Central Dynamics of Multi-mass Rotating Star Clusters

Maria Tiongco*, Angela Collier, Anna Lisa Varri

*Corresponding author for this work

Research output: Contribution to journalArticlepeer-review

Abstract / Description of output

We investigate the evolutionary nexus between the morphology and internal kinematics of the central regions of collisional, rotating, multi-mass stellar systems, with special attention to the spatial characterisation of the process of mass segregation. We report results from idealized, purely $N$-body simulations that show multi-mass, rotating, and spherical systems rapidly form an oblate, spheroidal massive core, unlike single-mass rotating or multi-mass non-rotating configurations with otherwise identical initial properties, indicating that this evolution is a result of the interplay between the presence of a mass spectrum and angular momentum. This feature appears to be long-lasting, preserving itself for several relaxation times. The degree of flattening experienced by the systems is directly proportional to the initial degree of internal rotation. In addition, this morphological effect has a clear characterisation in terms of orbital architecture, as it lowers the inclination of the orbits of massive stars. We offer an idealised dynamical interpretation that could explain the mechanism underpinning this effect and we highlight possible useful implications, from kinematic hysteresis to spatial distribution of dark remnants in dense stellar systems.
Original languageEnglish
Pages (from-to)4488-4498
Number of pages11
JournalMonthly Notices of the Royal Astronomical Society
Issue number3
Early online date14 Jul 2021
Publication statusPublished - 1 Sept 2021

Keywords / Materials (for Non-textual outputs)

  • astro-ph.GA


Dive into the research topics of 'Central Dynamics of Multi-mass Rotating Star Clusters'. Together they form a unique fingerprint.

Cite this