2011/06/01 by Enrico Vesperini, Stephen L. W. McMillan, F. D’Antona +3 · 3 citations
Physics and Astronomy · #Astronomy #Astronomy and Astrophysical Research #Astrophysics #Astrophysics and Star Formation Studies #Binary number #Binary star #Blue straggler #Cluster (spacecraft) #Ejecta #Globular cluster #Physics #Population #Star cluster #Star formation #Stars #Stellar, planetary, and galactic studies #Supernova #astro-ph.GA
paper · pdf · doi:10.1111/j.1365-2966.2011.19046.x
6 pages, 6 figures. Accepted for publication in MNRAS
openalex publication_date 2011/06/01 · arxiv created 2011/06/03 · arxiv updated 2015/05/28 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
The discovery of multiple stellar populations in globular clusters raises fundamental questions concerning the formation and dynamical history of these systems. In a previous study aimed at exploring the formation of second-generation (SG) stars from the ejecta of first-generation (FG) asymptotic giant branch stars, and the subsequent dynamical evolution of the cluster, we showed that SG stars are expected to form in a dense subsystem concentrated in the inner regions of the FG cluster. In this paper we explore the implications of the structural properties of multiple-population clusters, and in particular the presence of the inner SG subsystem, for the disruption of binary stars. We quantify the enhancement of the binary disruption rate due to the presence of the central SG subsystem for a number of different initial conditions. Our calculations show that SG binaries, which are assumed to be more concentrated in the cluster inner regions, are disrupted at a substantially larger rate than FG binaries. Assuming a similar initial fraction of FG and SG binaries, our dynamical study indicates that the SG population is now expected to contain a significantly smaller binary fraction than the FG population.