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Peer-reviewedCC BY 4.0Monthly Notices of the Royal Astronomical Society

The fingerprint of primordial mass segregation on the tidal tails of star clusters

  • S Mojtaba Ghasemi1
  • Hosein Haghi1,2,3,4
  • Mohammad Mansoury1
  • Akram Hasani Zonoozi1,2
  • Pouriya Miri1,5
  • Pavel Kroupa2,6
6 affiliations
  1. 1Institute for Advanced Studies in Basic Sciences (IASBS) Department of Physics, , PO Box 11365-9161, Zanjan ,
  2. 2Helmholtz-Institut für Strahlen-und Kernphysik (HISKP) , Universität Bonn, Nussallee 14-16, D-53115 Bonn ,
  3. 3School of Astronomy, Institute for Research in Fundamental Sciences (IPM) , PO Box 19395 5531, Tehran ,
  4. 4Center for International Scientific studies and Collaborations (CISSC), Ministery of Science, Research and Technology , PO Box 15986-86515, Tehran ,
  5. 5Faculty of Computer and Information Science, University of Ljubljana , večna pot 113, 1000 Ljubljana ,
  6. 6Charles University in Prague, Faculty of Mathematics and Physics, Astronomical Institute , V Holešovičkách 2, CZ-180 00, Praha 8 ,
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Abstract

We investigate the effect of primordial mass segregation (PMS) in shaping the tidal tail structures of star clusters, searching for any trace of PMS on the tails at both early and late evolutionary stages. Through N-body simulations, we analyze clusters with two different degrees of PMS at various Galactocentric distances (RG), considering two black hole retention scenarios. Our findings reveal that PMS influences early cluster expansion and the formation of tidal tails with a bottom-heavy stellar mass function, this being more pronounced at smaller RG but diminishes over time. Primordially segregated clusters exhibit denser, unified, and longer tail structures compared to non-segregated clusters. The mean stellar mass distribution along the tails shows distinct patterns for primordially segregated and non-segregated clusters, converging at later evolutionary stages. The retention of stellar remnants has a weak impact on the mean mass distribution along the tails and on its morphology. We find that although mean mass differences persist along the tidal tails, the rate of change in primordially mass-segregated clusters eventually converges with that of non-segregated clusters, suggesting that the influence of primordial mass segregation on the tidal tails gradually diminishes over the course of cluster evolution.

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Cite

BibTeXRIS
BibTeX
@article{ghasemi2026fingerprint,
  title = {{The fingerprint of primordial mass segregation on the tidal tails of star clusters}},
  author = {S Mojtaba Ghasemi and Hosein Haghi and Mohammad Mansoury and Akram Hasani Zonoozi and Pouriya Miri and Pavel Kroupa},
  journal = {Monthly Notices of the Royal Astronomical Society},
  year = {2026},
  month = nov,
  doi = {10.1093/mnras/stag1199},
  url = {https://academic.oup.com/mnras/advance-article/doi/10.1093/mnras/stag1199/9011261},
  note = {CC BY 4.0},
}
RIS
TY  - JOUR
TI  - The fingerprint of primordial mass segregation on the tidal tails of star clusters
AU  - S Mojtaba Ghasemi
AU  - Hosein Haghi
AU  - Mohammad Mansoury
AU  - Akram Hasani Zonoozi
AU  - Pouriya Miri
AU  - Pavel Kroupa
PY  - 2026
DA  - 2026/11/03
JO  - Monthly Notices of the Royal Astronomical Society
DO  - 10.1093/mnras/stag1199
UR  - https://academic.oup.com/mnras/advance-article/doi/10.1093/mnras/stag1199/9011261
AB  - We investigate the effect of primordial mass segregation (PMS) in shaping the tidal tail structures of star clusters, searching for any trace of PMS on the tails at both early and late evolutionary stages. Through N-body simulations, we analyze clusters with two different degrees of PMS at various Galactocentric distances (RG), considering two black hole retention scenarios. Our findings reveal that PMS influences early cluster expansion and the formation of tidal tails with a bottom-heavy stellar mass function, this being more pronounced at smaller RG but diminishes over time. Primordially segregated clusters exhibit denser, unified, and longer tail structures compared to non-segregated clusters. The mean stellar mass distribution along the tails shows distinct patterns for primordially segregated and non-segregated clusters, converging at later evolutionary stages. The retention of stellar remnants has a weak impact on the mean mass distribution along the tails and on its morphology. We find that although mean mass differences persist along the tidal tails, the rate of change in primordially mass-segregated clusters eventually converges with that of non-segregated clusters, suggesting that the influence of primordial mass segregation on the tidal tails gradually diminishes over the course of cluster evolution.
SN  - 0035-8711
SN  - 1365-2966
ER  -