FROST-CLUSTERS – III. Metallicity-dependent intermediate mass black hole formation by runaway collisions in dense star clusters
Clicks: 3
ID: 315084
2026
Article Quality & Performance Metrics
Overall Quality
Not rated
Combines reader engagement with the AI quality analysis. This
article has not been analysed, so there is no overall score —
reader engagement is measured and shown alongside.
Reader Engagement
Steady Performance
0.6
/100
3 views
2 readers
AI Quality Assessment
Not analyzed
Readership in this journal
SteadyRanked #659 of 913 articles by views in monthly notices of the royal astronomical society
Most read
Least read
Bar heights use a square-root scale. Only the 120 most-read articles are drawn; the journal has 913 in total.
Mint this article as an NFT
Not yet mintedCreate a permanent, verifiable on-chain record of this article on the Scimatic Network. The NFT is held in your Journament account, and you can withdraw it to your own wallet at any time.
5
SUSD
one-off · no wallet required
Abstract
Abstract We explore the formation of intermediate mass black holes (IMBHs), potential seeds for supermassive black holes (SMBHs), via runaway stellar collisions for a wide range of star cluster (surface) densities (4 × 103 M⊙ pc−2 ≲ Σh ≲ 4 × 106 M⊙ pc−2) and metallicities (0.01 Z⊙ ≲ Z ≲ 1.0 Z⊙). Our sample of isolated (>1400) and hierarchical (30) simulations of young, massive star clusters with up to N = 1.8 × 106 stars includes collisional stellar dynamics, stellar evolution, and post-Newtonian equations of motion for black holes using the BIFROST code. High stellar wind rates suppress IMBH formation at high metallicities (Z ≳ 0.2 Z⊙) and low collision rates prevent their formation at low densities (Σh ≲ 3 × 104 M⊙ pc−2). The assumptions about stellar wind loss rates strongly affect the maximum final IMBH masses (M• ~ 6000 M⊙ vs. 25000 M⊙). The total stellar mass loss from collisions and collisionally boosted winds before t = 3 Myr can together reach up to 5–10 % of the final cluster mass. We present fitting formulae for IMBH masses as a function of host star cluster Σh and Z which can be used to seed SMBHs in high resolution cosmological hydrodynamical simulations and in semi-analytic models for galaxy formation. Our results favour IMBH formation in dense low metallicity environments similar to z ~ 10 James Webb Space Telescope (JWST) proto globular clusters. IMBH formation is suppressed in the high metallicity and low density conditions of the local Universe.
| Reference Key |
openalex_W7162572181
Use this key to autocite in the manuscript while using
SciMatic Manuscript Manager or Thesis Manager
|
|---|---|
| Authors | Antti Rantala, Thorsten Naab, Natalia Lahén, Klaus Reuter, Markus Rampp, Martyna Chruślińska, B. Reinoso |
| Journal | monthly notices of the royal astronomical society |
| Year | 2026 |
| DOI |
10.1093/mnras/stag986
|
| URL | |
| Keywords | Keywords not found |
Citations
No citations found. To add a citation, contact the admin at info@scimatic.org
Comments
No comments yet. Be the first to comment on this article.