pd), which is particularly significant for massive clusters. In the framework of the binarymediated collision scenario for the formation of the second-generation stars in globular clusters, we test the effect of a varying stellarinitial mass function (IMF) of the G1 stars on the (N(G1)/N(tot)) − α_pd anticorrelation. We use a simple collision model that has onlytwo input parameters, the shape of the IMF of G1 stars and the fraction of G1 stars that coalesce to form second-generation stars.We show that a variable efficiency of the collision process is necessary in order to explain the (N(G1)/N(tot)) − α_pd anticorrelation;however, the scatter in the anticorrelation can only be explained by variations in the IMF, and in particular by variations in the slopein the mass interval ≈ (0.1-0.5) M⊙. Our results indicate that in order to explain the scatter in the (N(G1)/N(tot)) − α_pd relation, itis necessary to invoke variations in the slope in this mass range between ≈ −0.9 and ≈ −1.9. Interpreted in terms of a Kroupa-likebroken power law, this translates into variations in the mean mass of between ≈ 0.2 and 0.55 M⊙. This level of variation is consistentwith what is observed for young stellar clusters in the Milky Way and may reflect variations in the physical conditions of the globularcluster progenitor clouds at the time the G1 population formed or may indicate the occurrence of collisions between protostellarembryos before stars settle on the main sequence.
- Добавил в систему: Кравцов Валерий Витальевич