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MOCCA: dynamics and evolution of single and binary stars of multiple stellar populations in tidally filling and underfilling globular star clusters

Hypki, Arkadiusz ; Giersz, Mirek ; Hong, Jongsuk ; Leveque, Agostino ; Askar, Abbas LU orcid ; Belloni, Diogo and Otulakowska-Hypka, Magdalena (2022) In Monthly Notices of the Royal Astronomical Society 517(4). p.4768-4787
Abstract

We present an upgraded version of the mocca code for the study of dynamical evolution of globular clusters (GCs) and its first application to the study of evolution of multiple stellar populations. We explore initial conditions spanning different structural parameters for the first (FG) and second generation of stars (SG) and we analyse their effect on the binary dynamics and survival. Here, we focus on the number ratio of FG and SG binaries, their spatial variation, and the way their abundances are affected by various cluster initial properties. We find that present-day SG stars are more abundant in clusters that were initially tidally filling. Conversely, FG stars stay more abundant in clusters that were initially tidally... (More)

We present an upgraded version of the mocca code for the study of dynamical evolution of globular clusters (GCs) and its first application to the study of evolution of multiple stellar populations. We explore initial conditions spanning different structural parameters for the first (FG) and second generation of stars (SG) and we analyse their effect on the binary dynamics and survival. Here, we focus on the number ratio of FG and SG binaries, their spatial variation, and the way their abundances are affected by various cluster initial properties. We find that present-day SG stars are more abundant in clusters that were initially tidally filling. Conversely, FG stars stay more abundant in clusters that were initially tidally underfilling. We find that the ratio between binary fractions is not affected by the way we calculate these fractions [e.g. only main-sequence binaries (MS) or observational binaries, i.e. MS stars >0.4 M⊙ mass ratios >0.5]. This implies that the MS stars themselves are a very good proxy for probing entire populations of FG and SG. We also discuss how it relates to the observations of Milky Way GCs. We show that mocca models are able to reproduce the observed range of SG fractions for Milky Way GCs for which we know these fractions. We show how the SG fractions depend on the initial conditions and provide some constraints for the initial conditions to have more numerous FG or SG stars at the Hubble time.

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author
; ; ; ; ; and
organization
publishing date
type
Contribution to journal
publication status
published
subject
keywords
galaxies: star clusters: general, methods: numerical, software: data analysis, stars: chemically peculiar
in
Monthly Notices of the Royal Astronomical Society
volume
517
issue
4
pages
20 pages
publisher
Oxford University Press
external identifiers
  • scopus:85145346646
ISSN
0035-8711
DOI
10.1093/mnras/stac2815
language
English
LU publication?
yes
id
69328428-ac52-4ee1-9c86-e4aa6673dae1
date added to LUP
2023-01-16 16:28:14
date last changed
2024-04-03 18:43:23
@article{69328428-ac52-4ee1-9c86-e4aa6673dae1,
  abstract     = {{<p>We present an upgraded version of the mocca code for the study of dynamical evolution of globular clusters (GCs) and its first application to the study of evolution of multiple stellar populations. We explore initial conditions spanning different structural parameters for the first (FG) and second generation of stars (SG) and we analyse their effect on the binary dynamics and survival. Here, we focus on the number ratio of FG and SG binaries, their spatial variation, and the way their abundances are affected by various cluster initial properties. We find that present-day SG stars are more abundant in clusters that were initially tidally filling. Conversely, FG stars stay more abundant in clusters that were initially tidally underfilling. We find that the ratio between binary fractions is not affected by the way we calculate these fractions [e.g. only main-sequence binaries (MS) or observational binaries, i.e. MS stars &gt;0.4 M⊙ mass ratios &gt;0.5]. This implies that the MS stars themselves are a very good proxy for probing entire populations of FG and SG. We also discuss how it relates to the observations of Milky Way GCs. We show that mocca models are able to reproduce the observed range of SG fractions for Milky Way GCs for which we know these fractions. We show how the SG fractions depend on the initial conditions and provide some constraints for the initial conditions to have more numerous FG or SG stars at the Hubble time.</p>}},
  author       = {{Hypki, Arkadiusz and Giersz, Mirek and Hong, Jongsuk and Leveque, Agostino and Askar, Abbas and Belloni, Diogo and Otulakowska-Hypka, Magdalena}},
  issn         = {{0035-8711}},
  keywords     = {{galaxies: star clusters: general; methods: numerical; software: data analysis; stars: chemically peculiar}},
  language     = {{eng}},
  number       = {{4}},
  pages        = {{4768--4787}},
  publisher    = {{Oxford University Press}},
  series       = {{Monthly Notices of the Royal Astronomical Society}},
  title        = {{MOCCA: dynamics and evolution of single and binary stars of multiple stellar populations in tidally filling and underfilling globular star clusters}},
  url          = {{http://dx.doi.org/10.1093/mnras/stac2815}},
  doi          = {{10.1093/mnras/stac2815}},
  volume       = {{517}},
  year         = {{2022}},
}